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CDAWeb Served Heliophysics Datasets Beginning with 'M'

MARINER2_HELIO1HR_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)

MARINER2_R0_MAGPLASMA: Mariner2 merged magnetic field and plasma hourly data from COHOWeb Service

MARS_HELIO1HR_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)

MAVEN_HELIO1HR_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)

MERCURY_HELIO1HR_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)

MESSENGER_HELIO1HR_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)

MESSENGER_MAG_RTN: MESSENGER interplanetary magnetic field (1-second/high resolution) in RTN coordinates - Prof. Sean C. Solomon (Carnegie Institution of Washington)

METOP1_POES-SEM2_FLUXES-2SEC: POES-SEM2 2-second Particle Precipitation Data, MetOp-B (MetOp-1 before Sept2012 launch) [Important: these data have known contamination problems: please consult Rob Redmon (sem.poes@noaa.gov) for usage recommendations.] - NGDC and SWPC (NOAA)

METOP2_POES-SEM2_FLUXES-2SEC: POES-SEM2 2-second Particle Precipitation Data, MetOp-A (MetOp-2 before Oct2006 launch) [Important: these data have known contamination problems: please consult Rob Redmon (sem.poes@noaa.gov) for usage recommendations.] - NGDC and SWPC (NOAA)

METOP3_POES-SEM2_FLUXES-2SEC: POES-SEM2 2-second Particle Precipitation Data, MetOp-C (MetOp-3 launched 07 November 2018) [Important: these data have known contamination problems: please consult Rob Redmon (sem.poes@noaa.gov) for usage recommendations.] - NCEI (NOAA)

MGS_MAG_HIGH: Mars Global Surveyor Magnetometer High Resolution - M. Acuna (NASA/GSFC)

MGS_MAG_LOW: Mars Global Surveyor Magnetometer Modified Data - M. Acuna (NASA/GSFC)

MMS1_ASPOC_SRVY_L2: Level 2 Active Spacecraft Potential Control Survey Data - K. Torkar, R. Nakamura (IWF)

MMS1_DSP_FAST_L2_BPSD: search coil magnetometer spectral density - J. Burch, R. Ergun, O. Le Contel (SWRI, LASP, LPP)

MMS1_DSP_FAST_L2_EPSD: electric spectral density - J. Burch, R. Ergun (SWRI, LASP)

MMS1_DSP_SLOW_L2_BPSD: search coil magnetometer spectral density - J. Burch, R. Ergun, O. Le Contel (SWRI, LASP, LPP)

MMS1_DSP_SLOW_L2_EPSD: electric spectral density - J. Burch, R. Ergun (SWRI, LASP)

MMS1_EDI_BRST_L2_AMB: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS1_EDI_BRST_L2_AMB-PM2: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS1_EDI_BRST_L2_EFIELD: Level 2 EDI electric field - Roy Torbert and Hans Vaith (UNH)

MMS1_EDI_BRST_L2_Q0: Level 2 EDI Quality 0 Counts - Roy Torbert, Hans Vaith (UNH)

MMS1_EDI_SRVY_L2_AMB: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS1_EDI_SRVY_L2_AMB-PM2: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS1_EDI_SRVY_L2_EFIELD: Level 2 EDI electric field - Roy Torbert and Hans Vaith (UNH)

MMS1_EDI_SRVY_L2_Q0: Level 2 EDI Quality 0 Counts - Roy Torbert, Hans Vaith (UNH)

MMS1_EDP_BRST_L2_DCE: MMS1 L2 (brst), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS1_EDP_BRST_L2_HMFE: MMS1 l2 (brst), 3D HMFE Electric field - Burch, J, Ergun, R., Lindqvist, P. (SwRI, LASP, KTH)

MMS1_EDP_BRST_L2_SCPOT: MMS 1 dual probe scpot (brst), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS1_EDP_FAST_L2_DCE: MMS1 L2 (fast), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS1_EDP_FAST_L2_SCPOT: MMS 1 dual probe scpot (fast), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS1_EDP_SLOW_L2_DCE: MMS1 L2 (slow), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS1_EDP_SLOW_L2_SCPOT: MMS 1 dual probe scpot (slow), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS1_EDP_SRVY_L2_HFESP: MMS1 L2 (srvy), HF ACE Spectra - Burch, J, Ergun, R., Lindqvist, P. (SwRI, LASP, KTH)

MMS1_EPD-EIS_BRST_L2_EXTOF: Level 2 Energetic Ion Spectrometer EnergyxTOF Brst - B. Mauk (JHU/APL)

MMS1_EPD-EIS_BRST_L2_PHXTOF: Level 2 Energetic Ion Spectrometer PulseHeightxTOF Brst - B. Mauk (JHU/APL)

MMS1_EPD-EIS_SRVY_L2_ELECTRONENERGY: Level 2 Energetic Ion Spectrometer Electron Spectra Srvy - B. Mauk (JHU/APL)

MMS1_EPD-EIS_SRVY_L2_EXTOF: Level 2 Energetic Ion Spectrometer EnergyxTOF Srvy - B. Mauk (JHU/APL)

MMS1_EPD-EIS_SRVY_L2_PHXTOF: Level 2 Energetic Ion Spectrometer PulseHeightxTOF Srvy - B. Mauk (JHU/APL)

MMS1_FEEPS_BRST_L2_ELECTRON: Level 2 Flys Eye Energetic Particle Sensor Burst Data - STP (LASP)

MMS1_FEEPS_BRST_L2_ION: Level 2 Flys Eye Energetic Particle Sensor Burst Data - STP (LASP)

MMS1_FEEPS_SRVY_L2_ELECTRON: Level 2 Flys Eye Energetic Particle Sensor Survey Data - STP (LASP)

MMS1_FEEPS_SRVY_L2_ION: Level 2 Flys Eye Energetic Particle Sensor Survey Data - STP (LASP)

MMS1_FGM_BRST_L2: Level2 Flux Gate Magnetometer Burst DC Magnetic Field for MMS Satellite Number 1 - J. Burch, C. Russell, W. Magnus (SWRI, UCLA, IWF)

MMS1_FGM_SRVY_L2: Level2 Flux Gate Magnetometer Combined Fast/Slow Survey DC Magnetic Field for MMS Satellite Number 1 - J. Burch, C. Russell, W. Magnus (SWRI, UCLA, IWF)

MMS1_FPI_BRST_L2_DES-DIST: MMS Satellite Number 1 Dual Electron Spectrometer Burst-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS1_FPI_BRST_L2_DES-MOMS: MMS Satellite Number 1 Dual Electron Spectrometer Burst-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS1_FPI_BRST_L2_DES-PARTMOMS: MMS Satellite Number 1 Dual Electron Spectrometer Burst-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS1_FPI_BRST_L2_DIS-DIST: MMS Satellite Number 1 Dual Ion Spectrometer Burst-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS1_FPI_BRST_L2_DIS-MOMS: MMS Satellite Number 1 Dual Ion Spectrometer Burst-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS1_FPI_BRST_L2_DIS-PARTMOMS: MMS Satellite Number 1 Dual Ion Spectrometer Burst-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS1_FPI_FAST_L2_DES-DIST: MMS Satellite Number 1 Dual Electron Spectrometer FastSurvey-resolution instrument distributions - J. Burch, B. Giles (SwRI, GSFC)

MMS1_FPI_FAST_L2_DES-MOMS: MMS Satellite Number 1 Dual Electron Spectrometer FastSurvey-resolution distribution moments - J. Burch, B. Giles (SwRI, GSFC)

MMS1_FPI_FAST_L2_DES-MOMSAUX: MMS Satellite Number 1 Dual Electron Spectrometer FastSurvey-resolution auxiliary moments - J. Burch, B. Giles (SwRI, GSFC)

MMS1_FPI_FAST_L2_DES-PARTMOMS: MMS Satellite Number 1 Dual Electron Spectrometer FastSurvey-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS1_FPI_FAST_L2_DIS-DIST: MMS Satellite Number 1 Dual Ion Spectrometer FastSurvey-resolution instrument distributions - J. Burch, B. Giles (SwRI, GSFC)

MMS1_FPI_FAST_L2_DIS-MOMS: MMS Satellite Number 1 Dual Ion Spectrometer FastSurvey-resolution distribution moments - J. Burch, B. Giles (SwRI, GSFC)

MMS1_FPI_FAST_L2_DIS-MOMSAUX: MMS Satellite Number 1 Dual Ion Spectrometer FastSurvey-resolution auxiliary moments - J. Burch, B. Giles (SwRI, GSFC)

MMS1_FPI_FAST_L2_DIS-PARTMOMS: MMS Satellite Number 1 Dual Ion Spectrometer FastSurvey-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS1_FPI_SLOW_L2_DES-DIST: MMS Satellite Number 1 Dual Electron Spectrometer SlowSurvey-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS1_FPI_SLOW_L2_DES-MOMS: MMS Satellite Number 1 Dual Electron Spectrometer SlowSurvey-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS1_FPI_SLOW_L2_DES-MOMSAUX: MMS Satellite Number 1 Dual Electron Spectrometer SlowSurvey-resolution auxiliary moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS1_FPI_SLOW_L2_DIS-DIST: MMS Satellite Number 1 Dual Ion Spectrometer SlowSurvey-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS1_FPI_SLOW_L2_DIS-MOMS: MMS Satellite Number 1 Dual Ion Spectrometer SlowSurvey-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS1_FPI_SLOW_L2_DIS-MOMSAUX: MMS Satellite Number 1 Dual Ion Spectrometer SlowSurvey-resolution auxiliary moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS1_HPCA_BRST_L2_ION: Level 2> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS1_HPCA_BRST_L2_MOMENTS: Level 2 Moments> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS1_HPCA_SRVY_L2_ION: Level 2> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS1_HPCA_SRVY_L2_MOMENTS: Level 2 Moments> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS1_HPCA_SRVY_L2_TOF-COUNTS: Level 1b> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS1_MEC_BRST_L2_EPHT89D: Magnetic ephemeris and support data for MMS satellite number 1 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS1_MEC_BRST_L2_EPHT89Q: Magnetic ephemeris and support data for MMS satellite number 1 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS1_MEC_BRST_L2_EPHTS04D: Magnetic ephemeris and support data for MMS satellite number 1 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS1_MEC_SRVY_L2_EPHT89D: Magnetic ephemeris and support data for MMS satellite number 1 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS1_MEC_SRVY_L2_EPHT89Q: Magnetic ephemeris and support data for MMS satellite number 1 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS1_MEC_SRVY_L2_EPHTS04D: Magnetic ephemeris and support data for MMS satellite number 1 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS1_R0_SUMMARY: Links to MMS-1 pre-generated Quicklook Summary plots - James Burch (SWRI)

MMS1_SCM_BRST_L2_SCB: Level 2 Search Coil Magnetometer AC Magnetic Field Burst (8192S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS1_SCM_BRST_L2_SCHB: Level 2 Search Coil Magnetometer AC Magnetic Field High Burst (16384S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS1_SCM_SRVY_L2_SCSRVY: Level 2 Search Coil Magnetometer AC Magnetic Field Survey (32S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS2_ASPOC_SRVY_L2: Level 2 Active Spacecraft Potential Control Survey Data - K. Torkar, R. Nakamura (IWF)

MMS2_DSP_FAST_L2_BPSD: search coil magnetometer spectral density - J. Burch, R. Ergun, O. Le Contel (SWRI, LASP, LPP)

MMS2_DSP_FAST_L2_EPSD: electric spectral density - J. Burch, R. Ergun (SWRI, LASP)

MMS2_DSP_SLOW_L2_BPSD: search coil magnetometer spectral density - J. Burch, R. Ergun, O. Le Contel (SWRI, LASP, LPP)

MMS2_DSP_SLOW_L2_EPSD: electric spectral density - J. Burch, R. Ergun (SWRI, LASP)

MMS2_EDI_BRST_L2_AMB: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS2_EDI_BRST_L2_AMB-PM2: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS2_EDI_BRST_L2_EFIELD: Level 2 EDI electric field - Roy Torbert and Hans Vaith (UNH)

MMS2_EDI_BRST_L2_Q0: Level 2 EDI Quality 0 Counts - Roy Torbert, Hans Vaith (UNH)

MMS2_EDI_SRVY_L2_AMB: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS2_EDI_SRVY_L2_AMB-PM2: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS2_EDI_SRVY_L2_EFIELD: Level 2 EDI electric field - Roy Torbert and Hans Vaith (UNH)

MMS2_EDI_SRVY_L2_Q0: Level 2 EDI Quality 0 Counts - Roy Torbert, Hans Vaith (UNH)

MMS2_EDP_BRST_L2_DCE: MMS2 L2 (brst), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS2_EDP_BRST_L2_HMFE: MMS2 l2 (brst), 3D HMFE Electric field - Burch, J, Ergun, R., Lindqvist, P. (SwRI, LASP, KTH)

MMS2_EDP_BRST_L2_SCPOT: MMS 2 dual probe scpot (brst), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS2_EDP_FAST_L2_DCE: MMS2 L2 (fast), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS2_EDP_FAST_L2_SCPOT: MMS 2 dual probe scpot (fast), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS2_EDP_SLOW_L2_DCE: MMS2 L2 (slow), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS2_EDP_SLOW_L2_SCPOT: MMS 2 dual probe scpot (slow), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS2_EDP_SRVY_L2_HFESP: MMS2 L2 (srvy), HF ACE Spectra - Burch, J, Ergun, R., Lindqvist, P. (SwRI, LASP, KTH)

MMS2_EPD-EIS_BRST_L2_EXTOF: Level 2 Energetic Ion Spectrometer EnergyxTOF Brst - B. Mauk (JHU/APL)

MMS2_EPD-EIS_BRST_L2_PHXTOF: Level 2 Energetic Ion Spectrometer PulseHeightxTOF Brst - B. Mauk (JHU/APL)

MMS2_EPD-EIS_SRVY_L2_ELECTRONENERGY: Level 2 Energetic Ion Spectrometer Electron Spectra Srvy - B. Mauk (JHU/APL)

MMS2_EPD-EIS_SRVY_L2_EXTOF: Level 2 Energetic Ion Spectrometer EnergyxTOF Srvy - B. Mauk (JHU/APL)

MMS2_EPD-EIS_SRVY_L2_PHXTOF: Level 2 Energetic Ion Spectrometer PulseHeightxTOF Srvy - B. Mauk (JHU/APL)

MMS2_FEEPS_BRST_L2_ELECTRON: Level 2 Flys Eye Energetic Particle Sensor Burst Data - STP (LASP)

MMS2_FEEPS_BRST_L2_ION: Level 2 Flys Eye Energetic Particle Sensor Burst Data - STP (LASP)

MMS2_FEEPS_SRVY_L2_ELECTRON: Level 2 Flys Eye Energetic Particle Sensor Survey Data - STP (LASP)

MMS2_FEEPS_SRVY_L2_ION: Level 2 Flys Eye Energetic Particle Sensor Survey Data - STP (LASP)

MMS2_FGM_BRST_L2: Level2 Flux Gate Magnetometer Burst DC Magnetic Field for MMS Satellite Number 2 - J. Burch, C. Russell, W. Magnus (SWRI, UCLA, IWF)

MMS2_FGM_SRVY_L2: Level2 Flux Gate Magnetometer Combined Fast/Slow Survey DC Magnetic Field for MMS Satellite Number 2 - J. Burch, C. Russell, W. Magnus (SWRI, UCLA, IWF)

MMS2_FPI_BRST_L2_DES-DIST: MMS Satellite Number 2 Dual Electron Spectrometer Burst-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS2_FPI_BRST_L2_DES-MOMS: MMS Satellite Number 2 Dual Electron Spectrometer Burst-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS2_FPI_BRST_L2_DES-PARTMOMS: MMS Satellite Number 2 Dual Electron Spectrometer Burst-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS2_FPI_BRST_L2_DIS-DIST: MMS Satellite Number 2 Dual Ion Spectrometer Burst-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS2_FPI_BRST_L2_DIS-MOMS: MMS Satellite Number 2 Dual Ion Spectrometer Burst-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS2_FPI_BRST_L2_DIS-PARTMOMS: MMS Satellite Number 2 Dual Ion Spectrometer Burst-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS2_FPI_FAST_L2_DES-DIST: MMS Satellite Number 2 Dual Electron Spectrometer FastSurvey-resolution instrument distributions - J. Burch, B. Giles (SwRI, GSFC)

MMS2_FPI_FAST_L2_DES-MOMS: MMS Satellite Number 2 Dual Electron Spectrometer FastSurvey-resolution distribution moments - J. Burch, B. Giles (SwRI, GSFC)

MMS2_FPI_FAST_L2_DES-MOMSAUX: MMS Satellite Number 2 Dual Electron Spectrometer FastSurvey-resolution auxiliary moments - J. Burch, B. Giles (SwRI, GSFC)

MMS2_FPI_FAST_L2_DES-PARTMOMS: MMS Satellite Number 2 Dual Electron Spectrometer FastSurvey-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS2_FPI_FAST_L2_DIS-DIST: MMS Satellite Number 2 Dual Ion Spectrometer FastSurvey-resolution instrument distributions - J. Burch, B. Giles (SwRI, GSFC)

MMS2_FPI_FAST_L2_DIS-MOMS: MMS Satellite Number 2 Dual Ion Spectrometer FastSurvey-resolution distribution moments - J. Burch, B. Giles (SwRI, GSFC)

MMS2_FPI_FAST_L2_DIS-MOMSAUX: MMS Satellite Number 2 Dual Ion Spectrometer FastSurvey-resolution auxiliary moments - J. Burch, B. Giles (SwRI, GSFC)

MMS2_FPI_FAST_L2_DIS-PARTMOMS: MMS Satellite Number 2 Dual Ion Spectrometer FastSurvey-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS2_FPI_SLOW_L2_DES-DIST: MMS Satellite Number 2 Dual Electron Spectrometer SlowSurvey-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS2_FPI_SLOW_L2_DES-MOMS: MMS Satellite Number 2 Dual Electron Spectrometer SlowSurvey-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS2_FPI_SLOW_L2_DES-MOMSAUX: MMS Satellite Number 2 Dual Electron Spectrometer SlowSurvey-resolution auxiliary moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS2_FPI_SLOW_L2_DIS-DIST: MMS Satellite Number 2 Dual Ion Spectrometer SlowSurvey-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS2_FPI_SLOW_L2_DIS-MOMS: MMS Satellite Number 2 Dual Ion Spectrometer SlowSurvey-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS2_FPI_SLOW_L2_DIS-MOMSAUX: MMS Satellite Number 2 Dual Ion Spectrometer SlowSurvey-resolution auxiliary moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS2_HPCA_BRST_L2_ION: Level 2> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS2_HPCA_BRST_L2_MOMENTS: Level 2 Moments> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS2_HPCA_SRVY_L2_ION: Level 2> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS2_HPCA_SRVY_L2_MOMENTS: Level 2 Moments> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS2_HPCA_SRVY_L2_TOF-COUNTS: Level 1b> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS2_MEC_BRST_L2_EPHT89D: Magnetic ephemeris and support data for MMS satellite number 2 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS2_MEC_BRST_L2_EPHT89Q: Magnetic ephemeris and support data for MMS satellite number 2 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS2_MEC_BRST_L2_EPHTS04D: Magnetic ephemeris and support data for MMS satellite number 2 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS2_MEC_SRVY_L2_EPHT89D: Magnetic ephemeris and support data for MMS satellite number 2 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS2_MEC_SRVY_L2_EPHT89Q: Magnetic ephemeris and support data for MMS satellite number 2 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS2_MEC_SRVY_L2_EPHTS04D: Magnetic ephemeris and support data for MMS satellite number 2 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS2_R0_SUMMARY: Links to MMS-2 pre-generated Quicklook Summary plots - James Burch (SWRI)

MMS2_SCM_BRST_L2_SCB: Level 2 Search Coil Magnetometer AC Magnetic Field Burst (8192S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS2_SCM_BRST_L2_SCHB: Level 2 Search Coil Magnetometer AC Magnetic Field High Burst (16384S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS2_SCM_SRVY_L2_SCSRVY: Level 2 Search Coil Magnetometer AC Magnetic Field Survey (32S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS3_ASPOC_SRVY_L2: Level 2 Active Spacecraft Potential Control Survey Data - K. Torkar, R. Nakamura (IWF)

MMS3_DSP_FAST_L2_BPSD: search coil magnetometer spectral density - J. Burch, R. Ergun, O. Le Contel (SWRI, LASP, LPP)

MMS3_DSP_FAST_L2_EPSD: electric spectral density - J. Burch, R. Ergun (SWRI, LASP)

MMS3_DSP_SLOW_L2_BPSD: search coil magnetometer spectral density - J. Burch, R. Ergun, O. Le Contel (SWRI, LASP, LPP)

MMS3_DSP_SLOW_L2_EPSD: electric spectral density - J. Burch, R. Ergun (SWRI, LASP)

MMS3_EDI_BRST_L2_AMB: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS3_EDI_BRST_L2_AMB-PM2: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS3_EDI_BRST_L2_EFIELD: Level 2 EDI electric field - Roy Torbert and Hans Vaith (UNH)

MMS3_EDI_BRST_L2_Q0: Level 2 EDI Quality 0 Counts - Roy Torbert, Hans Vaith (UNH)

MMS3_EDI_SRVY_L2_AMB: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS3_EDI_SRVY_L2_AMB-PM2: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS3_EDI_SRVY_L2_EFIELD: Level 2 EDI electric field - Roy Torbert and Hans Vaith (UNH)

MMS3_EDI_SRVY_L2_Q0: Level 2 EDI Quality 0 Counts - Roy Torbert, Hans Vaith (UNH)

MMS3_EDP_BRST_L2_DCE: MMS3 L2 (brst), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS3_EDP_BRST_L2_HMFE: MMS3 l2 (brst), 3D HMFE Electric field - Burch, J, Ergun, R., Lindqvist, P. (SwRI, LASP, KTH)

MMS3_EDP_BRST_L2_SCPOT: MMS 3 dual probe scpot (brst), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS3_EDP_FAST_L2_DCE: MMS3 L2 (fast), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS3_EDP_FAST_L2_SCPOT: MMS 3 dual probe scpot (fast), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS3_EDP_SLOW_L2_DCE: MMS3 L2 (slow), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS3_EDP_SLOW_L2_SCPOT: MMS 3 dual probe scpot (slow), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS3_EDP_SRVY_L2_HFESP: MMS3 L2 (srvy), HF ACE Spectra - Burch, J, Ergun, R., Lindqvist, P. (SwRI, LASP, KTH)

MMS3_EPD-EIS_BRST_L2_EXTOF: Level 2 Energetic Ion Spectrometer EnergyxTOF Brst - B. Mauk (JHU/APL)

MMS3_EPD-EIS_BRST_L2_PHXTOF: Level 2 Energetic Ion Spectrometer PulseHeightxTOF Brst - B. Mauk (JHU/APL)

MMS3_EPD-EIS_SRVY_L2_ELECTRONENERGY: Level 2 Energetic Ion Spectrometer Electron Spectra Srvy - B. Mauk (JHU/APL)

MMS3_EPD-EIS_SRVY_L2_EXTOF: Level 2 Energetic Ion Spectrometer EnergyxTOF Srvy - B. Mauk (JHU/APL)

MMS3_EPD-EIS_SRVY_L2_PHXTOF: Level 2 Energetic Ion Spectrometer PulseHeightxTOF Srvy - B. Mauk (JHU/APL)

MMS3_FEEPS_BRST_L2_ELECTRON: Level 2 Flys Eye Energetic Particle Sensor Burst Data - STP (LASP)

MMS3_FEEPS_BRST_L2_ION: Level 2 Flys Eye Energetic Particle Sensor Burst Data - STP (LASP)

MMS3_FEEPS_SRVY_L2_ELECTRON: Level 2 Flys Eye Energetic Particle Sensor Survey Data - STP (LASP)

MMS3_FEEPS_SRVY_L2_ION: Level 2 Flys Eye Energetic Particle Sensor Survey Data - STP (LASP)

MMS3_FGM_BRST_L2: Level2 Flux Gate Magnetometer Burst DC Magnetic Field for MMS Satellite Number 3 - J. Burch, C. Russell, W. Magnus (SWRI, UCLA, IWF)

MMS3_FGM_SRVY_L2: Level2 Flux Gate Magnetometer Combined Fast/Slow Survey DC Magnetic Field for MMS Satellite Number 3 - J. Burch, C. Russell, W. Magnus (SWRI, UCLA, IWF)

MMS3_FPI_BRST_L2_DES-DIST: MMS Satellite Number 3 Dual Electron Spectrometer Burst-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS3_FPI_BRST_L2_DES-MOMS: MMS Satellite Number 3 Dual Electron Spectrometer Burst-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS3_FPI_BRST_L2_DES-PARTMOMS: MMS Satellite Number 3 Dual Electron Spectrometer Burst-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS3_FPI_BRST_L2_DIS-DIST: MMS Satellite Number 3 Dual Ion Spectrometer Burst-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS3_FPI_BRST_L2_DIS-MOMS: MMS Satellite Number 3 Dual Ion Spectrometer Burst-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS3_FPI_BRST_L2_DIS-PARTMOMS: MMS Satellite Number 3 Dual Ion Spectrometer Burst-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS3_FPI_FAST_L2_DES-DIST: MMS Satellite Number 3 Dual Electron Spectrometer FastSurvey-resolution instrument distributions - J. Burch, B. Giles (SwRI, GSFC)

MMS3_FPI_FAST_L2_DES-MOMS: MMS Satellite Number 3 Dual Electron Spectrometer FastSurvey-resolution distribution moments - J. Burch, B. Giles (SwRI, GSFC)

MMS3_FPI_FAST_L2_DES-MOMSAUX: MMS Satellite Number 3 Dual Electron Spectrometer FastSurvey-resolution auxiliary moments - J. Burch, B. Giles (SwRI, GSFC)

MMS3_FPI_FAST_L2_DES-PARTMOMS: MMS Satellite Number 3 Dual Electron Spectrometer FastSurvey-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS3_FPI_FAST_L2_DIS-DIST: MMS Satellite Number 3 Dual Ion Spectrometer FastSurvey-resolution instrument distributions - J. Burch, B. Giles (SwRI, GSFC)

MMS3_FPI_FAST_L2_DIS-MOMS: MMS Satellite Number 3 Dual Ion Spectrometer FastSurvey-resolution distribution moments - J. Burch, B. Giles (SwRI, GSFC)

MMS3_FPI_FAST_L2_DIS-MOMSAUX: MMS Satellite Number 3 Dual Ion Spectrometer FastSurvey-resolution auxiliary moments - J. Burch, B. Giles (SwRI, GSFC)

MMS3_FPI_FAST_L2_DIS-PARTMOMS: MMS Satellite Number 3 Dual Ion Spectrometer FastSurvey-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS3_FPI_SLOW_L2_DES-DIST: MMS Satellite Number 3 Dual Electron Spectrometer SlowSurvey-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS3_FPI_SLOW_L2_DES-MOMS: MMS Satellite Number 3 Dual Electron Spectrometer SlowSurvey-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS3_FPI_SLOW_L2_DES-MOMSAUX: MMS Satellite Number 3 Dual Electron Spectrometer SlowSurvey-resolution auxiliary moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS3_FPI_SLOW_L2_DIS-DIST: MMS Satellite Number 3 Dual Ion Spectrometer SlowSurvey-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS3_FPI_SLOW_L2_DIS-MOMS: MMS Satellite Number 3 Dual Ion Spectrometer SlowSurvey-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS3_FPI_SLOW_L2_DIS-MOMSAUX: MMS Satellite Number 3 Dual Ion Spectrometer SlowSurvey-resolution auxiliary moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS3_HPCA_BRST_L2_ION: Level 2> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS3_HPCA_BRST_L2_MOMENTS: Level 2 Moments> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS3_HPCA_SRVY_L2_ION: Level 2> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS3_HPCA_SRVY_L2_MOMENTS: Level 2 Moments> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS3_HPCA_SRVY_L2_TOF-COUNTS: Level 1b> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS3_MEC_BRST_L2_EPHT89D: Magnetic ephemeris and support data for MMS satellite number 3 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS3_MEC_BRST_L2_EPHT89Q: Magnetic ephemeris and support data for MMS satellite number 3 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS3_MEC_BRST_L2_EPHTS04D: Magnetic ephemeris and support data for MMS satellite number 3 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS3_MEC_SRVY_L2_EPHT89D: Magnetic ephemeris and support data for MMS satellite number 3 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS3_MEC_SRVY_L2_EPHT89Q: Magnetic ephemeris and support data for MMS satellite number 3 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS3_MEC_SRVY_L2_EPHTS04D: Magnetic ephemeris and support data for MMS satellite number 3 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS3_R0_SUMMARY: Links to MMS-3 pre-generated Quicklook Summary plots - James Burch (SWRI)

MMS3_SCM_BRST_L2_SCB: Level 2 Search Coil Magnetometer AC Magnetic Field Burst (8192S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS3_SCM_BRST_L2_SCHB: Level 2 Search Coil Magnetometer AC Magnetic Field High Burst (16384S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS3_SCM_SRVY_L2_SCSRVY: Level 2 Search Coil Magnetometer AC Magnetic Field Survey (32S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS4_ASPOC_SRVY_L2: Level 2 Active Spacecraft Potential Control Survey Data - K. Torkar, R. Nakamura (IWF)

MMS4_DSP_FAST_L2_BPSD: search coil magnetometer spectral density - J. Burch, R. Ergun, O. Le Contel (SWRI, LASP, LPP)

MMS4_DSP_FAST_L2_EPSD: electric spectral density - J. Burch, R. Ergun (SWRI, LASP)

MMS4_DSP_SLOW_L2_BPSD: search coil magnetometer spectral density - J. Burch, R. Ergun, O. Le Contel (SWRI, LASP, LPP)

MMS4_DSP_SLOW_L2_EPSD: electric spectral density - J. Burch, R. Ergun (SWRI, LASP)

MMS4_EDI_BRST_L2_AMB: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS4_EDI_BRST_L2_AMB-PM2: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS4_EDI_BRST_L2_EFIELD: Level 2 EDI electric field - Roy Torbert and Hans Vaith (UNH)

MMS4_EDI_BRST_L2_Q0: Level 2 EDI Quality 0 Counts - Roy Torbert, Hans Vaith (UNH)

MMS4_EDI_SRVY_L2_AMB: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS4_EDI_SRVY_L2_AMB-PM2: Level 2 EDI Ambient electron flux - Roy Torbert, Hans Vaith (UNH)

MMS4_EDI_SRVY_L2_EFIELD: Level 2 EDI electric field - Roy Torbert and Hans Vaith (UNH)

MMS4_EDI_SRVY_L2_Q0: Level 2 EDI Quality 0 Counts - Roy Torbert, Hans Vaith (UNH)

MMS4_EDP_BRST_L2_DCE: MMS4 L2 (brst), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS4_EDP_BRST_L2_HMFE: MMS4 l2 (brst), 3D HMFE Electric field - Burch, J, Ergun, R., Lindqvist, P. (SwRI, LASP, KTH)

MMS4_EDP_BRST_L2_SCPOT: MMS 4 dual probe scpot (brst), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS4_EDP_FAST_L2_DCE: MMS4 L2 (fast), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS4_EDP_FAST_L2_SCPOT: MMS 4 dual probe scpot (fast), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS4_EDP_SLOW_L2_DCE: MMS4 L2 (slow), 3D Electric field - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS4_EDP_SLOW_L2_SCPOT: MMS 4 dual probe scpot (slow), Spacecraft potential - J.Burch, R.Ergun, P.Lindqvist. (SWRI, LASP, KTH)

MMS4_EDP_SRVY_L2_HFESP: MMS4 L2 (srvy), HF ACE Spectra - Burch, J, Ergun, R., Lindqvist, P. (SwRI, LASP, KTH)

MMS4_EPD-EIS_BRST_L2_EXTOF: Level 2 Energetic Ion Spectrometer EnergyxTOF Brst - B. Mauk (JHU/APL)

MMS4_EPD-EIS_BRST_L2_PHXTOF: Level 2 Energetic Ion Spectrometer PulseHeightxTOF Brst - B. Mauk (JHU/APL)

MMS4_EPD-EIS_SRVY_L2_ELECTRONENERGY: Level 2 Energetic Ion Spectrometer Electron Spectra Srvy - B. Mauk (JHU/APL)

MMS4_EPD-EIS_SRVY_L2_EXTOF: Level 2 Energetic Ion Spectrometer EnergyxTOF Srvy - B. Mauk (JHU/APL)

MMS4_EPD-EIS_SRVY_L2_PHXTOF: Level 2 Energetic Ion Spectrometer PulseHeightxTOF Srvy - B. Mauk (JHU/APL)

MMS4_FEEPS_BRST_L2_ELECTRON: Level 2 Flys Eye Energetic Particle Sensor Burst Data - STP (LASP)

MMS4_FEEPS_BRST_L2_ION: Level 2 Flys Eye Energetic Particle Sensor Burst Data - STP (LASP)

MMS4_FEEPS_SRVY_L2_ELECTRON: Level 2 Flys Eye Energetic Particle Sensor Survey Data - STP (LASP)

MMS4_FEEPS_SRVY_L2_ION: Level 2 Flys Eye Energetic Particle Sensor Survey Data - STP (LASP)

MMS4_FGM_BRST_L2: Level2 Flux Gate Magnetometer Burst DC Magnetic Field for MMS Satellite Number 4 - J. Burch, C. Russell, W. Magnus (SWRI, UCLA, IWF)

MMS4_FGM_SRVY_L2: Level2 Flux Gate Magnetometer Combined Fast/Slow Survey DC Magnetic Field for MMS Satellite Number 4 - J. Burch, C. Russell, W. Magnus (SWRI, UCLA, IWF)

MMS4_FPI_BRST_L2_DES-DIST: MMS Satellite Number 4 Dual Electron Spectrometer Burst-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS4_FPI_BRST_L2_DES-MOMS: MMS Satellite Number 4 Dual Electron Spectrometer Burst-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS4_FPI_BRST_L2_DES-PARTMOMS: MMS Satellite Number 4 Dual Electron Spectrometer Burst-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS4_FPI_BRST_L2_DIS-DIST: MMS Satellite Number 4 Dual Ion Spectrometer Burst-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS4_FPI_BRST_L2_DIS-MOMS: MMS Satellite Number 4 Dual Ion Spectrometer Burst-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS4_FPI_BRST_L2_DIS-PARTMOMS: MMS Satellite Number 4 Dual Ion Spectrometer Burst-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS4_FPI_FAST_L2_DES-DIST: MMS Satellite Number 4 Dual Electron Spectrometer FastSurvey-resolution instrument distributions - J. Burch, B. Giles (SwRI, GSFC)

MMS4_FPI_FAST_L2_DES-MOMS: MMS Satellite Number 4 Dual Electron Spectrometer FastSurvey-resolution distribution moments - J. Burch, B. Giles (SwRI, GSFC)

MMS4_FPI_FAST_L2_DES-MOMSAUX: MMS Satellite Number 4 Dual Electron Spectrometer FastSurvey-resolution auxiliary moments - J. Burch, B. Giles (SwRI, GSFC)

MMS4_FPI_FAST_L2_DES-PARTMOMS: MMS Satellite Number 4 Dual Electron Spectrometer FastSurvey-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS4_FPI_FAST_L2_DIS-DIST: MMS Satellite Number 4 Dual Ion Spectrometer FastSurvey-resolution instrument distributions - J. Burch, B. Giles (SwRI, GSFC)

MMS4_FPI_FAST_L2_DIS-MOMS: MMS Satellite Number 4 Dual Ion Spectrometer FastSurvey-resolution distribution moments - J. Burch, B. Giles (SwRI, GSFC)

MMS4_FPI_FAST_L2_DIS-MOMSAUX: MMS Satellite Number 4 Dual Ion Spectrometer FastSurvey-resolution auxiliary moments - J. Burch, B. Giles (SwRI, GSFC)

MMS4_FPI_FAST_L2_DIS-PARTMOMS: MMS Satellite Number 4 Dual Ion Spectrometer FastSurvey-resolution partial moments - J. Burch, B. Giles (SwRI, GSFC)

MMS4_FPI_SLOW_L2_DES-DIST: MMS Satellite Number 4 Dual Electron Spectrometer SlowSurvey-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS4_FPI_SLOW_L2_DES-MOMS: MMS Satellite Number 4 Dual Electron Spectrometer SlowSurvey-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS4_FPI_SLOW_L2_DES-MOMSAUX: MMS Satellite Number 4 Dual Electron Spectrometer SlowSurvey-resolution auxiliary moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS4_FPI_SLOW_L2_DIS-DIST: MMS Satellite Number 4 Dual Ion Spectrometer SlowSurvey-resolution instrument distributions - J. Burch, D. Gershman (SwRI, GSFC)

MMS4_FPI_SLOW_L2_DIS-MOMS: MMS Satellite Number 4 Dual Ion Spectrometer SlowSurvey-resolution distribution moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS4_FPI_SLOW_L2_DIS-MOMSAUX: MMS Satellite Number 4 Dual Ion Spectrometer SlowSurvey-resolution auxiliary moments - J. Burch, D. Gershman (SwRI, GSFC)

MMS4_HPCA_BRST_L2_ION: Level 2> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS4_HPCA_BRST_L2_MOMENTS: Level 2 Moments> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS4_HPCA_SRVY_L2_ION: Level 2> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS4_HPCA_SRVY_L2_MOMENTS: Level 2 Moments> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS4_HPCA_SRVY_L2_TOF-COUNTS: Level 1b> Hot Plasma Composition Analyzer - J. Burch, S. Fuselier (SWRI)

MMS4_MEC_BRST_L2_EPHT89D: Magnetic ephemeris and support data for MMS satellite number 4 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS4_MEC_BRST_L2_EPHT89Q: Magnetic ephemeris and support data for MMS satellite number 4 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS4_MEC_BRST_L2_EPHTS04D: Magnetic ephemeris and support data for MMS satellite number 4 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS4_MEC_SRVY_L2_EPHT89D: Magnetic ephemeris and support data for MMS satellite number 4 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS4_MEC_SRVY_L2_EPHT89Q: Magnetic ephemeris and support data for MMS satellite number 4 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS4_MEC_SRVY_L2_EPHTS04D: Magnetic ephemeris and support data for MMS satellite number 4 - M. G. Henderson, S. K. Morley (Los Alamos National Laboratory (LANL))

MMS4_R0_SUMMARY: Links to MMS-4 pre-generated Quicklook Summary plots - James Burch (SWRI)

MMS4_SCM_BRST_L2_SCB: Level 2 Search Coil Magnetometer AC Magnetic Field Burst (8192S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS4_SCM_BRST_L2_SCHB: Level 2 Search Coil Magnetometer AC Magnetic Field High Burst (16384S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MMS4_SCM_SRVY_L2_SCSRVY: Level 2 Search Coil Magnetometer AC Magnetic Field Survey (32S/s) Data - J. Burch, O. Le Contel (SWRI, LPP)

MOON_HELIO1HR_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)

MSL_RAD_OBS-L1: MSL/RAD Level 1 observational counter data - D. Hassler (SwRI-Boulder)

MSL_RAD_OBS-L2: MSL/RAD Level 2 observational radiation data - D. Hassler (SwRI-Boulder)

MUNIN_M1_MDSE: MUNIN, MEDUSA IDFS format - David Winningham (Southwest Research Institute)

MUNIN_M1_MDSI: MUNIN, MEDUSA IDFS format - David Winningham (Southwest Research Institute)

MUNIN_M1_OA: MUNIN, Orbit and attitude data IDFS format - Rymd Plasma Gruppen (Swedish Institute of Space Physics)

MVN_INSITU_KP-4SEC: MAVEN In-situ Key Parameters - B.M. Jakosky (LASP/U. Colorado)

MVN_MAG_L2-SUNSTATE-1SEC: MAVEN Magnetometer Sun-State 1 Second Magnetic Field - J. Connerney (NASA GSFC)

MVN_SEP_L2_S1-CAL-SVY-FULL: DERIVED FROM: MAVEN SEP (Solar Energetic Particle) Instrument - D. Larson (davin@ssl.berkeley.edu) (U.C. Berkeley Space Sciences Laboratory)

MVN_SEP_L2_S2-CAL-SVY-FULL: DERIVED FROM: MAVEN SEP (Solar Energetic Particle) Instrument - D. Larson (davin@ssl.berkeley.edu) (U.C. Berkeley Space Sciences Laboratory)

MVN_STA_L2_D8-12R1E: MAVEN Supra-Thermal And Thermal Ion Composition Particle Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)

MVN_STA_L2_D9-12R64E: MAVEN Supra-Thermal And Thermal Ion Composition Particle Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)

MVN_STA_L2_DA-1R64E: MAVEN Supra-Thermal And Thermal Ion Composition Particle Distributions - J. P. McFadden (U.C. Berkeley Space Sciences Laboratory)

MVN_SWE_L2_ARC3D: DERIVED FROM: MAVEN SWEA (Solar Wind Electron Analyzer) 3D Distributions - David L. Mitchell (mitchell@ssl.berkeley.edu) (UC Berkeley Space Sciences Laboratory)

MVN_SWE_L2_ARCPAD: DERIVED FROM: MAVEN SWEA (Solar Wind Electron Analyzer) Pitch Angle Distributions - David L. Mitchell (mitchell@ssl.berkeley.edu) (UC Berkeley Space Sciences Laboratory)

MVN_SWE_L2_SVY3D: DERIVED FROM: MAVEN SWEA (Solar Wind Electron Analyzer) 3D Distributions - David L. Mitchell (mitchell@ssl.berkeley.edu) (UC Berkeley Space Sciences Laboratory)

MVN_SWE_L2_SVYPAD: DERIVED FROM: MAVEN SWEA (Solar Wind Electron Analyzer) Pitch Angle Distributions - David L. Mitchell (mitchell@ssl.berkeley.edu) (UC Berkeley Space Sciences Laboratory)

MVN_SWE_L2_SVYSPEC: DERIVED FROM: MAVEN SWEA (Solar Wind Electron Analyzer) Energy Spectra - David L. Mitchell (mitchell@ssl.berkeley.edu) (UC Berkeley Space Sciences Laboratory)

MVN_SWI_L2_COARSEARC3D: DERIVED FROM: MAVEN SWIA (Solar Wind Ion Analyzer), Coarse 3d Distributions - J.S. Halekas (U Iowa)

MVN_SWI_L2_COARSESVY3D: DERIVED FROM: MAVEN SWIA (Solar Wind Ion Analyzer), Coarse 3d Distributions - J.S. Halekas (U Iowa)

MVN_SWI_L2_FINEARC3D: DERIVED FROM: MAVEN SWIA (Solar Wind Ion Analyzer), Fine 3d Distributions - J.S. Halekas (U Iowa)

MVN_SWI_L2_FINESVY3D: DERIVED FROM: MAVEN SWIA (Solar Wind Ion Analyzer), Fine 3d Distributions - J.S. Halekas (U Iowa)

MVN_SWI_L2_ONBOARDSVYMOM: DERIVED FROM: MAVEN SWIA (Solar Wind Ion Analyzer), Onboard Moments - J.S. Halekas (U Iowa)

MVN_SWI_L2_ONBOARDSVYSPEC: DERIVED FROM: MAVEN SWIA (Solar Wind Ion Analyzer), Onboard Energy Spectra - J.S. Halekas (U Iowa)

MARINER2_HELIO1HR_POSITION doi:10.48322/me2b-8q74
Proper citations should include the "Accessed on date" in the form .

Description

No TEXT global attribute value.

Data Variable Descriptions

Dataset in CDAWeb
Data Access Code Examples written in

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MARINER2_R0_MAGPLASMA

Description

Mariner2 COHOweb connection

Data Variable Descriptions

Dataset in CDAWeb
Data Access Code Examples written in

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MARS_HELIO1HR_POSITION

Description

No TEXT global attribute value.

Data Variable Descriptions

Dataset in CDAWeb
Data Access Code Examples written in

and IDL®.
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MAVEN_HELIO1HR_POSITION doi:10.48322/90ar-hx32
Proper citations should include the "Accessed on date" in the form .

Description

No TEXT global attribute value.

Data Variable Descriptions

Dataset in CDAWeb
Data Access Code Examples written in

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MERCURY_HELIO1HR_POSITION

Description

No TEXT global attribute value.

Data Variable Descriptions

Dataset in CDAWeb
Data Access Code Examples written in

and IDL®.
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MESSENGER_HELIO1HR_POSITION doi:10.48322/sx90-xh93
Proper citations should include the "Accessed on date" in the form .

Description

No TEXT global attribute value.

Data Variable Descriptions

Dataset in CDAWeb
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MESSENGER_MAG_RTN (spase://NASA/NumericalData/MESSENGER/MAG/PT0.05S)

Description

The Mercury Surface, Space Environment, Geochemistry and Ranging (MESSENGER)
mission is designed to study the characteristics and environment of Mercury from
orbit. Specifically, the scientific objectives of the mission are to
characterize the chemical composition of Mercury's surface, the geologic
history, the nature of the magnetic field, the size and state of the core, the
volatile inventory at the poles, and the nature of Mercurys exosphere and
magnetosphere over a nominal orbital mission of one Earth year
MESSENGER launched on 3 August 2004 at 6:15:56 UT (2:15:56 a.m. EDT) on a Delta
7925H (a Delta II Heavy launch vehicle with nine strap-on solid-rocket
boosters). The spacecraft was injected into solar orbit 57 minutes later.  The
solar panels were then deployed and the spacecraft began sending data on its
status. One year after launch, on 2 August 2005, MESSENGER flew by Earth at an
altitude of 2347 km. On 12 December 2005 at 11:30 UT, MESSENGER fired its large
thruster for 524 seconds, changing the spacecraft velocity by 316 m/s and
putting it on course for its 24 October 2006 Venus flyby at an altitude of 2990
km. The second Venus flyby took place on 5 June 2007 at 23:08 UT (7:08 p.m. EDT)
at an altitude of approximately 337 km. The first of three Mercury flybys, all
at roughly 200 km altitude, occurred on 14 January 2008 at 19:04:39 UT, and the
second on 6 October 2008 at 08:40:22 UT.  The third will be on 29 September
2009. There are also five deep space manuevers. Data collected during the
Mercury flybys will be used to help plan the scientific campaign during the
orbital phase. Mercury orbit insertion will take place on 18 March 2011,
requiring a delta-V of 0.867 km/s. The nominal orbit is planned to have a
periapsis of 200 km at 60 degrees N latitude, an apoapsis of 15,193 km, a period
of 12 hours and an inclination of 80 degrees. The periapsis will slowly rise due
to solar perturbations to over 400 km at the end of 88 days (one Mercury year)
at which point it will be readjusted to a 200 km, 12 hour orbit via a two burn
sequence. Data will be collected from orbit for one Earth year, the nominal end
of the primary mission will be in March 2012.  Global stereo image coverage at
250 m/pixel resolution is expected. The mission should also yield global
composition maps, a 3-D model of Mercury's magnetosphere, topographic profiles
of the northern hemisphere, gravity field to degree and order 16, altitude
profiles of elemental species, and a characterization of the volatiles in
permanently shadowed craters at the poles.
The MESSENGER spacecraft is a squat box (1.27 m x 1.42 m x 1.85 m) with a
semi-cylindrical thermal shade (roughly 2.5 meters tall and 2 meters wide) for
protection from the Sun and two solar panel wings extending radially about 6
meters from tip to tip.  A 3.6 m magnetometer boom also extends from the craft.
The total mass of the spacecraft is 1093 kg, 607.8 kg of this is propellant and
helium. The structure is primarily graphite-cyanate-ester (GrCE) composite and
consists of two vertical panels which support two large fuel tanks and two
vertical panels which support the oxidizer tank and plumbing panel. The four
vertical panels make up the center column and are bolted at their aft ends to an
aluminum adapter. A single top deck panel mounts the LVA (large velocity adjust)
thruster, small thrusters, helium and auxiliary fuel tanks, star trackers and
battery.
Main propulsion is via the 645-N, 317-s bipropellant LVA thruster, four 22-N
monopropellant thrusters provide spacecraft steering during main thruster burns,
and ten 4-N monopropellant thrusters are used for attitude control. There is
also a reaction-wheel attitude control system. Knowledge for attitude control is
provided by star tracking cameras, an inertial measurement unit, and six solar
sensors. Power is provided by the solar panels, which extend beyond the sunshade
and are rotatable to balance panel temperature and power generation, which
provides a nominal 450 W in Mercury orbit. The panels are 70% optical solar
reflectors and 30% GaAs/Ge cells. The power is stored in a
common-pressure-vessel nickel-hydrogen battery, with 11 vessels and 2 cells per
vessel.
Communications are in X-band with downlink through two fixed phased-array
antenna clusters and uplink and downlink through medium- and low-gain antennas
on the forward and aft sides of the spacecraft. Passive thermal control,
primarily a fixed opaque ceramic cloth sunshade, is utilized to maintain
operating temperatures near the Sun. Radiators are built into the structure and
the orbit is optimized to minimize infrared and visible light heating of the
spacecraft from the surface of Mercury. Multilayer insulation, low conductivity
couplings, and heaters are also used to maintain temperatures within operating
limits.
Five science instruments are mounted externally on the bottom deck of the main
body: the Mercury Dual Imaging System (MDIS), Gamma-Ray and Neutron Spectrometer
(GRNS), X-ray Spectrometer (XRS), Mercury Laser Altimeter (MLA), and Atmospheric
and Surface Composition Spectrometer (MASCS). The Energetic Particle and Plasma
Spectrometer (EPPS) is mounted on the side and top deck and the magnetometer
(MAG) is at the end of the 3.6 m boom. Radio Science (RS) experiments will use
the existing communications system.
The Messenger MAG instrument is a miniature three-axis ring-core fluxgate
magnetometer with low-noise electronics. It is mounted on a 3.6 m boom in the
anti-sunward direction. The MAG has .. 1530 and ..51300 nT ranges with 20-bit
internal resolution and 17-bit output resolution. The MAG probe samples magnetic
field values along the X, Y, and Z axes at a rate of up to 20 samples/second
(commandable and can vary). This dataset has 3-axis calibrated samples of the
magnetic field in heliospheric RTN coordinates in units of nano-Tesla, Br, Bt,
Bn. The spacecraft position is identified by radial distance from the Sun,
latitude above the ecliptic plane, and azimuth with respect to the Earth-Sun
line in the ecliptic plane. 
Anderson, B. J., M. H. Acuna, D. A. Lohr , J. Scheifele, A. Raval, H. Korth, and
J. A. Slavin, \'The Magnetometer instrument on MESSENGER\', Space Science
Reviews, 2007.[ANDREWSETAL2007]

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METOP1_POES-SEM2_FLUXES-2SEC (spase://NOAA/NumericalData/MetOp/B/SEM-2/CDF/PT2S)

Description

POES N19 data: POES/MetOp: Particle Precipitation Data (These data have known
contamination problems. Please consult provider rob.redmon@noaa.gov for usage
recommendations.)

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METOP2_POES-SEM2_FLUXES-2SEC (spase://NOAA/NumericalData/MetOp/A/SEM-2/CDF/PT2S)

Description

POES N19 data: POES/MetOp: Particle Precipitation Data (These data have known
contamination problems. Please consult provider rob.redmon@noaa.gov for usage
recommendations.)

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METOP3_POES-SEM2_FLUXES-2SEC

Description

POES N19 data: POES/MetOp: Particle Precipitation Data (These data have known
contamination problems. Please consult provider rob.redmon@noaa.gov for usage
recommendations.)

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MGS_MAG_HIGH

Description

The Mars Global Surveyor magnetic field instrument consists of dual, triaxial
fluxgate magnetometers, capable of measuring fields between +/- 4 nT and +/-
65536 nT. Automated range switching allows the instrument to maintain maximum
digital resolution over a wide range of field strengths. The text of this
instrument description has been abstracted from the   instrument paper:  Acuna,
M. A., J. E. P. Connerney, P. Wasilewski, R. P. Lin,     K. A. Anderson, C. W.
Carlson, J. McFadden, D. W. Curtis, H. Reme,  A. Cros, J. L. Medale, J. A.
Sauvaud, C. d'Uston, S. J. Bauer,  P. Cloutier, M. Mayhew, and N. F. Ness, Mars
Observer Magnetic   Fields Investigation, J. Geophys. Res., 97, 7799-7814, 1992.

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MGS_MAG_LOW

Description

The Mars Global Surveyor magnetic field instrument consists of dual, triaxial
fluxgate magnetometers, capable of measuring fields between +/- 4 nT and +/-
65536 nT. Automated range switching allows the instrument to maintain maximum
digital resolution over a wide range of field strengths. The text of this
instrument description has been abstracted from the   instrument paper:  Acuna,
M. A., J. E. P. Connerney, P. Wasilewski, R. P. Lin,     K. A. Anderson, C. W.
Carlson, J. McFadden, D. W. Curtis, H. Reme,  A. Cros, J. L. Medale, J. A.
Sauvaud, C. d'Uston, S. J. Bauer,  P. Cloutier, M. Mayhew, and N. F. Ness, Mars
Observer Magnetic   Fields Investigation, J. Geophys. Res., 97, 7799-7814, 1992.

Data Variable Descriptions

Altitude [altitude]

Low Resolution. Calculated as the radius of Mars (= 3389.5 km) subtracted from
the spacecraft position.

Decimal Day [decimal_day]

Low resolution

Dynamic Range [dynamic_b_pl_range]

Gain range of the instrument at the time of the sample. Sample quantization is
gain range dependent. A negative value indicate a detail word (versus fullword)
entry.

Dynamic Spacecraft Field X [dynamic_bx_lpl]

Dynamic spacecraft field in payload  coordinates (this has been removed from the
measured field to compensate for spacecraft field); see sc_mod.ker at
https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds://PPI/MGS-M-MAG-3-MAP1_F
ULLWORD-RES-MAG-V1.0/GEOMETRY and
https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds://PPI/MGS-M-MAG-3-PREMAP
_FULLWORD-RES-MAG-V1.0/GEOMETRY Low resolution.

Dynamic Spacecraft Field Y [dynamic_by_lpl]

Dynamic spacecraft field in payload  coordinates (this has been removed from the
measured field to compensate for spacecraft field); see sc_mod.ker at
https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds://PPI/MGS-M-MAG-3-MAP1_F
ULLWORD-RES-MAG-V1.0/GEOMETRY and
https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds://PPI/MGS-M-MAG-3-PREMAP
_FULLWORD-RES-MAG-V1.0/GEOMETRY Low resolution.

Dynamic Spacecraft Field Z [dynamic_bz_lpl]

Dynamic spacecraft field in payload  coordinates (this has been removed from the
measured field to compensate for spacecraft field); see sc_mod.ker at
https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds://PPI/MGS-M-MAG-3-MAP1_F
ULLWORD-RES-MAG-V1.0/GEOMETRY and
https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds://PPI/MGS-M-MAG-3-PREMAP
_FULLWORD-RES-MAG-V1.0/GEOMETRY Low resolution.

Static Spacecraft Field Range [static_b_pl_range]

Static spacecraft fields are due to permanent magnetization, for example,
magnets or magnetized objects.

Static Spacecraft Field X [static_bx_lpl]

Static spacecraft field in payload X coordinates (this has been removed from the
measured field to compensate for spacecraft fields); see sc_mod.ker at
https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds://PPI/MGS-M-MAG-3-MAP1_F
ULLWORD-RES-MAG-V1.0/GEOMETRY and
https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds://PPI/MGS-M-MAG-3-PREMAP
_FULLWORD-RES-MAG-V1.0/GEOMETRY Low resolution.

Static Spacecraft Field Y [static_by_lpl]

Static Spacecraft Field Z [static_bz_lpl]

Magnetic Field Range Planetocentric [b_range_lpc]

Planetocentric, low resolution.

Magnetic Field Range MSO [b_range_lss]

Sun-state, ss, or MSO. Low resolution.

Magnetic Field X Planetocentric [bx_lpc]

Low resolution in planetocentric coordinates. Outboard.

Magnetic Field X MSO [bx_lss]

Magnetic Field Y Planetocentric [by_lpc]

Low resolution in planetocentric coordinates. Outboard.

Magnetic Field Y MSO [by_lss]

Low resolution in sun-state or MSO coordinates. Outboard.

Magnetic Field Z Planetocentric [bz_lpc]

Low resolution in planetocentric coordinates. Outboard.

Magnetic Field Z MSO [bz_lss]

Low resolution in sun-state or MSO coordinates. Outboard.

RMS Range Planetocentric [rms_range_lpc]

Low resolution, planetocentric.

RMS Range MSO [rms_range_lss]

Low resolution, sun-state/ss/MSO

RMS X Planetocentric [rms_x_lpc]

Root mean square of the outboard delta words (there are 23 delta words between
fullwords, sampled at either 32, 16, or 8 per second depending on date rate
allocation. Planetocentric, low resolution.

RMS X MSO [rms_x_lss]

RMS Y Planetocentric [rms_y_lpc]

RMS Y MSO [rms_y_lss]

Low resolution, sun-state/ss/MSO

RMS Z Planetocentric [rms_z_lpc]

Low resolution, planetocentric.

RMS Z MSO [rms_z_lss]

Low resolution, sun-state/ss/MSO

Solar Array Negative Y Current [sa_neg_y_low]

Solar array (-Y panel) current from sc engineering data base. A fill value of
'-99' is used when the solar array currents are negative.'-999' is used as a
fill value when the data is not available for the time.

Total Solar Array Current [sa_total_low]

Solar array output current (total) from sc engineering data base. A fill value
of '-99' is used when the solar array currents are negative.'-999' is used as a
fill value when the data is not available for the time.

Solar Array Positive Y Current [sa_plus_y_low]

Solar array (+Y panel) current from sc engineering data base. A fill value of
'-99' is used when the solar array currents are negative. '-999' is used as a
fill value when the data is not available for the time.

Spacecraft Position X Planetocentric [sc_pos_x_lpc]

Low resolution in planeocentric coordinates.

Spacecraft Position X MSO [sc_pos_x_lss]

Low resolution in sun-state or MSO coordinates.

Spacecraft Position Y Planetocentric [sc_pos_y_lpc]

Low resolution in planetocentric coordinates.

Spacecraft Position Y MSO [sc_pos_y_lss]

Low resolution in sun-state or MSO coordinates.

Spacecraft Position Z Planetocentric [sc_pos_z_lpc]

Low resolution in planetocentric coordinates.

Spacecraft Position Z MSO [sc_pos_z_lss]

Low resolution in sun-state or MSO coordinates.

Magnetic Field Magnitude [magnitude]

Magnitude calculated via the square root of the sum of the squares. Low
resolution data.

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MMS1_ASPOC_SRVY_L2 (spase://NASA/NumericalData/MMS/1/ASPOC/Survey/Level2/PT1S)

Description

K. Torkar et al, Active Spacecraft Potential Control Investigation
Space Science Reviews, 2014, DOI: 10.1007/s11214-014-0049-3
Further information:
- http://www.iwf.oeaw.ac.at/en/research/near-earth-space/mms/ 
- http://mms.space.swri.edu/

Modification History

150224 Initial version
150831 Minor updates and fixes
160205 CDF file format guide compliant

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MMS1_DSP_FAST_L2_BPSD (spase://NASA/NumericalData/MMS/1/FIELDS/DSP/Fast/Level2/MagneticFieldPowerSpectralDensity/PT2S)

Description

BPSD is the low frequency B spectral density covering the frequency range of .2
to 6000 Hz.

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MMS1_DSP_FAST_L2_EPSD (spase://NASA/NumericalData/MMS/1/FIELDS/DSP/Fast/Level2/ElectricFieldPowerSpectralDensity/PT2S)

Description

EPSD combines the low frequency E spectral density covering the frequency range
of 1 to 8000 Hz and the  medium frequency E spectral density covering the
frequency range of .25 to 100 kHz.

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MMS1_DSP_SLOW_L2_BPSD (spase://NASA/NumericalData/MMS/1/FIELDS/DSP/Slow/Level2/MagneticFieldPowerSpectralDensity/PT16S)

Description

search coil magnetometer spectral density

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MMS1_DSP_SLOW_L2_EPSD (spase://NASA/NumericalData/MMS/1/FIELDS/DSP/Slow/Level2/ElectricFieldPowerSpectralDensity/PT16S)

Description

electric spectral density

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MMS1_EDI_BRST_L2_AMB (spase://NASA/NumericalData/MMS/1/FIELDS/EDI/Burst/Level2/ElectronFluxAmbient/ProjectionMethod1/PT0.0009765625S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - Original version.
v1.0.0 - Include trajectory vectors and optics state.
v1.1.0 - Update metadata: counts -> flux.
v1.2.0 - Added flux error.
v1.3.0 - Trajectory vector errors are now deltas.
v1.4.0 - Fixed dead-time correction and error values.
v1.5.0 - Factor of 2 for accumulation time & 2 for abscal factor in srvy mode.
v1.6.0 - No factor of 2 for accumulation time in srvy mode.
v2.0.0 - Reduced file size with scalar errors. Update metadata.
v2.1.0 - Correct fill value for fluxes.
v3.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v4.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.

Data Variable Descriptions

Optics state [mms1_edi_optics_state_brst_l2]

---> GDU1 energy [mms1_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms1_edi_energy_gdu2_brst_l2]

Flux for electrons with trajectories given by Traj-1 0PA [mms1_edi_flux1_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-1 0PA [mms1_edi_flux1_0_brst_l2_noerr]

---> Error for flux1 0-degree pitch angle electron flux. [mms1_edi_flux1_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-2 0PA [mms1_edi_flux2_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-2 0PA [mms1_edi_flux2_0_brst_l2_noerr]

---> Error for flux2 0-degree pitch angle electron flux. [mms1_edi_flux2_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-3 0PA [mms1_edi_flux3_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-3 0PA [mms1_edi_flux3_0_brst_l2_noerr]

---> Error for flux3 0-degree pitch angle electron flux. [mms1_edi_flux3_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-4 0PA [mms1_edi_flux4_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-4 0PA [mms1_edi_flux4_0_brst_l2_noerr]

---> Error for flux4 0-degree pitch angle electron flux. [mms1_edi_flux4_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-1 180PA [mms1_edi_flux1_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-1 180PA [mms1_edi_flux1_180_brst_l2_noerr]

---> Error for flux1 180-degree pitch angle electron flux. [mms1_edi_flux1_180_delta_brst_l2]

Flux for electrons with trajectories given by traj2 180PA [mms1_edi_flux2_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-2 180PA [mms1_edi_flux2_180_brst_l2_noerr]

---> Error for flux2 180-degree pitch angle electron flux. [mms1_edi_flux2_180_delta_brst_l2]

Flux for electrons with trajectories given by traj3 180PA [mms1_edi_flux3_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-3 180PA [mms1_edi_flux3_180_brst_l2_noerr]

---> Error for flux3 180-degree pitch angle electron flux. [mms1_edi_flux3_180_delta_brst_l2]

Flux for electrons with trajectories given by traj4 180PA [mms1_edi_flux4_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-4 180PA [mms1_edi_flux4_180_brst_l2_noerr]

---> Error for flux4 180-degree pitch angle electron flux. [mms1_edi_flux4_180_delta_brst_l2]

Trajectory of flux1 0-degree pitch angle electrons in GSE coordinates. [mms1_edi_traj1_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 0-degree pitch angle electrons in GSE coordinates. [mms1_edi_traj2_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 0-degree pitch angle electrons in GSE coordinates. [mms1_edi_traj3_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 0-degree pitch angle electrons in GSE coordinates. [mms1_edi_traj4_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 180-degree pitch angle electrons in GSE coordinates. [mms1_edi_traj1_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 180-degree pitch angle electrons in GSE coordinates. [mms1_edi_traj2_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 180-degree pitch angle electrons in GSE coordinates. [mms1_edi_traj3_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 180-degree pitch angle electrons in GSE coordinates. [mms1_edi_traj4_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj1_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 0-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj2_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 0-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj3_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 0-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj4_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj1_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 180-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj2_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 180-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj3_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 180-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj4_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms1_edi_traj1_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms1_edi_traj2_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms1_edi_traj3_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms1_edi_traj4_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms1_edi_traj1_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms1_edi_traj2_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms1_edi_traj3_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms1_edi_traj4_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS1_EDI_BRST_L2_AMB-PM2 (spase://NASA/NumericalData/MMS/1/FIELDS/EDI/Burst/Level2/AmbientElectronFlux/ProjectionMethod2/PT0.0009765625S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v1.0.0 - Original version.
v1.1.0 - Correct fill value for fluxes.
v2.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v3.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.
v4.0.0 - Each trajectory has its own LABL_PTR_1 variable.

Data Variable Descriptions

Optics state [mms1_edi_optics_state_brst_l2]

---> GDU1 energy [mms1_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms1_edi_energy_gdu2_brst_l2]

Field-aligned electron flux from channel 1 of both GDUs [mms1_edi_flux1_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 1 of both GDUs [mms1_edi_flux1_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 1 of both GDUs. [mms1_edi_flux1_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 1 of both GDUs [mms1_edi_flux1_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 1 of both GDUs [mms1_edi_flux1_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 1 of both GDUs. [mms1_edi_flux1_180_delta_brst_l2]

Field-aligned electron flux from channel 2 of both GDUs [mms1_edi_flux2_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 2 of both GDUs [mms1_edi_flux2_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 2 of both GDUs. [mms1_edi_flux2_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 2 of both GDUs [mms1_edi_flux2_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 2 of both GDUs [mms1_edi_flux2_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 2 of both GDUs. [mms1_edi_flux2_180_delta_brst_l2]

Field-aligned electron flux from channel 3 of both GDUs [mms1_edi_flux3_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 3 of both GDUs [mms1_edi_flux3_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 3 of both GDUs. [mms1_edi_flux3_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 3 of both GDUs [mms1_edi_flux3_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 3 of both GDUs [mms1_edi_flux3_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 3 of both GDUs. [mms1_edi_flux3_180_delta_brst_l2]

Field-aligned electron flux from channel 4 of both GDUs [mms1_edi_flux4_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 4 of both GDUs [mms1_edi_flux4_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 4 of both GDUs. [mms1_edi_flux4_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 4 of both GDUs [mms1_edi_flux4_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 4 of both GDUs [mms1_edi_flux4_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 4 of both GDUs. [mms1_edi_flux4_180_delta_brst_l2]

Trajectory of field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms1_edi_traj1_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms1_edi_traj1_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 1 of both GDUs in GSE coordinates. [mms1_edi_traj1_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs, in GSE coordinates. [mms1_edi_traj1_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms1_edi_traj2_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms1_edi_traj2_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in GSE coordinates. [mms1_edi_traj2_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs, in GSE coordinates. [mms1_edi_traj2_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms1_edi_traj3_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms1_edi_traj3_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in GSE coordinates. [mms1_edi_traj3_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs, in GSE coordinates. [mms1_edi_traj3_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms1_edi_traj4_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms1_edi_traj4_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in GSE coordinates. [mms1_edi_traj4_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs, in GSE coordinates. [mms1_edi_traj4_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj1_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj1_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS1_EDI_BRST_L2_EFIELD (spase://NASA/NumericalData/MMS/1/FIELDS/EDI/Burst/Level2/ElectricField/PT0.0009765625S)

Description

EDI electric field data. Instrument papers for EDI can be found at:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7

Modification History

v1.0.0 - First version. TRI-TOF selection based on smallest error.
v1.1.0 - TRI-TOF merged by weighted average.
v1.2.0 - Fixed t_delta_plus/minus CDF_type.
v1.3.0 - Fixed Fixed vdrift SI conversion.
v1.4.0 - Fixed data duplication caused by multiple l2pre file locations.
v1.5.0 - Inplemented baseline*beams*Bmag filter for triangulation.
v1.6.0 - Inplemented null files for no or low quality data.

Data Variable Descriptions

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MMS1_EDI_BRST_L2_Q0 (spase://NASA/NumericalData/MMS/1/FIELDS/EDI/Burst/Level2/QualityZero/PT0.0078125S)

Description

EDI Q0 data. The EDI instrument paper and data products guidescan be found at
the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - First version.
v0.0.1 - Filled energy variables.
v0.0.2 - Energy written properly.
v1.0.0 - Update variable names.
v1.1.0 - Added optics state.
v2.0.0 - Added electron trajectories.
v2.1.0 - Deltas on trajectory vectors are now deltas.
v3.0.0 - Reduced file size with scalar errors. Add VAR_NOTES.
v3.1.0 - Fixed optics datatype.
v4.0.0 - Removed unused Epoch variable.
v5.0.0 - Trajectories are provided in DBCS coordinates.

Data Variable Descriptions

Optics state [mms1_edi_optics_state_brst_l2]

---> GDU1 energy [mms1_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms1_edi_energy_gdu2_brst_l2]

GDU1 quality 0 counts. [mms1_edi_counts_gdu1_brst_l2]

Q0 data consists of raw electron counts. The error at any one time is the
square-root of the counts. Note that there may be contamination from the EDI
electron beams. See the data products guide or contact an EDI team member to
learn about beam contamination.

GDU2 quality 0 counts. [mms1_edi_counts_gdu2_brst_l2]

GDU1 electron incident trajectory vectors in spherical BCS coordinates. [mms1_edi_traj_bcs_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical BCS coordinates. [mms1_edi_traj_bcs_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical DBCS coordinates. [mms1_edi_traj_dbcs_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical DBCS coordinates. [mms1_edi_traj_dbcs_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSE coordinates. [mms1_edi_traj_gse_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSE coordinates. [mms1_edi_traj_gse_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSM coordinates. [mms1_edi_traj_gsm_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSM coordinates. [mms1_edi_traj_gsm_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS1_EDI_SRVY_L2_AMB (spase://NASA/NumericalData/MMS/1/FIELDS/EDI/Survey/Level2/ElectronFluxAmbient/ProjectionMethod1/PT0.03125S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - Original version.
v1.0.0 - Include trajectory vectors and optics state.
v1.1.0 - Update metadata: counts -> flux.
v1.2.0 - Added flux error.
v1.3.0 - Trajectory vector errors are now deltas.
v1.4.0 - Fixed dead-time correction and error values.
v1.5.0 - Factor of 2 for accumulation time & 2 for abscal factor in srvy mode.
v1.6.0 - No factor of 2 for accumulation time in srvy mode.
v2.0.0 - Reduced file size with scalar errors. Update metadata.
v2.1.0 - Correct fill value for fluxes.
v3.0.0 - Omni-directional error for trajectories. Correct time deltas. Y-Version
linked to cal file. Single epoch for counts.
v4.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.

Data Variable Descriptions

Optics state [mms1_edi_optics_state_srvy_l2]

---> GDU1 energy [mms1_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms1_edi_energy_gdu2_srvy_l2]

Field-aligned electron flux from both GDUs [mms1_edi_flux1_0_srvy_l2]

---> (no error bars displayed) Field-aligned electron flux from both GDUs [mms1_edi_flux1_0_srvy_l2_noerr]

---> Error in field-aligned electron flux from both GDUs. [mms1_edi_flux1_0_delta_srvy_l2]

Anti-field-aligned electron flux from both GDUs [mms1_edi_flux1_180_srvy_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from both GDUs [mms1_edi_flux1_180_srvy_l2_noerr]

---> Error in anti-field-aligned electron flux from both GDUs. [mms1_edi_flux1_180_delta_srvy_l2]

Trajectory of field-aligned electrons from both GDUs in DBCS coordinates. [mms1_edi_traj1_dbcs_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs in DBCS coordinates. [mms1_edi_traj1_dbcs_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from both GDUs in GSE coordinates. [mms1_edi_traj1_gse_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs, in GSE coordinates. [mms1_edi_traj1_gse_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj1_gsm_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj1_gsm_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS1_EDI_SRVY_L2_AMB-PM2 (spase://NASA/NumericalData/MMS/1/FIELDS/EDI/Survey/Level2/ElectronFluxAmbient/ProjectionMethod2/PT0.03125S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v1.0.0 - Original version.
v1.1.0 - Correct fill value for fluxes.
v2.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v3.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.
v4.0.0 - Each trajectory has its own LABL_PTR_1 variable.

Data Variable Descriptions

Optics state [mms1_edi_optics_state_srvy_l2]

---> GDU1 energy [mms1_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms1_edi_energy_gdu2_srvy_l2]

Field-aligned electron flux from both GDUs [mms1_edi_flux1_0_srvy_l2]

---> (no error bars displayed) Field-aligned electron flux from both GDUs [mms1_edi_flux1_0_srvy_l2_noerr]

---> Error in field-aligned electron flux from both GDUs. [mms1_edi_flux1_0_delta_srvy_l2]

Anti-field-aligned electron flux from both GDUs [mms1_edi_flux1_180_srvy_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from both GDUs [mms1_edi_flux1_180_srvy_l2_noerr]

---> Error in anti-field-aligned electron flux from both GDUs. [mms1_edi_flux1_180_delta_srvy_l2]

Trajectory of field-aligned electrons from both GDUs in DBCS coordinates. [mms1_edi_traj1_dbcs_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs in DBCS coordinates. [mms1_edi_traj1_dbcs_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from both GDUs in GSE coordinates. [mms1_edi_traj1_gse_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs, in GSE coordinates. [mms1_edi_traj1_gse_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj1_gsm_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms1_edi_traj1_gsm_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS1_EDI_SRVY_L2_EFIELD (spase://NASA/NumericalData/MMS/1/FIELDS/EDI/Survey/Level2/ElectricField/PT5S)

Description

EDI electric field data. Instrument papers for EDI can be found at:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7

Modification History

v1.0.0 - First version. TRI-TOF selection based on smallest error.
v1.1.0 - TRI-TOF merged by weighted average.
v1.2.0 - Fixed t_delta_plus/minus CDF_type.
v1.3.0 - Fixed Fixed vdrift SI conversion.
v1.4.0 - Fixed data duplication caused by multiple l2pre file locations.
v1.5.0 - Inplemented baseline*beams*Bmag filter for triangulation.
v1.6.0 - Inplemented null files for no or low quality data.

Data Variable Descriptions

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MMS1_EDI_SRVY_L2_Q0 (spase://NASA/NumericalData/MMS/1/FIELDS/EDI/Survey/Level2/QualityZero/PT0.125S)

Description

EDI Q0 data. The EDI instrument paper and data products guidescan be found at
the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - First version.
v0.0.1 - Filled energy variables.
v0.0.2 - Energy written properly.
v1.0.0 - Update variable names.
v1.1.0 - Added optics state.
v2.0.0 - Added electron trajectories.
v2.1.0 - Deltas on trajectory vectors are now deltas.
v3.0.0 - Reduced file size with scalar errors. Add VAR_NOTES.
v4.0.0 - Removed unused Epoch variable.
v5.0.0 - Trajectories are provided in DBCS coordinates.

Data Variable Descriptions

Optics state [mms1_edi_optics_state_srvy_l2]

---> GDU1 energy [mms1_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms1_edi_energy_gdu2_srvy_l2]

GDU1 quality 0 counts. [mms1_edi_counts_gdu1_srvy_l2]

Q0 data consists of raw electron counts. The error at any one time is the
square-root of the counts. Note that there may be contamination from the EDI
electron beams. See the data products guide or contact an EDI team member to
learn about beam contamination.

GDU2 quality 0 counts. [mms1_edi_counts_gdu2_srvy_l2]

GDU1 electron incident trajectory vectors in spherical BCS coordinates. [mms1_edi_traj_bcs_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical BCS coordinates. [mms1_edi_traj_bcs_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical DBCS coordinates. [mms1_edi_traj_dbcs_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical DBCS coordinates. [mms1_edi_traj_dbcs_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSE coordinates. [mms1_edi_traj_gse_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSE coordinates. [mms1_edi_traj_gse_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSM coordinates. [mms1_edi_traj_gsm_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSM coordinates. [mms1_edi_traj_gsm_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS1_EDP_BRST_L2_DCE (spase://NASA/NumericalData/MMS/1/FIELDS/EDP/Burst/Level2/DCElectricField/PT0.0001220703125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS1_EDP_BRST_L2_HMFE (spase://NASA/NumericalData/MMS/1/FIELDS/EDP/Burst/Level2Pre/HMFE/PT0.00001525878906S)

Description

Data Variable Descriptions

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MMS1_EDP_BRST_L2_SCPOT doi:10.48322/7t5y-eq71
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

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MMS1_EDP_FAST_L2_DCE (spase://NASA/NumericalData/MMS/1/FIELDS/EDP/Fast/Level2/DCElectricField/PT0.03125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS1_EDP_FAST_L2_SCPOT doi:10.48322/jjsp-6g51
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

Data Variable Descriptions

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MMS1_EDP_SLOW_L2_DCE (spase://NASA/NumericalData/MMS/1/FIELDS/EDP/Slow/Level2/DCElectricField/PT0.125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS1_EDP_SLOW_L2_SCPOT doi:10.48322/5t77-ka57
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

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MMS1_EDP_SRVY_L2_HFESP (spase://NASA/NumericalData/MMS/1/FIELDS/EDP/Survey/Level2/HighFrequencyElectricFieldSpectra/PT16S)

Description

 AC Electric Field

Data Variable Descriptions

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MMS1_EPD-EIS_BRST_L2_EXTOF (spase://NASA/NumericalData/MMS/1/EnergeticParticleDetector/EIS/Burst/Level2/EnergyByTimeOfFlight/PT0.605S)

Description

empty

Modification History

Constantly modifying this code

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MMS1_EPD-EIS_BRST_L2_PHXTOF (spase://NASA/NumericalData/MMS/1/EnergeticParticleDetector/EIS/Burst/Level2/PulseHeightByTimeOfFlight/PT0.605S)

Description

empty

Modification History

Constantly modifying this code

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MMS1_EPD-EIS_SRVY_L2_ELECTRONENERGY (spase://NASA/NumericalData/MMS/1/EnergeticParticleDetector/EIS/Survey/Level2/ElectronEnergySpectra/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS1_EPD-EIS_SRVY_L2_EXTOF (spase://NASA/NumericalData/MMS/1/EnergeticParticleDetector/EIS/Survey/Level2/EnergyByTimeOfFlight/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS1_EPD-EIS_SRVY_L2_PHXTOF (spase://NASA/NumericalData/MMS/1/EnergeticParticleDetector/EIS/Survey/Level2/PulseHeightByTimeOfFlight/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS1_FEEPS_BRST_L2_ELECTRON (spase://NASA/NumericalData/MMS/1/EnergeticParticleDetector/FEEPS/Burst/Level2/Electron/PT0.3025S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS1_FEEPS_BRST_L2_ION (spase://NASA/NumericalData/MMS/1/EnergeticParticleDetector/FEEPS/Burst/Level2/Ion/PT0.3025S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS1_FEEPS_SRVY_L2_ELECTRON (spase://NASA/NumericalData/MMS/1/EnergeticParticleDetector/FEEPS/Survey/Level2/Electron/PT2.42S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS1_FEEPS_SRVY_L2_ION (spase://NASA/NumericalData/MMS/1/EnergeticParticleDetector/FEEPS/Survey/Level2/Ion/PT2.42S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS1_FGM_BRST_L2 (spase://NASA/NumericalData/MMS/1/FIELDS/FGM/Burst/Level2/PT0.0078125S)

Description

The Fluxgate Magnetometers (FGM) on Magnetospheric Multiscale consist of a
traditional Analog Fluxgate Magnetometer (AFG), and a Digital Fluxgate
magnetometer (DFG). The dual magnetometers are operated as a single instrument
providing a single intercalibrated data product. Range changes occur at
different times on the two instruments so the gains checked each periapsis can
be carried out unambiguously to apoapsis. Cross correlation of calibration
parameters can separate causes of the any apparent calibration changes. Use of
Electron Drift Instrument (EDI) to determine the field along the rotation axis
allows accurate monitoring of the zero levels along the rotation axis.  Prior to
launch the magnetometers were calibrated at the Technical University,
Braunschweig, except for the AFG magnetometers on MMS3 and MMS4, which were
calibrated at UCLA.  Both sets of sensors are operated for the entire MMS orbit,
with slow survey (8 samples per second) outside of the Region of Interest (ROI),
and fast survey (16 samples per second) inside the ROI. Within the ROI burst
mode data (128 samples per second) are also acquired.  A detailed description of
the MMS fluxgate magnetometers, including science objectives, instrument
description, calibration, magnetic cleanliness program, and data flow can be
found at http://link.springer.com/article/10.1007%2Fs11214-014-0057-3 (DOI 
10.1007/s11214-014-0057-3).Additional information can also be found at
http://www-spc.igpp.ucla.edu/ssc/mms (UCLA),and http://www.iwf.oeaw.ac.at (IWF,
Graz).
For the purpose of creating a unified FGM Level2 data product, burst mode data
is taken from DFG and survey mode data is taken from AFG.  Because AFG and DFG
are cross-calibrated on an orbit-averaged basis, small differences in offset may
be observed between Level2 burst and survey mode data.  Consequently, any
differences are within the error of the measurement. Based on preliminary
analysis of the data, the absolute error within the Region of Interest (ROI) is
estimated to be no more than 0.1 nT in the spin-plane, 0.15 nT along the
spin-axis and 0.2 nT in total magnitude.

Modification History

version X=5:  * Y-version number comes from cal file entries. 
              *
Ensures there are 2 ephemeris points before/after data to enable proper spline. 

              * Fix to depend_0 of rdeltahalf:  fixes bug when reading position
data.
              * L-vector for DMPA2GSE transformation is smoothed with a
gaussian filter, instead 
                of using a single average value for
the day.  This short-term filter avoids  
                introduding artificial
jumps at 00:00 UTC and removes 7-minute 'wobble' after  
               
maneuvers in the GSE result.   
              * Fixes error with DEFATT file
selection found when choosing the 
                daily DEFATT files to be used
in Phase 2.
              * Fixed bug where reference Etemp was used for high
range gain.  Now uses measured Etemp.
version X=4:  First version for public
release of L2.
              Renamed variables to conform with new MMS variable
name guidelines 
              (obs_instr_paramName[_coordSys]_mode_level):  
  
             Mag field parameters include 'b' for paramName.  
               
Use 'r' instead of 'pos' for S/C position paramName.  
               
Eliminated 'rate', replaced with 'bdeltahalf'.  Added 'rdeltahalf'.
            
   l1a_mode is now just 'mode'.
version X=3:  fixed removal of overlap between
modes.
              fixed a bug that caused stemp and etemp to be
empty.
version X=2:  flag parameter name corrected: was 'status'
               
        added bits 4, 5, 6 to flag saturation on B1, B2, and B3, respectively
  
                     added bit 7 to flag bad data at range changes
             
Added etemp and l1a_mode parameters.  
              rate, hirange, and stemp
parameters now comply with MMS CDF Guidlelines, e.g.
              FILLVAL now
defined for stemp and etemp, and is set to !values.f_nan
              No longer
use Var_Parents attribute in stemp -- see Parents instead
              In this
version, temperature-corrected gains are applied.  Reference temperatures are
used when 
              stemp or etemp are set to FILLVAL. 
             
Non-linearity correction is applied to high rage DFG data.
version X=1:  added
'flag', rate and hirange parameters (but 'flag' is actually called 'status')

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MMS1_FGM_SRVY_L2 (spase://NASA/NumericalData/MMS/1/FIELDS/FGM/Survey/Level2/PT0.125S)

Description

The Fluxgate Magnetometers (FGM) on Magnetospheric Multiscale consist of a
traditional Analog Fluxgate Magnetometer (AFG), and a Digital Fluxgate
magnetometer (DFG). The dual magnetometers are operated as a single instrument
providing a single intercalibrated data product. Range changes occur at
different times on the two instruments so the gains checked each periapsis can
be carried out unambiguously to apoapsis. Cross correlation of calibration
parameters can separate causes of the any apparent calibration changes. Use of
Electron Drift Instrument (EDI) to determine the field along the rotation axis
allows accurate monitoring of the zero levels along the rotation axis.  Prior to
launch the magnetometers were calibrated at the Technical University,
Braunschweig, except for the AFG magnetometers on MMS3 and MMS4, which were
calibrated at UCLA.  Both sets of sensors are operated for the entire MMS orbit,
with slow survey (8 samples per second) outside of the Region of Interest (ROI),
and fast survey (16 samples per second) inside the ROI. Within the ROI burst
mode data (128 samples per second) are also acquired.  A detailed description of
the MMS fluxgate magnetometers, including science objectives, instrument
description, calibration, magnetic cleanliness program, and data flow can be
found at http://link.springer.com/article/10.1007%2Fs11214-014-0057-3 (DOI 
10.1007/s11214-014-0057-3).Additional information can also be found at
http://www-spc.igpp.ucla.edu/ssc/mms (UCLA),and http://www.iwf.oeaw.ac.at (IWF,
Graz).
For the purpose of creating a unified FGM Level2 data product, burst mode data
is taken from DFG and survey mode data is taken from AFG.  Because AFG and DFG
are cross-calibrated on an orbit-averaged basis, small differences in offset may
be observed between Level2 burst and survey mode data.  Consequently, any
differences are within the error of the measurement. Based on preliminary
analysis of the data, the absolute error within the Region of Interest (ROI) is
estimated to be no more than 0.1 nT in the spin-plane, 0.15 nT along the
spin-axis and 0.2 nT in total magnitude.

Modification History

version X=5:  * Y-version number comes from cal file entries. 
              *
Ensures there are 2 ephemeris points before/after data to enable proper spline. 

              * Fix to depend_0 of rdeltahalf:  fixes bug when reading position
data.
              * L-vector for DMPA2GSE transformation is smoothed with a
gaussian filter, instead 
                of using a single average value for
the day.  This short-term filter avoids  
                introduding artificial
jumps at 00:00 UTC and removes 7-minute 'wobble' after  
               
maneuvers in the GSE result.   
              * Fixes error with DEFATT file
selection found when choosing the 
                daily DEFATT files to be used
in Phase 2.
              * Fixed bug where reference Etemp was used for high
range gain.  Now uses measured Etemp.
version X=4:  First version for public
release of L2.
              Renamed variables to conform with new MMS variable
name guidelines 
              (obs_instr_paramName[_coordSys]_mode_level):  
  
             Mag field parameters include 'b' for paramName.  
               
Use 'r' instead of 'pos' for S/C position paramName.  
               
Eliminated 'rate', replaced with 'bdeltahalf'.  Added 'rdeltahalf'.
            
   l1a_mode is now just 'mode'.
version X=3:  fixed removal of overlap between
modes.
              fixed a bug that caused stemp and etemp to be
empty.
version X=2:  flag parameter name corrected: was 'status'
               
        added bits 4, 5, 6 to flag saturation on B1, B2, and B3, respectively
  
                     added bit 7 to flag bad data at range changes
             
Added etemp and l1a_mode parameters.  
              rate, hirange, and stemp
parameters now comply with MMS CDF Guidlelines, e.g.
              FILLVAL now
defined for stemp and etemp, and is set to !values.f_nan
              No longer
use Var_Parents attribute in stemp -- see Parents instead
              In this
version, temperature-corrected gains are applied.  Reference temperatures are
used when 
              stemp or etemp are set to FILLVAL. 
             
Non-linearity correction is applied to high rage DFG data.
version X=1:  added
'flag', rate and hirange parameters (but 'flag' is actually called 'status')

Data Variable Descriptions

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MMS1_FPI_BRST_L2_DES-DIST (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DES/Burst/Level2/Distribution/PT0.03S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data are taken at burst (30/150 ms for DES/DIS)
resolution in this mode.  Data are also made available at survey (4.5 s, etc)
resolution; these form a separate product from this.  Per mission design, not
all burst-resolution data are downlinked.  This product contains phase-space
distribution maps of those burst-resolution data selected for downlink.  In
particular, the (highest possible quality at the time of release)
corrected/converted "Burst SkyMap" distributions are reported with time-stamps
and other annotation characterizing the state of the instrument system at the
indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

[CDAWeb List/Download/Create ONLY] MMS1 FPI/DES burst sky-map instrument distribution [mms1_des_dist_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 10.9 eV (E1/even) [mms1_des_dist_brst1_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 12.4 eV (E1/odd) [mms1_des_dist_brst1_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~11.6 eV (E1 even-odd) [mms1_des_dist_brst1_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 10.9 eV (E1/even) [mms1_des_dist_brst1_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 12.4 eV (E1/odd) [mms1_des_dist_brst1_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 37.9 eV (E6/even) [mms1_des_dist_brst6_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 42.9 eV (E6/odd) [mms1_des_dist_brst6_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~40.4 eV (E6 even-odd) [mms1_des_dist_brst6_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 37.9 eV (E6/even) [mms1_des_dist_brst6_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 42.9 eV (E6/odd) [mms1_des_dist_brst6_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 80.0 eV (E9/even) [mms1_des_dist_brst9_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 90.6 eV (E9/odd) [mms1_des_dist_brst9_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~85 eV (E9 even-odd) [mms1_des_dist_brst9_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 80.0 eV (E9/even) [mms1_des_dist_brst9_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 90.6 eV (E9/odd) [mms1_des_dist_brst9_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 169 eV (E12/even) [mms1_des_dist_brst12_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 191 eV (E12/odd) [mms1_des_dist_brst12_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~180 eV (E12 even-odd) [mms1_des_dist_brst12_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 169 eV (E12/even) [mms1_des_dist_brst12_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 191 eV (E12/odd) [mms1_des_dist_brst12_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 277 eV (E14/even) [mms1_des_dist_brst14_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 314 eV (E14/odd) [mms1_des_dist_brst14_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~295 eV (E14 even-odd) [mms1_des_dist_brst14_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 277 eV (E14/even) [mms1_des_dist_brst14_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 314 eV (E14/odd) [mms1_des_dist_brst14_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 456 eV (E16/even) [mms1_des_dist_brst16_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 517 eV (E16/odd) [mms1_des_dist_brst16_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~485 eV (E16 even-odd) [mms1_des_dist_brst16_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 456 eV (E16/even) [mms1_des_dist_brst16_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 517 eV (E16/odd) [mms1_des_dist_brst16_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 750 eV (E18/even) [mms1_des_dist_brst18_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 850 eV (E18/odd) [mms1_des_dist_brst18_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~800 eV (E18 even-odd) [mms1_des_dist_brst18_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 750 eV (E18/even) [mms1_des_dist_brst18_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 850 eV (E18/odd) [mms1_des_dist_brst18_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 1230 eV (E20/even) [mms1_des_dist_brst20_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 1400 eV (E20/odd) [mms1_des_dist_brst20_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~1310 eV (E20 even-odd) [mms1_des_dist_brst20_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1230 eV (E20/even) [mms1_des_dist_brst20_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1400 eV (E20/odd) [mms1_des_dist_brst20_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 2600 eV (E23/even) [mms1_des_dist_brst23_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 2950 eV (E23/odd) [mms1_des_dist_brst23_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~2770 eV (E23 even-odd) [mms1_des_dist_brst23_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2600 eV (E23/even) [mms1_des_dist_brst23_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2950 eV (E23/odd) [mms1_des_dist_brst23_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 5490 eV (E26/even) [mms1_des_dist_brst26_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 6210 eV (E26/odd) [mms1_des_dist_brst26_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~5840 eV (E26 even-odd) [mms1_des_dist_brst26_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5490 eV (E26/even) [mms1_des_dist_brst26_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 6210 eV (E26/odd) [mms1_des_dist_brst26_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 24400 eV (E32/even) [mms1_des_dist_brst32_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst sky-map instrument distribution - 27600 eV (E32/odd) [mms1_des_dist_brst32_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~26000 eV (E32 even-odd) [mms1_des_dist_brst32_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 24400 eV (E32/even) [mms1_des_dist_brst32_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 27600 eV (E32/odd) [mms1_des_dist_brst32_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[List/Create only in CDAWeb] 1-sigma error: MMS1 FPI/DES burst sky-map instrument distribution [mms1_des_disterr_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES burst average f1 count values [mms1_des_avgf1counts_brst]

Average f1-count level as a function of energy

MMS1 FPI/DES burst sky-map microsecond offsets from Epoch [mms1_des_steptimeoffsets_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order. Offsets reflect 128 steps over the 30 msec sweep
period. See FPI docs for details.

MMS1 FPI/DES vector of data-quality indicators at burst-start time [mms1_des_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS1 FPI/DES compression lossless/lossy indicator at survey-start time [mms1_des_compressionloss_brst]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

---> MMS1 FPI/DES step table parity, this burst [mms1_des_steptable_parity_brst]

FPI/DES alternates between two tables, designated "even" (0) and "odd" (1).

---> MMS1 FPI/DES Del-Phi (obs spin-phase) count at burst-start time [mms1_des_startdelphi_count_brst]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS1 FPI/DES Del-Phi (obs spin-phase) angle at burst-start time [mms1_des_startdelphi_angle_brst]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

---> MMS1 FPI/DES sector de-Spin P value, this burst [mms1_des_sector_despinp_brst]

Records P-value used to de-spin this burst sky-map on board.  See FPI docs for
details.

MMS1 FPI/DES burst sky-map instrument azimuthal angles [mms1_des_phi_brst]

see FPI docs for details

MMS FPI/DES burst sky-map parity 0/1 energies [mms1_des_energy_brst]

Energies (parity 0/1) in the 64-step FPI energy table

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MMS1_FPI_BRST_L2_DES-MOMS (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DES/Burst/Level2/Moments/PT0.03S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode.  Data are also made available at survey (4.5
s, etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked.  Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available.  This product contains results from
integrating the standard moments of phase-space distributions formed from the
indicated data type (DES/DIS burst, FS or SS).  For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS1_FPI_BRST_L2_DES-PARTMOMS (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DES/Burst/Level2/PartialMoments/PT0.03S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s,
etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked. Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available. This product contains partial moments that
come from performing the standard moment integrals over a limited portion of
velocity space. The resulting quantities are named similarly to their
corresponding standard moments, but are decorated with 'part' to differentiate.
For example, density_part is the density moment integrated from a particular
energy step to infinity. These partial moments are formed from the indicated
data type (DES/DIS burst, FS or SS). For convenience, some additional parameters
are included to augment those most commonly found in a moments product of this
sort, plus time-stamps and other annotation characterizing the state of the
instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DES vector of data-quality indicators at burst-start time [mms1_des_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of brst l2pre
magnetic field, Bit-9 = srvy l2pre magnetic field used instead of brst l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS1 FPI/DES partial electron number density during this burst [mms1_des_numberdensity_part_brst]

MMS1 FPI/DES partial electron bulk-velocity vector in DBCS during this burst [mms1_des_bulkv_part_dbcs_brst]

MMS1 FPI/DES partial electron bulk-velocity vector in GSE during this burst [mms1_des_bulkv_part_gse_brst]

MMS1 FPI/DES partial electron pressure tensor in DBCS during this burst [mms1_des_prestensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES partial electron pressure tensor in GSE during this burst [mms1_des_prestensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES partial electron temperature tensor in DBCS during this burst [mms1_des_temptensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES partial electron temperature tensor in GSE during this burst [mms1_des_temptensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES partial electron parallel temperature during this burst [mms1_des_temppara_part_brst]

MMS1 FPI/DES partial electron perpendicular temperature during this burst [mms1_des_tempperp_part_brst]

MMS1 FPI/DES recommended energy index during this burst [mms1_des_part_index_brst]

Recommended energy index during this burst

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MMS1_FPI_BRST_L2_DIS-DIST (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DIS/Burst/Level2/Distribution/PT0.15S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data are taken at burst (30/150 ms for DES/DIS)
resolution in this mode.  Data are also made available at survey (4.5 s, etc)
resolution; these form a separate product from this.  Per mission design, not
all burst-resolution data are downlinked.  This product contains phase-space
distribution maps of those burst-resolution data selected for downlink.  In
particular, the (highest possible quality at the time of release)
corrected/converted "Burst SkyMap" distributions are reported with time-stamps
and other annotation characterizing the state of the instrument system at the
indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

[CDAWeb List/Download/Create ONLY] MMS1 FPI/DIS burst sky-map instrument distribution [mms1_dis_dist_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 10.6 eV (E1/even) [mms1_dis_dist_brst1_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 12.0 eV (E1/odd) [mms1_dis_dist_brst1_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~11.3 eV (E1 even-odd) [mms1_dis_dist_brst1_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 10.6 eV (E1/even) [mms1_dis_dist_brst1_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 12.0 eV (E1/odd) [mms1_dis_dist_brst1_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 37.2 eV (E6/even) [mms1_dis_dist_brst6_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 42.1 eV (E6/odd) [mms1_dis_dist_brst6_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~39.6 eV (E6 even-odd) [mms1_dis_dist_brst6_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 37.2 eV (E6/even) [mms1_dis_dist_brst6_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 42.1 eV (E6/odd) [mms1_dis_dist_brst6_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 78.8 eV (E9/even) [mms1_dis_dist_brst9_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 89.3 eV (E9/odd) [mms1_dis_dist_brst9_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~83.9 eV (E9 even-odd) [mms1_dis_dist_brst9_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 78.8 eV (E9/even) [mms1_dis_dist_brst9_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 89.3 eV (E9/odd) [mms1_dis_dist_brst9_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 167 eV (E12/even) [mms1_dis_dist_brst12_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 189 eV (E12/odd) [mms1_dis_dist_brst12_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~178 eV (E12 even-odd) [mms1_dis_dist_brst12_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 167 eV (E12/even) [mms1_dis_dist_brst12_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 189 eV (E12/odd) [mms1_dis_dist_brst12_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 275 eV (E14/even) [mms1_dis_dist_brst14_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 312 eV (E14/odd) [mms1_dis_dist_brst14_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~293 eV (E14 even-odd) [mms1_dis_dist_brst14_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 275 eV (E14/even) [mms1_dis_dist_brst14_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 312 eV (E14/odd) [mms1_dis_dist_brst14_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 455 eV (E16/even) [mms1_dis_dist_brst16_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 515 eV (E16/odd) [mms1_dis_dist_brst16_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~484 eV (E16 even-odd) [mms1_dis_dist_brst16_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 455 eV (E16/even) [mms1_dis_dist_brst16_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 515 eV (E16/odd) [mms1_dis_dist_brst16_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 750 eV (E18/even) [mms1_dis_dist_brst18_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 850 eV (E18/odd) [mms1_dis_dist_brst18_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~800 eV (E18 even-odd) [mms1_dis_dist_brst18_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 750 eV (E18/even) [mms1_dis_dist_brst18_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 850 eV (E18/odd) [mms1_dis_dist_brst18_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 1240 eV (E20/even) [mms1_dis_dist_brst20_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 1400 eV (E20/odd) [mms1_dis_dist_brst20_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~1320 eV (E20 even-odd) [mms1_dis_dist_brst20_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1240 eV (E20/even) [mms1_dis_dist_brst20_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1400 eV (E20/odd) [mms1_dis_dist_brst20_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 2620 eV (E23/even) [mms1_dis_dist_brst23_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 2970 eV (E23/odd) [mms1_dis_dist_brst23_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~2800 eV (E23 even-odd) [mms1_dis_dist_brst23_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2620 eV (E23/even) [mms1_dis_dist_brst23_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2970 eV (E23/odd) [mms1_dis_dist_brst23_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 5560 eV (E26/even) [mms1_dis_dist_brst26_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 6300 eV (E26/odd) [mms1_dis_dist_brst26_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~5920 eV (E26 even-odd) [mms1_dis_dist_brst26_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5560 eV (E26/even) [mms1_dis_dist_brst26_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 6300 eV (E26/odd) [mms1_dis_dist_brst26_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 25000 eV (E32/even) [mms1_dis_dist_brst32_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS burst sky-map instrument distribution - 28300 eV (E32/odd) [mms1_dis_dist_brst32_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~26600 eV (E32 even-odd) [mms1_dis_dist_brst32_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 25000 eV (E32/even) [mms1_dis_dist_brst32_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 28300 eV (E32/odd) [mms1_dis_dist_brst32_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[List/Create only in CDAWeb] 1-sigma error: MMS1 FPI/DIS burst sky-map instrument distribution [mms1_dis_disterr_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS vector of data-quality indicators at burst-start time [mms1_dis_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS1 FPI/DIS compression lossless/lossy indicator at survey-start time [mms1_dis_compressionloss_brst]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

---> MMS1 FPI/DIS step table parity, this burst [mms1_dis_steptable_parity_brst]

FPI/DIS alternates between two tables, designated "even" (0) and "odd" (1).

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) count at burst-start time [mms1_dis_startdelphi_count_brst]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at burst-start time [mms1_dis_startdelphi_angle_brst]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS1 FPI/DIS burst average f1 count values [mms1_dis_avgf1counts_brst]

Average f1-count level as a function of energy

MMS1 FPI/DIS burst sky-map microsecond offsets from Epoch [mms1_dis_steptimeoffsets_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order. Offsets reflect 128 steps over the 150 msec sweep
period. See FPI docs for details.

---> MMS1 FPI/DIS sector de-Spin P value, this burst [mms1_dis_sector_despinp_brst]

Records P-value used to de-spin this burst sky-map on board.  See FPI docs for
details.

MMS1 FPI/DIS burst sky-map instrument azimuthal angles [mms1_dis_phi_brst]

see FPI docs for details

MMS FPI/DIS burst sky-map parity 0/1 energies [mms1_dis_energy_brst]

Energies (parity 0/1) in the 64-step FPI energy table

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MMS1_FPI_BRST_L2_DIS-MOMS (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DIS/Burst/Level2/Moments/PT0.15S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode.  Data are also made available at survey (4.5
s, etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked.  Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available.  This product contains results from
integrating the standard moments of phase-space distributions formed from the
indicated data type (DES/DIS burst, FS or SS).  For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS1_FPI_BRST_L2_DIS-PARTMOMS (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DIS/Burst/Level2/PartialMoments/PT0.15S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s,
etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked. Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available. This product contains partial moments that
come from performing the standard moment integrals over a limited portion of
velocity space. The resulting quantities are named similarly to their
corresponding standard moments, but are decorated with 'part' to differentiate.
For example, density_part is the density moment integrated from a particular
energy step to infinity. These partial moments are formed from the indicated
data type (DES/DIS burst, FS or SS). For convenience, some additional parameters
are included to augment those most commonly found in a moments product of this
sort, plus time-stamps and other annotation characterizing the state of the
instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DIS vector of data-quality indicators at burst-start time [mms1_dis_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of brst l2pre
magnetic field, Bit-9 = srvy l2pre magnetic field used instead of brst l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS1 FPI/DIS partial ion number density during this burst [mms1_dis_numberdensity_part_brst]

MMS1 FPI/DIS partial ion bulk-velocity vector in DBCS during this burst [mms1_dis_bulkv_part_dbcs_brst]

MMS1 FPI/DIS partial ion bulk-velocity vector in GSE during this burst [mms1_dis_bulkv_part_gse_brst]

MMS1 FPI/DIS partial ion pressure tensor in DBCS during this burst [mms1_dis_prestensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS partial ion pressure tensor in GSE during this burst [mms1_dis_prestensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS partial ion temperature tensor in DBCS during this burst [mms1_dis_temptensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS partial ion temperature tensor in GSE during this burst [mms1_dis_temptensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS partial ion parallel temperature during this burst [mms1_dis_temppara_part_brst]

MMS1 FPI/DIS partial ion perpendicular temperature during this burst [mms1_dis_tempperp_part_brst]

MMS1 FPI/DIS recommended energy index during this burst [mms1_dis_part_index_brst]

Recommended energy index during this burst

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MMS1_FPI_FAST_L2_DES-DIST (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DES/Fast/Level2/Distribution/PT4.5S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data taken at burst (30/150 ms for DES/DIS)
resolution are aggregated on board and made available at survey (4.5 s)
resolution in this mode.  This product contains phase-space distribution maps of
results from surveying the high-resolution observations during each 4.5 s
period.  In particular, the (highest possible quality at the time of release)
corrected/converted "Fast Survey SkyMap" distributions are reported with
time-stamps and other annotation characterizing the state of the instrument
system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DES fast sky-map instrument distribution - 11.6 eV (E1) using averaged even/odd steps [mms1_des_dist_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 11.6 eV [mms1_des_dist_fast1_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES fast sky-map instrument distribution - 40.4 eV (E6) using averaged even/odd steps [mms1_des_dist_fast6]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 40.4 eV [mms1_des_dist_fast6_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES fast sky-map instrument distribution - 85.1 eV (E9) using averaged even/odd steps [mms1_des_dist_fast9]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 85.1 eV [mms1_des_dist_fast9_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES fast sky-map instrument distribution - 179 eV (E12) using averaged even/odd steps [mms1_des_dist_fast12]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 179 eV [mms1_des_dist_fast12_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES fast sky-map instrument distribution - 295 eV (E14) using averaged even/odd steps [mms1_des_dist_fast14]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 295 eV [mms1_des_dist_fast14_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES fast sky-map instrument distribution - 485 eV (E16) using averaged even/odd steps [mms1_des_dist_fast16]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 485 eV [mms1_des_dist_fast16_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES fast sky-map instrument distribution - 798 eV (E18) using averaged even/odd steps [mms1_des_dist_fast18]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 798 eV [mms1_des_dist_fast18_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES fast sky-map instrument distribution - 1310 eV (E20) using averaged even/odd steps [mms1_des_dist_fast20]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1310 eV [mms1_des_dist_fast20_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES fast sky-map instrument distribution - 2770 eV (E23) using averaged even/odd steps [mms1_des_dist_fast23]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2770 eV [mms1_des_dist_fast23_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES fast sky-map instrument distribution - 5840 eV (E26) using averaged even/odd steps [mms1_des_dist_fast26]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5840 eV [mms1_des_dist_fast26_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES fast sky-map instrument distribution - 26000 eV (E32) using averaged even/odd steps [mms1_des_dist_fast32]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 26000 eV [mms1_des_dist_fast32_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[Only List/Create in CDAWeb] MMS1 FPI/DES fast sky-map instrument distribution 1-sigma error [mms1_des_disterr_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES vector of data-quality indicators at fast survey-start time - 32-bit error flags [mms1_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS1 FPI/DES compression lossless/lossy indicator at survey-start time [mms1_des_compressionloss_fast]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

---> MMS1 FPI/DES Del-Phi (obs spin-phase) count at fast survey-start time [mms1_des_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS1 FPI/DES Del-Phi (obs spin-phase) angle at fast survey-start time [mms1_des_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS1 FPI/DES fast survey average f1 count values [mms1_des_avgf1counts_fast]

Average f1-count level as a function of energy

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MMS1_FPI_FAST_L2_DES-MOMS (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DES/Fast/Level2/Moments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution.  Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This moments product
contains results from integrating the standard moments of phase-space
distributions formed from the indicated data type (DES/DIS burst, FS or SS). For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotation characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS1_FPI_FAST_L2_DES-MOMSAUX

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DES vector of data-quality indicators at survey-start time [mms1_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS1 FPI/DES partial electron number density during this survey [mms1_des_numberdensity_part_fast]

MMS1 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms1_des_bulkv_part_dbcs_fast]

MMS1 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms1_des_bulkv_part_gse_fast]

MMS1 FPI/DES partial electron pressure tensor in DBCS during this survey [mms1_des_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES partial electron pressure tensor in GSE during this survey [mms1_des_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES partial electron temperature tensor in DBCS during this survey [mms1_des_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES partial electron temperature tensor in GSE during this survey [mms1_des_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES partial electron parallel temperature during this survey [mms1_des_temppara_part_fast]

MMS1 FPI/DES partial electron perpendicular temperature during this survey [mms1_des_tempperp_part_fast]

MMS1 FPI/DES recommended energy index for partial moments during this survey [mms1_des_part_index_fast]

Recommended energy index during this survey

MMS1 FPI/DES compression lossless/lossy indicator at survey-start time [mms1_des_compressionloss_fast]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS1 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms1_des_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS1 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms1_des_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS1 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms1_des_pitchangdist_lowen_fast]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size: 6
deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS1 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms1_des_pitchangdist_miden_fast]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS1 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms1_des_pitchangdist_highen_fast]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS1 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms1_des_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS1 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms1_des_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS1 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms1_des_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS1 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms1_des_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS1 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms1_des_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS1 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms1_des_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS1 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms1_des_energyspectr_par_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS1 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms1_des_energyspectr_anti_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS1 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms1_des_energyspectr_perp_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS1 FPI/DES omni-directional electron energy spectrum during this survey [mms1_des_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS1 FPI/DES electron number density during this survey [mms1_des_numberdensity_fast]

MMS1 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms1_des_densityextrapolation_low_fast]

MMS1 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms1_des_densityextrapolation_high_fast]

MMS1 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms1_des_bulkv_dbcs_fast]

MMS1 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this survey [mms1_des_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS1 FPI/DES electron bulk-velocity vector in GSE during this survey [mms1_des_bulkv_gse_fast]

MMS1 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this survey [mms1_des_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS1 FPI/DES electron pressure tensor in DBCS during this survey [mms1_des_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES electron pressure tensor in GSE during this survey [mms1_des_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES electron temperature tensor in DBCS during this survey [mms1_des_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES electron temperature tensor in GSE during this survey [mms1_des_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES electron heat-flux vector in DBCS during this survey [mms1_des_heatq_dbcs_fast]

MMS1 FPI/DES electron heat-flux vector in GSE during this survey [mms1_des_heatq_gse_fast]

MMS1 FPI/DES electron parallel temperature during this BP [mms1_des_temppara_fast]

MMS1 FPI/DES electron perpendicular temperature during this BP [mms1_des_tempperp_fast]

MMS1 FPI/DES S/C potential mean [mms1_des_scpot_mean_fast]

Average spacecraft potential during this FP used to shift the measure energies.

MMS1 FPI/DES S/C potential max [mms1_des_scpot_max_fast]

Maximum spacecraft potential during this FP used to exclude energies containing
spacecraft photoelectron fluxes.

MMS1 FPI/DES Mag data X,Y,Z,Norm DSC components [nT] at survey-start time [mms1_des_fpibentpipe_dsc_fast]

X, Y, Z are unit vector components.

Magnetic field vector X,Y,Z, and magnitude B [mms1_des_fpib_gse_srvy_fast]

Averaged survey magnetic field data during this FP

Magnetic field vector X,Y,Z, and magnitude B [mms1_des_fpib_dmpa_srvy_fast]

Averaged survey magnetic field data during this FP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms1_des_pos_gse_fast]

Position in GSM coordinates, 30 second [mms1_des_pos_gsm_fast]

MMS1 number density integrands [mms1_des_numberdensity_int_fast]

Integrand terms used in normalized energy integration for number density

number flux [mms1_des_numberflux_int_dbcs_fast]

Integrand terms used in normalized energy integration for number flux

MMS1 pressure tensor integrands [mms1_des_prestensor_int_dbcs_fast]

Integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms1_des_ugrid_int_fast]

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MMS1_FPI_FAST_L2_DES-PARTMOMS (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DES/Fast/Level2/PartialMoments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DES vector of data-quality indicators at survey-start time [mms1_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS1 FPI/DES partial electron number density during this survey [mms1_des_numberdensity_part_fast]

MMS1 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms1_des_bulkv_part_dbcs_fast]

MMS1 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms1_des_bulkv_part_gse_fast]

MMS1 FPI/DES partial electron pressure tensor in DBCS during this survey [mms1_des_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES partial electron pressure tensor in GSE during this survey [mms1_des_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES partial electron temperature tensor in DBCS during this survey [mms1_des_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES partial electron temperature tensor in GSE during this survey [mms1_des_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES partial electron parallel temperature during this survey [mms1_des_temppara_part_fast]

MMS1 FPI/DES partial electron perpendicular temperature during this survey [mms1_des_tempperp_part_fast]

MMS1 FPI/DES recommended energy index during this survey [mms1_des_part_index_fast]

Recommended energy index during this survey

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MMS1_FPI_FAST_L2_DIS-DIST (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DIS/Fast/Level2/Distribution/PT4.5S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data taken at burst (30/150 ms for DES/DIS)
resolution are aggregated on board and made available at survey (4.5 s)
resolution in this mode.  This product contains phase-space distribution maps of
results from surveying the high-resolution observations during each 4.5 s
period.  In particular, the (highest possible quality at the time of release)
corrected/converted "Fast Survey SkyMap" distributions are reported with
time-stamps and other annotation characterizing the state of the instrument
system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DIS fast sky-map instrument distribution - 11.3 eV (E1) using averaged even/odd steps [mms1_dis_dist_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 11.3 eV [mms1_dis_dist_fast1_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS fast sky-map instrument distribution - 39.6 eV (E6) using averaged even/odd steps [mms1_dis_dist_fast6]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 39.6 eV [mms1_dis_dist_fast6_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS fast sky-map instrument distribution - 83.9 eV (E9 using averaged even/odd steps) [mms1_dis_dist_fast9]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 83.9 eV [mms1_dis_dist_fast9_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS fast sky-map instrument distribution - 178 eV (E12) using averaged even/odd steps [mms1_dis_dist_fast12]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 178 eV [mms1_dis_dist_fast12_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS fast sky-map instrument distribution - 293 eV (E14) using averaged even/odd steps [mms1_dis_dist_fast14]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 293 eV [mms1_dis_dist_fast14_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS fast sky-map instrument distribution - 484 eV (E16) using averaged even/odd steps [mms1_dis_dist_fast16]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 484 eV [mms1_dis_dist_fast16_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS fast sky-map instrument distribution - 799 eV (E18) using averaged even/odd steps [mms1_dis_dist_fast18]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 799 eV [mms1_dis_dist_fast18_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS fast sky-map instrument distribution - 1320 eV (E20) using averaged even/odd steps [mms1_dis_dist_fast20]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1320 eV [mms1_dis_dist_fast20_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS fast sky-map instrument distribution - 2800 eV (E23) using averaged even/odd steps [mms1_dis_dist_fast23]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2800 eV [mms1_dis_dist_fast23_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS fast sky-map instrument distribution - 5920 eV (E26) using averaged even/odd steps [mms1_dis_dist_fast26]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5920 eV [mms1_dis_dist_fast26_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS fast sky-map instrument distribution - 26600 eV (E32) using averaged even/odd steps [mms1_dis_dist_fast32]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 26600 eV [mms1_dis_dist_fast32_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[Only List/Create in CDAWeb] MMS1 FPI/DIS fast sky-map instrument distribution 1-sigma error [mms1_dis_disterr_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS vector of data-quality indicators at fast survey-start time - 32-bit error flags [mms1_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS1 FPI/DIS compression lossless/lossy indicator at survey-start time [mms1_dis_compressionloss_fast]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) count at fast survey-start time [mms1_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at fast survey-start time [mms1_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS1 FPI/DIS fast survey average f1 count values [mms1_dis_avgf1counts_fast]

Average f1-count level as a function of energy

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MMS1_FPI_FAST_L2_DIS-MOMS (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DIS/Fast/Level2/Moments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution.  Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This moments product
contains results from integrating the standard moments of phase-space
distributions formed from the indicated data type (DES/DIS burst, FS or SS). For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotation characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DIS vector of data-quality indicators at survey-start time [mms1_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation, Bit-14 =
high MMS3 spintone due to DIS008 anomaly

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms1_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

---> MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms1_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS1 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms1_dis_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

---> MMS1 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms1_dis_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

---> MMS1 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms1_dis_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

---> MMS1 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms1_dis_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

---> MMS1 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms1_dis_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

---> MMS1 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms1_dis_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS1 FPI/DIS omni-directional ion energy spectrum during this survey [mms1_dis_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS1 FPI/DIS ion background energy during this survey [mms1_dis_spectr_bg_fast]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS1 FPI/DIS ion background number density during this survey [mms1_dis_numberdensity_bg_fast]

Background number density derived via integration of the estimated background
differential energy flux.

MMS1 FPI/DIS ion number density during this survey [mms1_dis_numberdensity_fast]

---> (no error bars displayed) MMS1 FPI/DIS ion number density during this survey [mms1_dis_numberdensity_fast_noerr]

MMS1 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms1_dis_densityextrapolation_low_fast]

MMS1 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms1_dis_densityextrapolation_high_fast]

MMS1 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms1_dis_bulkv_dbcs_fast]

---> (no error bars displayed) MMS1 FPI/DIS ion bulk-velocity DBCS vector during this survey [mms1_dis_bulkv_dbcs_fast_noerr]

MMS1 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey [mms1_dis_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS1 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms1_dis_bulkv_gse_fast]

MMS1 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey [mms1_dis_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

---> (no error bars displayed) MMS1 FPI/DIS ion bulk-velocity GSE vector during this survey [mms1_dis_bulkv_gse_fast_noerr]

MMS1 FPI/DIS ion pressure tensor in DBCS during this survey [mms1_dis_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS ion pressure tensor in GSE during this survey [mms1_dis_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS ion background pressure during this survey [mms1_dis_pres_bg_fast]

MMS1 FPI/DIS ion temperature tensor in DBCS during this survey [mms1_dis_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS ion temperature tensor in GSE during this survey [mms1_dis_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS ion heat-flux vector in DBCS during this survey [mms1_dis_heatq_dbcs_fast]

MMS1 FPI/DIS ion heat-flux vector in GSE during this survey [mms1_dis_heatq_gse_fast]

MMS1 FPI/DIS ion parallel temperature during this BP [mms1_dis_temppara_fast]

MMS1 FPI/DIS ion perpendicular temperature during this BP [mms1_dis_tempperp_fast]

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MMS1_FPI_FAST_L2_DIS-MOMSAUX

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DIS vector of data-quality indicators at survey-start time [mms1_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS1 FPI/DIS partial ion number density during this survey [mms1_dis_numberdensity_part_fast]

MMS1 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms1_dis_bulkv_part_dbcs_fast]

MMS1 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms1_dis_bulkv_part_gse_fast]

MMS1 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms1_dis_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS partial ion pressure tensor in GSE during this survey [mms1_dis_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms1_dis_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS partial ion temperature tensor in GSE during this survey [mms1_dis_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS partial ion parallel temperature during this survey [mms1_dis_temppara_part_fast]

MMS1 FPI/DIS partial ion perpendicular temperature during this survey [mms1_dis_tempperp_part_fast]

MMS1 FPI/DIS recommended energy index for partial moments during this survey [mms1_dis_part_index_fast]

Recommended energy index during this survey

MMS1 FPI/DIS compression lossless/lossy indicator at survey-start time [mms1_dis_compressionloss_fast]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS1 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms1_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms1_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS1 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms1_dis_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS1 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms1_dis_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS1 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms1_dis_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS1 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms1_dis_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS1 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms1_dis_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS1 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms1_dis_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS1 FPI/DIS omni-directional ion energy spectrum during this survey [mms1_dis_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS1 FPI/DIS ion background energy during this survey [mms1_dis_spectr_bg_fast]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS1 FPI/DIS ion background number density during this survey [mms1_dis_numberdensity_bg_fast]

Background number density derived via integration of the estimated background
differential energy flux.

MMS1 FPI/DIS ion number density during this survey [mms1_dis_numberdensity_fast]

MMS1 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms1_dis_densityextrapolation_low_fast]

MMS1 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms1_dis_densityextrapolation_high_fast]

MMS1 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms1_dis_bulkv_dbcs_fast]

MMS1 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey [mms1_dis_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS1 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms1_dis_bulkv_gse_fast]

MMS1 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey [mms1_dis_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS1 FPI/DIS ion pressure tensor in DBCS during this survey [mms1_dis_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS ion pressure tensor in GSE during this survey [mms1_dis_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS ion background pressure during this survey [mms1_dis_pres_bg_fast]

MMS1 FPI/DIS ion temperature tensor in DBCS during this survey [mms1_dis_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS ion temperature tensor in GSE during this survey [mms1_dis_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS ion heat-flux vector in DBCS during this survey [mms1_dis_heatq_dbcs_fast]

MMS1 FPI/DIS ion heat-flux vector in GSE during this survey [mms1_dis_heatq_gse_fast]

MMS1 FPI/DIS ion parallel temperature during this BP [mms1_dis_temppara_fast]

MMS1 FPI/DIS ion perpendicular temperature during this BP [mms1_dis_tempperp_fast]

MMS1 FPI/DIS S/C potential mean [mms1_dis_scpot_mean_fast]

Average spacecraft potential during this FP used to shift the measure energies.

MMS1 FPI/DIS S/C potential max [mms1_dis_scpot_max_fast]

Maximum spacecraft potential during this FP used to exclude energies containing
spacecraft photoelectron fluxes.

MMS1 FPI/DIS Mag data X,Y,Z,Norm DSC components [nT] at survey-start time [mms1_dis_fpibentpipe_dsc_fast]

X, Y, Z are unit vector components.

Magnetic field vector X,Y,Z, and magnitude B [mms1_dis_fpib_gse_srvy_fast]

Averaged survey magnetic field data during this FP

Magnetic field vector X,Y,Z, and magnitude B [mms1_dis_fpib_dmpa_srvy_fast]

Averaged survey magnetic field data during this FP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms1_dis_pos_gse_fast]

Position in GSM coordinates, 30 second [mms1_dis_pos_gsm_fast]

MMS1 number density integrands [mms1_dis_numberdensity_int_fast]

integrand terms used in normalized energy integration for number density

number flux [mms1_dis_numberflux_int_dbcs_fast]

integrand terms used in normalized energy integration for number flux

MMS1 pressure tensor integrands [mms1_dis_prestensor_int_dbcs_fast]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms1_dis_ugrid_int_fast]

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MMS1_FPI_FAST_L2_DIS-PARTMOMS (spase://NASA/NumericalData/MMS/1/FastPlasmaInvestigation/DIS/Fast/Level2/PartialMoments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DIS vector of data-quality indicators at survey-start time [mms1_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS1 FPI/DIS partial ion number density during this survey [mms1_dis_numberdensity_part_fast]

MMS1 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms1_dis_bulkv_part_dbcs_fast]

MMS1 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms1_dis_bulkv_part_gse_fast]

MMS1 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms1_dis_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS partial ion pressure tensor in GSE during this survey [mms1_dis_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms1_dis_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS partial ion temperature tensor in GSE during this survey [mms1_dis_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS partial ion parallel temperature during this survey [mms1_dis_temppara_part_fast]

MMS1 FPI/DIS partial ion perpendicular temperature during this survey [mms1_dis_tempperp_part_fast]

MMS1 FPI/DIS recommended energy index during this survey [mms1_dis_part_index_fast]

Recommended energy index during this survey

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MMS1_FPI_SLOW_L2_DES-DIST

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode.  This product contains phase-space distribution maps of those
survey-resolution data from Slow Mode.  In particular, the (highest possible
quality at the time of release) corrected/converted "Slow Survey SkyMap"
distributions are reported with time-stamps and other annotation characterizing
the state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DES vector of data-quality indicators at survey-start time [mms1_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = compression pipeline error

MMS1 FPI/DES compression lossless/lossy indicator at survey-start time [mms1_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS1 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms1_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS1 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms1_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS1 FPI/DES Slow Survey sky-map instrument distribution [mms1_des_dist_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES Slow Survey sky-map instrument distribution 1-sigma error [mms1_des_disterr_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DES slow survey average f1 count values [mms1_des_avgf1counts_slow]

Average f1-count level as a function of energy

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MMS1_FPI_SLOW_L2_DES-MOMS

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DES vector of data-quality indicators at survey-start time [mms1_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only)

MMS1 FPI/DES compression lossless/lossy indicator at survey-start time [mms1_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS1 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms1_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS1 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms1_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS1 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms1_des_pitchangdist_lowen_slow]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS1 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms1_des_pitchangdist_miden_slow]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS1 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms1_des_pitchangdist_highen_slow]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS1 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms1_des_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS1 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms1_des_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS1 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms1_des_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS1 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms1_des_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS1 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms1_des_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS1 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms1_des_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS1 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms1_des_energyspectr_par_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS1 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms1_des_energyspectr_anti_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS1 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms1_des_energyspectr_perp_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS1 FPI/DES omni-directional electron energy spectrum during this survey [mms1_des_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS1 FPI/DES electron number density during this survey [mms1_des_numberdensity_slow]

MMS1 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms1_des_densityextrapolation_low_slow]

MMS1 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms1_des_densityextrapolation_high_slow]

MMS1 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms1_des_bulkv_dbcs_slow]

MMS1 FPI/DES electron bulk-velocity vector in GSE during this survey [mms1_des_bulkv_gse_slow]

MMS1 FPI/DES electron pressure tensor in DBCS during this survey [mms1_des_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES electron pressure tensor in GSE during this survey [mms1_des_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES electron temperature tensor in DBCS during this survey [mms1_des_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES electron temperature tensor in GSE during this survey [mms1_des_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES electron heat-flux vector in DBCS during this survey [mms1_des_heatq_dbcs_slow]

MMS1 FPI/DES electron heat-flux vector in GSE during this survey [mms1_des_heatq_gse_slow]

MMS1 FPI/DES electron parallel temperature during this BP [mms1_des_temppara_slow]

MMS1 FPI/DES electron perpendicular temperature during this BP [mms1_des_tempperp_slow]

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MMS1_FPI_SLOW_L2_DES-MOMSAUX

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DES vector of data-quality indicators at survey-start time [mms1_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only)

MMS1 FPI/DES partial electron number density during this survey [mms1_des_numberdensity_part_slow]

MMS1 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms1_des_bulkv_part_dbcs_slow]

MMS1 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms1_des_bulkv_part_gse_slow]

MMS1 FPI/DES partial electron pressure tensor in DBCS during this survey [mms1_des_prestensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES partial electron pressure tensor in GSE during this survey [mms1_des_prestensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES partial electron temperature tensor in DBCS during this survey [mms1_des_temptensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES partial electron temperature tensor in GSE during this survey [mms1_des_temptensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES partial electron parallel temperature during this survey [mms1_des_temppara_part_slow]

MMS1 FPI/DES partial electron perpendicular temperature during this survey [mms1_des_tempperp_part_slow]

MMS1 FPI/DES recommended energy index for partial moments during this survey [mms1_des_part_index_slow]

Recommended energy index during this survey

MMS1 FPI/DES compression lossless/lossy indicator at survey-start time [mms1_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS1 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms1_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS1 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms1_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS1 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms1_des_pitchangdist_lowen_slow]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS1 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms1_des_pitchangdist_miden_slow]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS1 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms1_des_pitchangdist_highen_slow]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS1 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms1_des_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS1 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms1_des_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS1 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms1_des_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS1 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms1_des_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS1 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms1_des_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS1 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms1_des_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS1 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms1_des_energyspectr_par_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS1 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms1_des_energyspectr_anti_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS1 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms1_des_energyspectr_perp_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS1 FPI/DES omni-directional electron energy spectrum during this survey [mms1_des_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS1 FPI/DES electron number density during this survey [mms1_des_numberdensity_slow]

MMS1 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms1_des_densityextrapolation_low_slow]

MMS1 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms1_des_densityextrapolation_high_slow]

MMS1 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms1_des_bulkv_dbcs_slow]

MMS1 FPI/DES electron bulk-velocity vector in GSE during this survey [mms1_des_bulkv_gse_slow]

MMS1 FPI/DES electron pressure tensor in DBCS during this survey [mms1_des_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES electron pressure tensor in GSE during this survey [mms1_des_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DES electron temperature tensor in DBCS during this survey [mms1_des_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES electron temperature tensor in GSE during this survey [mms1_des_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DES electron heat-flux vector in DBCS during this survey [mms1_des_heatq_dbcs_slow]

MMS1 FPI/DES electron heat-flux vector in GSE during this survey [mms1_des_heatq_gse_slow]

MMS1 FPI/DES electron parallel temperature during this BP [mms1_des_temppara_slow]

MMS1 FPI/DES electron perpendicular temperature during this BP [mms1_des_tempperp_slow]

MMS1 FPI/DES S/C potential mean [mms1_des_scpot_mean_slow]

Average spacecraft potential during this SP used to shift the measure energies.

MMS1 FPI/DES S/C potential max [mms1_des_scpot_max_slow]

Maximum spacecraft potential during this SP used to exclude energies containing
spacecraft photoelectron fluxes.

Magnetic field vector X,Y,Z, and magnitude B [mms1_des_fpib_gse_srvy_slow]

Averaged survey magnetic field data during this SP

Magnetic field vector X,Y,Z, and magnitude B [mms1_des_fpib_dmpa_srvy_slow]

Averaged survey magnetic field data during this SP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms1_des_pos_gse_slow]

Position in GSM coordinates, 30 second [mms1_des_pos_gsm_slow]

MMS1 number density integrands [mms1_des_numberdensity_int_slow]

integrand terms used in normalized energy integration for number density

number flux [mms1_des_numberflux_int_dbcs_slow]

integrand terms used in normalized energy integration for number flux

MMS1 pressure tensor integrands [mms1_des_prestensor_int_dbcs_slow]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms1_des_ugrid_int_slow]

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MMS1_FPI_SLOW_L2_DIS-DIST

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode.  This product contains phase-space distribution maps of those
survey-resolution data from Slow Mode.  In particular, the (highest possible
quality at the time of release) corrected/converted "Slow Survey SkyMap"
distributions are reported with time-stamps and other annotation characterizing
the state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DIS vector of data-quality indicators at survey-start time [mms1_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = compression pipeline error

MMS1 FPI/DIS compression lossless/lossy indicator at survey-start time [mms1_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS1 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms1_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms1_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS1 FPI/DIS Slow Survey sky-map instrument distribution [mms1_dis_dist_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS Slow Survey sky-map instrument distribution 1-sigma error [mms1_dis_disterr_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS1 FPI/DIS slow survey average f1 count values [mms1_dis_avgf1counts_slow]

Average f1-count level as a function of energy

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MMS1_FPI_SLOW_L2_DIS-MOMS

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DIS vector of data-quality indicators at survey-start time [mms1_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only), Bit-13 =
significant (>=20%) penetrating radiation, Bit-14 = high MMS3 spintone due to
DIS008 anomaly

MMS1 FPI/DIS compression lossless/lossy indicator at survey-start time [mms1_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS1 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms1_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms1_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS1 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms1_dis_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS1 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms1_dis_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS1 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms1_dis_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS1 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms1_dis_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS1 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms1_dis_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS1 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms1_dis_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS1 FPI/DIS omni-directional ion energy spectrum during this survey [mms1_dis_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS1 FPI/DIS ion background energy during this survey [mms1_dis_spectr_bg_slow]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS1 FPI/DIS ion background number density during this survey [mms1_dis_numberdensity_bg_slow]

Background number density derived via integration of the estimated background
differential energy flux.

MMS1 FPI/DIS ion number density during this survey [mms1_dis_numberdensity_slow]

MMS1 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms1_dis_densityextrapolation_low_slow]

MMS1 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms1_dis_densityextrapolation_high_slow]

MMS1 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms1_dis_bulkv_dbcs_slow]

MMS1 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms1_dis_bulkv_gse_slow]

MMS1 FPI/DIS ion pressure tensor in DBCS during this survey [mms1_dis_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS ion pressure tensor in GSE during this survey [mms1_dis_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS ion background pressure during this survey [mms1_dis_pres_bg_slow]

MMS1 FPI/DIS ion temperature tensor in DBCS during this survey [mms1_dis_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS ion temperature tensor in GSE during this survey [mms1_dis_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS ion heat-flux vector in DBCS during this survey [mms1_dis_heatq_dbcs_slow]

MMS1 FPI/DIS ion heat-flux vector in GSE during this survey [mms1_dis_heatq_gse_slow]

MMS1 FPI/DIS ion parallel temperature during this BP [mms1_dis_temppara_slow]

MMS1 FPI/DIS ion perpendicular temperature during this BP [mms1_dis_tempperp_slow]

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MMS1_FPI_SLOW_L2_DIS-MOMSAUX

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS1 FPI/DIS vector of data-quality indicators at survey-start time [mms1_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only), Bit-13 =
significant (>=20%) penetrating radiation, Bit-14 = high MMS3 spintone due to
DIS008 anomaly

MMS1 FPI/DIS partial ion number density during this survey [mms1_dis_numberdensity_part_slow]

MMS1 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms1_dis_bulkv_part_dbcs_slow]

MMS1 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms1_dis_bulkv_part_gse_slow]

MMS1 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms1_dis_prestensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS partial ion pressure tensor in GSE during this survey [mms1_dis_prestensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms1_dis_temptensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS partial ion temperature tensor in GSE during this survey [mms1_dis_temptensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS partial ion parallel temperature during this survey [mms1_dis_temppara_part_slow]

MMS1 FPI/DIS partial ion perpendicular temperature during this survey [mms1_dis_tempperp_part_slow]

MMS1 FPI/DIS recommended energy index for partial moments during this survey [mms1_dis_part_index_slow]

Recommended energy index during this survey

MMS1 FPI/DIS compression lossless/lossy indicator at survey-start time [mms1_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS1 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms1_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS1 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms1_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS1 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms1_dis_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS1 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms1_dis_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS1 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms1_dis_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS1 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms1_dis_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS1 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms1_dis_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS1 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms1_dis_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS1 FPI/DIS omni-directional ion energy spectrum during this survey [mms1_dis_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS1 FPI/DIS ion background energy during this survey [mms1_dis_spectr_bg_slow]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS1 FPI/DIS ion background number density during this survey [mms1_dis_numberdensity_bg_slow]

Background number density derived via integration of the estimated background
differential energy flux.

MMS1 FPI/DIS ion number density during this survey [mms1_dis_numberdensity_slow]

MMS1 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms1_dis_densityextrapolation_low_slow]

MMS1 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms1_dis_densityextrapolation_high_slow]

MMS1 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms1_dis_bulkv_dbcs_slow]

MMS1 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms1_dis_bulkv_gse_slow]

MMS1 FPI/DIS ion pressure tensor in DBCS during this survey [mms1_dis_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS ion pressure tensor in GSE during this survey [mms1_dis_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS1 FPI/DIS ion background pressure during this survey [mms1_dis_pres_bg_slow]

MMS1 FPI/DIS ion temperature tensor in DBCS during this survey [mms1_dis_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS ion temperature tensor in GSE during this survey [mms1_dis_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS1 FPI/DIS ion heat-flux vector in DBCS during this survey [mms1_dis_heatq_dbcs_slow]

MMS1 FPI/DIS ion heat-flux vector in GSE during this survey [mms1_dis_heatq_gse_slow]

MMS1 FPI/DIS ion parallel temperature during this BP [mms1_dis_temppara_slow]

MMS1 FPI/DIS ion perpendicular temperature during this BP [mms1_dis_tempperp_slow]

MMS1 FPI/DIS S/C potential mean [mms1_dis_scpot_mean_slow]

Average spacecraft potential during this SP used to shift the measure energies.

MMS1 FPI/DIS S/C potential max [mms1_dis_scpot_max_slow]

Maximum spacecraft potential during this SP used to exclude energies containing
spacecraft photoelectron fluxes.

Magnetic field vector X,Y,Z, and magnitude B [mms1_dis_fpib_gse_srvy_slow]

Averaged survey magnetic field data during this SP

Magnetic field vector X,Y,Z, and magnitude B [mms1_dis_fpib_dmpa_srvy_slow]

Averaged survey magnetic field data during this SP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms1_dis_pos_gse_slow]

Position in GSM coordinates, 30 second [mms1_dis_pos_gsm_slow]

MMS1 number density integrands [mms1_dis_numberdensity_int_slow]

integrand terms used in normalized energy integration for number density

number flux [mms1_dis_numberflux_int_dbcs_slow]

integrand terms used in normalized energy integration for number flux

MMS1 pressure tensor integrands [mms1_dis_prestensor_int_dbcs_slow]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms1_dis_ugrid_int_slow]

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MMS1_HPCA_BRST_L2_ION (spase://NASA/NumericalData/MMS/1/HotPlasmaCompositionAnalyzer/Burst/Level2/Ion/PT0.625S)

Description

References

Modification History

Initial Public Release

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MMS1_HPCA_BRST_L2_MOMENTS (spase://NASA/NumericalData/MMS/1/HotPlasmaCompositionAnalyzer/Burst/Level2/Moments/PT10S)

Description

References

Modification History

Initial Public Release

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MMS1_HPCA_SRVY_L2_ION (spase://NASA/NumericalData/MMS/1/HotPlasmaCompositionAnalyzer/Survey/Level2/Ion/PT0.625S)

Description

References

Modification History

Initial Public Release

Data Variable Descriptions

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MMS1_HPCA_SRVY_L2_MOMENTS (spase://NASA/NumericalData/MMS/1/HotPlasmaCompositionAnalyzer/Survey/Level2/Moments/PT10S)

Description

References

Modification History

Initial Public Release

Data Variable Descriptions

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MMS1_HPCA_SRVY_L2_TOF-COUNTS (spase://NASA/NumericalData/MMS/1/HotPlasmaCompositionAnalyzer/Survey/Level2/TimeOfFlight/Counts/PT0.625S)

Description

References

Modification History

Initial Public Release

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MMS1_MEC_BRST_L2_EPHT89D (spase://NASA/NumericalData/MMS/1/Ephemeris/Burst/Level2/Tsyganenko_89_Dynamic/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS1_MEC_BRST_L2_EPHT89Q (spase://NASA/NumericalData/MMS/1/Ephemeris/Burst/Level2/Tsyganenko_89_Quiet/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS1_MEC_BRST_L2_EPHTS04D (spase://NASA/NumericalData/MMS/1/Ephemeris/Burst/Level2/Tsyganenko_04_Dynamic/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS1_MEC_SRVY_L2_EPHT89D (spase://NASA/NumericalData/MMS/1/Ephemeris/Survey/Level2/Tsyganenko_89_Dynamic/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS1_MEC_SRVY_L2_EPHT89Q (spase://NASA/NumericalData/MMS/1/Ephemeris/Survey/Level2/Tsyganenko_89_Quiet/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS1_MEC_SRVY_L2_EPHTS04D (spase://NASA/NumericalData/MMS/1/Ephemeris/Survey/Level2/Tsyganenko_04_Dynamic/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS1_R0_SUMMARY

Description

Pre-generated MMS Quicklook Summary Plots
File location: https://cdaweb.gsfc.nasa.gov/pub/data/mms/ql_plots/al1_mms4_summ

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MMS1_SCM_BRST_L2_SCB (spase://NASA/NumericalData/MMS/1/FIELDS/SCM/Burst/Level2/PT0.0001220703125S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
https://urldefense.proofpoint.com/v2/url?u=http-3A__link.springer.com_article_10
.1007_s11214-2D014-2D0096-2D9&d=DwIFAg&c=c6MrceVCY5m5A_KAUkrdoA&r=bjziExGTRYoZgE
2xb_dDSm9NxNIo0lG6Q-rB0Y6rHS4&m=CMzo0Vv9zPtWSdbdY1Wq9-jIkYS2cOMV9JYZsMV10y0&s=Xb
P9PiEAswHGl5lqgsDVI6zs8ivJx7yek9i2undKl10&e=

Modification History

unpack telemetry, assign sample times
2026-07-10T20:12:20.00006318092028Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-16T12:36:26.00005209445941Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-16T12:36:32.00005978345859Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms1_scm_acb_gse_scb_brst_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 8192S/s.
They are high-pass filtered above 1.00Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide.

(List/Create Only) Quality Factor (one letter per antenna, G=good) [mms1_scm_qf_scm123_scb_brst_l2]

Each letter refers to one SCM physical antenna in the SCM123 order. 'G' stands
for good data, 'Z' for data that are affected or set to zero by convolution
boundary effect, 'S' for saturated data, 'X' for out of range data, 'B' for
fillvalue/bad data.

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MMS1_SCM_BRST_L2_SCHB (spase://NASA/NumericalData/MMS/1/FIELDS/SCM/Burst/Level2/PT0.00006101515625S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
http://link.springer.com/article/10.1007/s11214-014-0096-9

Modification History

unpack telemetry, assign sample times
2026-07-10T20:12:49.0000668168036Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-16T12:41:02.00004369020467Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-16T12:41:07.00005680322652Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms1_scm_acb_gse_schb_brst_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 16384S/s.
They are high-pass filtered above 32.00Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide
(https://lasp.colorado.edu/mms/sdc/public/datasets/fields/Science_Data_Products_ 
Guide_vol2_SCM_v11_20160301.pdf).

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MMS1_SCM_SRVY_L2_SCSRVY (spase://NASA/NumericalData/MMS/1/FIELDS/SCM/Survey/Level2/PT0.03125S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
https://urldefense.proofpoint.com/v2/url?u=http-3A__link.springer.com_article_10
.1007_s11214-2D014-2D0096-2D9&d=DwIFAg&c=c6MrceVCY5m5A_KAUkrdoA&r=bjziExGTRYoZgE
2xb_dDSm9NxNIo0lG6Q-rB0Y6rHS4&m=CMzo0Vv9zPtWSdbdY1Wq9-jIkYS2cOMV9JYZsMV10y0&s=Xb
P9PiEAswHGl5lqgsDVI6zs8ivJx7yek9i2undKl10&e=

Modification History

unpack telemetry, assign sample times
2026-07-02T23:55:03.00004184245717Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-15T23:54:12.00003683566739Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-15T23:54:59.00006353854825Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms1_scm_acb_gse_scsrvy_srvy_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 32S/s. They
are high-pass filtered above 0.50Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide.

(List/Create Only) Quality Factor (one letter per antenna, G=good) [mms1_scm_qf_scm123_scsrvy_srvy_l2]

Each letter refers to one SCM physical antenna in the SCM123 order. 'G' stands
for good data, 'Z' for data that are affected or set to zero by convolution
boundary effect, 'S' for saturated data, 'X' for out of range data, 'B' for
fillvalue/bad data.

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MMS2_ASPOC_SRVY_L2 (spase://NASA/NumericalData/MMS/2/ASPOC/Survey/Level2/PT1S)

Description

K. Torkar et al, Active Spacecraft Potential Control Investigation
Space Science Reviews, 2014, DOI: 10.1007/s11214-014-0049-3
Further information:
- http://www.iwf.oeaw.ac.at/en/research/near-earth-space/mms/ 
- http://mms.space.swri.edu/

Modification History

150224 Initial version
150831 Minor updates and fixes
160205 CDF file format guide compliant

Data Variable Descriptions

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MMS2_DSP_FAST_L2_BPSD (spase://NASA/NumericalData/MMS/2/FIELDS/DSP/Fast/Level2/MagneticFieldPowerSpectralDensity/PT2S)

Description

BPSD is the low frequency B spectral density covering the frequency range of .2
to 6000 Hz.

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MMS2_DSP_FAST_L2_EPSD (spase://NASA/NumericalData/MMS/2/FIELDS/DSP/Fast/Level2/ElectricFieldPowerSpectralDensity/PT2S)

Description

EPSD combines the low frequency E spectral density covering the frequency range
of 1 to 8000 Hz and the  medium frequency E spectral density covering the
frequency range of .25 to 100 kHz.

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MMS2_DSP_SLOW_L2_BPSD (spase://NASA/NumericalData/MMS/2/FIELDS/DSP/Slow/Level2/MagneticFieldPowerSpectralDensity/PT16S)

Description

search coil magnetometer spectral density

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MMS2_DSP_SLOW_L2_EPSD (spase://NASA/NumericalData/MMS/2/FIELDS/DSP/Slow/Level2/ElectricFieldPowerSpectralDensity/PT16S)

Description

electric spectral density

Data Variable Descriptions

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MMS2_EDI_BRST_L2_AMB (spase://NASA/NumericalData/MMS/2/FIELDS/EDI/Burst/Level2/ElectronFluxAmbient/ProjectionMethod1/PT0.0009765625S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - Original version.
v1.0.0 - Include trajectory vectors and optics state.
v1.1.0 - Update metadata: counts -> flux.
v1.2.0 - Added flux error.
v1.3.0 - Trajectory vector errors are now deltas.
v1.4.0 - Fixed dead-time correction and error values.
v1.5.0 - Factor of 2 for accumulation time & 2 for abscal factor in srvy mode.
v1.6.0 - No factor of 2 for accumulation time in srvy mode.
v2.0.0 - Reduced file size with scalar errors. Update metadata.
v2.1.0 - Correct fill value for fluxes.
v3.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v4.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.

Data Variable Descriptions

Optics state [mms2_edi_optics_state_brst_l2]

---> GDU1 energy [mms2_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms2_edi_energy_gdu2_brst_l2]

Flux for electrons with trajectories given by Traj-1 0PA [mms2_edi_flux1_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-1 0PA [mms2_edi_flux1_0_brst_l2_noerr]

---> Error for flux1 0-degree pitch angle electron flux. [mms2_edi_flux1_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-2 0PA [mms2_edi_flux2_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-2 0PA [mms2_edi_flux2_0_brst_l2_noerr]

---> Error for flux2 0-degree pitch angle electron flux. [mms2_edi_flux2_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-3 0PA [mms2_edi_flux3_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-3 0PA [mms2_edi_flux3_0_brst_l2_noerr]

---> Error for flux3 0-degree pitch angle electron flux. [mms2_edi_flux3_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-4 0PA [mms2_edi_flux4_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-4 0PA [mms2_edi_flux4_0_brst_l2_noerr]

---> Error for flux4 0-degree pitch angle electron flux. [mms2_edi_flux4_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-1 180PA [mms2_edi_flux1_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-1 180PA [mms2_edi_flux1_180_brst_l2_noerr]

---> Error for flux1 180-degree pitch angle electron flux. [mms2_edi_flux1_180_delta_brst_l2]

Flux for electrons with trajectories given by traj2 180PA [mms2_edi_flux2_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-2 180PA [mms2_edi_flux2_180_brst_l2_noerr]

---> Error for flux2 180-degree pitch angle electron flux. [mms2_edi_flux2_180_delta_brst_l2]

Flux for electrons with trajectories given by traj3 180PA [mms2_edi_flux3_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-3 180PA [mms2_edi_flux3_180_brst_l2_noerr]

---> Error for flux3 180-degree pitch angle electron flux. [mms2_edi_flux3_180_delta_brst_l2]

Flux for electrons with trajectories given by traj4 180PA [mms2_edi_flux4_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-4 180PA [mms2_edi_flux4_180_brst_l2_noerr]

---> Error for flux4 180-degree pitch angle electron flux. [mms2_edi_flux4_180_delta_brst_l2]

Trajectory of flux1 0-degree pitch angle electrons in GSE coordinates. [mms2_edi_traj1_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 0-degree pitch angle electrons in GSE coordinates. [mms2_edi_traj2_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 0-degree pitch angle electrons in GSE coordinates. [mms2_edi_traj3_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 0-degree pitch angle electrons in GSE coordinates. [mms2_edi_traj4_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 180-degree pitch angle electrons in GSE coordinates. [mms2_edi_traj1_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 180-degree pitch angle electrons in GSE coordinates. [mms2_edi_traj2_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 180-degree pitch angle electrons in GSE coordinates. [mms2_edi_traj3_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 180-degree pitch angle electrons in GSE coordinates. [mms2_edi_traj4_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj1_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 0-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj2_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 0-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj3_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 0-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj4_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj1_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 180-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj2_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 180-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj3_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 180-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj4_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms2_edi_traj1_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms2_edi_traj2_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms2_edi_traj3_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms2_edi_traj4_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms2_edi_traj1_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms2_edi_traj2_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms2_edi_traj3_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms2_edi_traj4_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS2_EDI_BRST_L2_AMB-PM2 (spase://NASA/NumericalData/MMS/2/FIELDS/EDI/Burst/Level2/AmbientElectronFlux/ProjectionMethod2/PT0.0009765625S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v1.0.0 - Original version.
v1.1.0 - Correct fill value for fluxes.
v2.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v3.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.
v4.0.0 - Each trajectory has its own LABL_PTR_1 variable.

Data Variable Descriptions

Optics state [mms2_edi_optics_state_brst_l2]

---> GDU1 energy [mms2_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms2_edi_energy_gdu2_brst_l2]

Field-aligned electron flux from channel 1 of both GDUs [mms2_edi_flux1_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 1 of both GDUs [mms2_edi_flux1_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 1 of both GDUs. [mms2_edi_flux1_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 1 of both GDUs [mms2_edi_flux1_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 1 of both GDUs [mms2_edi_flux1_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 1 of both GDUs. [mms2_edi_flux1_180_delta_brst_l2]

Field-aligned electron flux from channel 2 of both GDUs [mms2_edi_flux2_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 2 of both GDUs [mms2_edi_flux2_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 2 of both GDUs. [mms2_edi_flux2_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 2 of both GDUs [mms2_edi_flux2_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 2 of both GDUs [mms2_edi_flux2_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 2 of both GDUs. [mms2_edi_flux2_180_delta_brst_l2]

Field-aligned electron flux from channel 3 of both GDUs [mms2_edi_flux3_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 3 of both GDUs [mms2_edi_flux3_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 3 of both GDUs. [mms2_edi_flux3_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 3 of both GDUs [mms2_edi_flux3_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 3 of both GDUs [mms2_edi_flux3_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 3 of both GDUs. [mms2_edi_flux3_180_delta_brst_l2]

Field-aligned electron flux from channel 4 of both GDUs [mms2_edi_flux4_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 4 of both GDUs [mms2_edi_flux4_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 4 of both GDUs. [mms2_edi_flux4_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 4 of both GDUs [mms2_edi_flux4_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 4 of both GDUs [mms2_edi_flux4_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 4 of both GDUs. [mms2_edi_flux4_180_delta_brst_l2]

Trajectory of field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms2_edi_traj1_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms2_edi_traj1_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 1 of both GDUs in GSE coordinates. [mms2_edi_traj1_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs, in GSE coordinates. [mms2_edi_traj1_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms2_edi_traj2_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms2_edi_traj2_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in GSE coordinates. [mms2_edi_traj2_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs, in GSE coordinates. [mms2_edi_traj2_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms2_edi_traj3_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms2_edi_traj3_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in GSE coordinates. [mms2_edi_traj3_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs, in GSE coordinates. [mms2_edi_traj3_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms2_edi_traj4_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms2_edi_traj4_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in GSE coordinates. [mms2_edi_traj4_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs, in GSE coordinates. [mms2_edi_traj4_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj1_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj1_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS2_EDI_BRST_L2_EFIELD (spase://NASA/NumericalData/MMS/2/FIELDS/EDI/Burst/Level2/ElectricField/PT0.0009765625S)

Description

EDI electric field data. Instrument papers for EDI can be found at:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7

Modification History

v1.0.0 - First version. TRI-TOF selection based on smallest error.
v1.1.0 - TRI-TOF merged by weighted average.
v1.2.0 - Fixed t_delta_plus/minus CDF_type.
v1.3.0 - Fixed Fixed vdrift SI conversion.
v1.4.0 - Fixed data duplication caused by multiple l2pre file locations.
v1.5.0 - Inplemented baseline*beams*Bmag filter for triangulation.
v1.6.0 - Inplemented null files for no or low quality data.

Data Variable Descriptions

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MMS2_EDI_BRST_L2_Q0 (spase://NASA/NumericalData/MMS/2/FIELDS/EDI/Burst/Level2/QualityZero/PT0.0078125S)

Description

EDI Q0 data. The EDI instrument paper and data products guidescan be found at
the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - First version.
v0.0.1 - Filled energy variables.
v0.0.2 - Energy written properly.
v1.0.0 - Update variable names.
v1.1.0 - Added optics state.
v2.0.0 - Added electron trajectories.
v2.1.0 - Deltas on trajectory vectors are now deltas.
v3.0.0 - Reduced file size with scalar errors. Add VAR_NOTES.
v3.1.0 - Fixed optics datatype.
v4.0.0 - Removed unused Epoch variable.
v5.0.0 - Trajectories are provided in DBCS coordinates.

Data Variable Descriptions

Optics state [mms2_edi_optics_state_brst_l2]

---> GDU1 energy [mms2_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms2_edi_energy_gdu2_brst_l2]

GDU1 quality 0 counts. [mms2_edi_counts_gdu1_brst_l2]

Q0 data consists of raw electron counts. The error at any one time is the
square-root of the counts. Note that there may be contamination from the EDI
electron beams. See the data products guide or contact an EDI team member to
learn about beam contamination.

GDU2 quality 0 counts. [mms2_edi_counts_gdu2_brst_l2]

GDU1 electron incident trajectory vectors in spherical BCS coordinates. [mms2_edi_traj_bcs_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical BCS coordinates. [mms2_edi_traj_bcs_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical DBCS coordinates. [mms2_edi_traj_dbcs_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical DBCS coordinates. [mms2_edi_traj_dbcs_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSE coordinates. [mms2_edi_traj_gse_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSE coordinates. [mms2_edi_traj_gse_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSM coordinates. [mms2_edi_traj_gsm_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSM coordinates. [mms2_edi_traj_gsm_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS2_EDI_SRVY_L2_AMB (spase://NASA/NumericalData/MMS/2/FIELDS/EDI/Survey/Level2/ElectronFluxAmbient/ProjectionMethod1/PT0.03125S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - Original version.
v1.0.0 - Include trajectory vectors and optics state.
v1.1.0 - Update metadata: counts -> flux.
v1.2.0 - Added flux error.
v1.3.0 - Trajectory vector errors are now deltas.
v1.4.0 - Fixed dead-time correction and error values.
v1.5.0 - Factor of 2 for accumulation time & 2 for abscal factor in srvy mode.
v1.6.0 - No factor of 2 for accumulation time in srvy mode.
v2.0.0 - Reduced file size with scalar errors. Update metadata.
v2.1.0 - Correct fill value for fluxes.
v3.0.0 - Omni-directional error for trajectories. Correct time deltas. Y-Version
linked to cal file. Single epoch for counts.
v4.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.

Data Variable Descriptions

Optics state [mms2_edi_optics_state_srvy_l2]

---> GDU1 energy [mms2_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms2_edi_energy_gdu2_srvy_l2]

Field-aligned electron flux from both GDUs [mms2_edi_flux1_0_srvy_l2]

---> (no error bars displayed) Field-aligned electron flux from both GDUs [mms2_edi_flux1_0_srvy_l2_noerr]

---> Error in field-aligned electron flux from both GDUs. [mms2_edi_flux1_0_delta_srvy_l2]

Anti-field-aligned electron flux from both GDUs [mms2_edi_flux1_180_srvy_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from both GDUs [mms2_edi_flux1_180_srvy_l2_noerr]

---> Error in anti-field-aligned electron flux from both GDUs. [mms2_edi_flux1_180_delta_srvy_l2]

Trajectory of field-aligned electrons from both GDUs in DBCS coordinates. [mms2_edi_traj1_dbcs_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs in DBCS coordinates. [mms2_edi_traj1_dbcs_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from both GDUs in GSE coordinates. [mms2_edi_traj1_gse_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs, in GSE coordinates. [mms2_edi_traj1_gse_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj1_gsm_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj1_gsm_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS2_EDI_SRVY_L2_AMB-PM2 (spase://NASA/NumericalData/MMS/2/FIELDS/EDI/Survey/Level2/ElectronFluxAmbient/ProjectionMethod2/PT0.03125S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v1.0.0 - Original version.
v1.1.0 - Correct fill value for fluxes.
v2.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v3.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.
v4.0.0 - Each trajectory has its own LABL_PTR_1 variable.

Data Variable Descriptions

Optics state [mms2_edi_optics_state_srvy_l2]

---> GDU1 energy [mms2_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms2_edi_energy_gdu2_srvy_l2]

Field-aligned electron flux from both GDUs [mms2_edi_flux1_0_srvy_l2]

---> (no error bars displayed) Field-aligned electron flux from both GDUs [mms2_edi_flux1_0_srvy_l2_noerr]

---> Error in field-aligned electron flux from both GDUs. [mms2_edi_flux1_0_delta_srvy_l2]

Anti-field-aligned electron flux from both GDUs [mms2_edi_flux1_180_srvy_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from both GDUs [mms2_edi_flux1_180_srvy_l2_noerr]

---> Error in anti-field-aligned electron flux from both GDUs. [mms2_edi_flux1_180_delta_srvy_l2]

Trajectory of field-aligned electrons from both GDUs in DBCS coordinates. [mms2_edi_traj1_dbcs_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs in DBCS coordinates. [mms2_edi_traj1_dbcs_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from both GDUs in GSE coordinates. [mms2_edi_traj1_gse_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs, in GSE coordinates. [mms2_edi_traj1_gse_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj1_gsm_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms2_edi_traj1_gsm_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS2_EDI_SRVY_L2_EFIELD (spase://NASA/NumericalData/MMS/2/FIELDS/EDI/Survey/Level2/ElectricField/PT5S)

Description

EDI electric field data. Instrument papers for EDI can be found at:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7

Modification History

v1.0.0 - First version. TRI-TOF selection based on smallest error.
v1.1.0 - TRI-TOF merged by weighted average.
v1.2.0 - Fixed t_delta_plus/minus CDF_type.
v1.3.0 - Fixed Fixed vdrift SI conversion.
v1.4.0 - Fixed data duplication caused by multiple l2pre file locations.
v1.5.0 - Inplemented baseline*beams*Bmag filter for triangulation.
v1.6.0 - Inplemented null files for no or low quality data.

Data Variable Descriptions

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MMS2_EDI_SRVY_L2_Q0 (spase://NASA/NumericalData/MMS/2/FIELDS/EDI/Survey/Level2/QualityZero/PT0.125S)

Description

EDI Q0 data. The EDI instrument paper and data products guidescan be found at
the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - First version.
v0.0.1 - Filled energy variables.
v0.0.2 - Energy written properly.
v1.0.0 - Update variable names.
v1.1.0 - Added optics state.
v2.0.0 - Added electron trajectories.
v2.1.0 - Deltas on trajectory vectors are now deltas.
v3.0.0 - Reduced file size with scalar errors. Add VAR_NOTES.
v4.0.0 - Removed unused Epoch variable.
v5.0.0 - Trajectories are provided in DBCS coordinates.

Data Variable Descriptions

Optics state [mms2_edi_optics_state_srvy_l2]

---> GDU1 energy [mms2_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms2_edi_energy_gdu2_srvy_l2]

GDU1 quality 0 counts. [mms2_edi_counts_gdu1_srvy_l2]

Q0 data consists of raw electron counts. The error at any one time is the
square-root of the counts. Note that there may be contamination from the EDI
electron beams. See the data products guide or contact an EDI team member to
learn about beam contamination.

GDU2 quality 0 counts. [mms2_edi_counts_gdu2_srvy_l2]

GDU1 electron incident trajectory vectors in spherical BCS coordinates. [mms2_edi_traj_bcs_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical BCS coordinates. [mms2_edi_traj_bcs_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical DBCS coordinates. [mms2_edi_traj_dbcs_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical DBCS coordinates. [mms2_edi_traj_dbcs_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSE coordinates. [mms2_edi_traj_gse_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSE coordinates. [mms2_edi_traj_gse_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSM coordinates. [mms2_edi_traj_gsm_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSM coordinates. [mms2_edi_traj_gsm_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS2_EDP_BRST_L2_DCE (spase://NASA/NumericalData/MMS/2/FIELDS/EDP/Burst/Level2/DCElectricField/PT0.0001220703125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS2_EDP_BRST_L2_HMFE (spase://NASA/NumericalData/MMS/2/FIELDS/EDP/Burst/Level2Pre/HMFE/PT0.00001525878906S)

Description

Data Variable Descriptions

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MMS2_EDP_BRST_L2_SCPOT doi:10.48322/a6r6-hr28
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

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MMS2_EDP_FAST_L2_DCE (spase://NASA/NumericalData/MMS/2/FIELDS/EDP/Fast/Level2/DCElectricField/PT0.03125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS2_EDP_FAST_L2_SCPOT doi:10.48322/myvz-be60
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

Data Variable Descriptions

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MMS2_EDP_SLOW_L2_DCE (spase://NASA/NumericalData/MMS/2/FIELDS/EDP/Slow/Level2/DCElectricField/PT0.125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS2_EDP_SLOW_L2_SCPOT doi:10.48322/mgay-bk26
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

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MMS2_EDP_SRVY_L2_HFESP (spase://NASA/NumericalData/MMS/2/FIELDS/EDP/Survey/Level2/HighFrequencyElectricFieldSpectra/PT16S)

Description

 AC Electric Field

Data Variable Descriptions

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MMS2_EPD-EIS_BRST_L2_EXTOF (spase://NASA/NumericalData/MMS/2/EnergeticParticleDetector/EIS/Burst/Level2/EnergyByTimeOfFlight/PT0.605S)

Description

empty

Modification History

Constantly modifying this code

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MMS2_EPD-EIS_BRST_L2_PHXTOF (spase://NASA/NumericalData/MMS/2/EnergeticParticleDetector/EIS/Burst/Level2/PulseHeightByTimeOfFlight/PT0.605S)

Description

empty

Modification History

Constantly modifying this code

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MMS2_EPD-EIS_SRVY_L2_ELECTRONENERGY (spase://NASA/NumericalData/MMS/2/EnergeticParticleDetector/EIS/Survey/Level2/ElectronEnergySpectra/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS2_EPD-EIS_SRVY_L2_EXTOF (spase://NASA/NumericalData/MMS/2/EnergeticParticleDetector/EIS/Survey/Level2/EnergyByTimeOfFlight/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

Data Variable Descriptions

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MMS2_EPD-EIS_SRVY_L2_PHXTOF (spase://NASA/NumericalData/MMS/2/EnergeticParticleDetector/EIS/Survey/Level2/PulseHeightByTimeOfFlight/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS2_FEEPS_BRST_L2_ELECTRON (spase://NASA/NumericalData/MMS/2/EnergeticParticleDetector/FEEPS/Burst/Level2/Electron/PT0.3025S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS2_FEEPS_BRST_L2_ION (spase://NASA/NumericalData/MMS/2/EnergeticParticleDetector/FEEPS/Burst/Level2/Ion/PT0.3025S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS2_FEEPS_SRVY_L2_ELECTRON (spase://NASA/NumericalData/MMS/2/EnergeticParticleDetector/FEEPS/Survey/Level2/Electron/PT2.42S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS2_FEEPS_SRVY_L2_ION (spase://NASA/NumericalData/MMS/2/EnergeticParticleDetector/FEEPS/Survey/Level2/Ion/PT2.42S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS2_FGM_BRST_L2 (spase://NASA/NumericalData/MMS/2/FIELDS/FGM/Burst/Level2/PT0.0078125S)

Description

The Fluxgate Magnetometers (FGM) on Magnetospheric Multiscale consist of a
traditional Analog Fluxgate Magnetometer (AFG), and a Digital Fluxgate
magnetometer (DFG). The dual magnetometers are operated as a single instrument
providing a single intercalibrated data product. Range changes occur at
different times on the two instruments so the gains checked each periapsis can
be carried out unambiguously to apoapsis. Cross correlation of calibration
parameters can separate causes of the any apparent calibration changes. Use of
Electron Drift Instrument (EDI) to determine the field along the rotation axis
allows accurate monitoring of the zero levels along the rotation axis.  Prior to
launch the magnetometers were calibrated at the Technical University,
Braunschweig, except for the AFG magnetometers on MMS3 and MMS4, which were
calibrated at UCLA.  Both sets of sensors are operated for the entire MMS orbit,
with slow survey (8 samples per second) outside of the Region of Interest (ROI),
and fast survey (16 samples per second) inside the ROI. Within the ROI burst
mode data (128 samples per second) are also acquired.  A detailed description of
the MMS fluxgate magnetometers, including science objectives, instrument
description, calibration, magnetic cleanliness program, and data flow can be
found at http://link.springer.com/article/10.1007%2Fs11214-014-0057-3 (DOI 
10.1007/s11214-014-0057-3).Additional information can also be found at
http://www-spc.igpp.ucla.edu/ssc/mms (UCLA),and http://www.iwf.oeaw.ac.at (IWF,
Graz).
For the purpose of creating a unified FGM Level2 data product, burst mode data
is taken from DFG and survey mode data is taken from AFG.  Because AFG and DFG
are cross-calibrated on an orbit-averaged basis, small differences in offset may
be observed between Level2 burst and survey mode data.  Consequently, any
differences are within the error of the measurement. Based on preliminary
analysis of the data, the absolute error within the Region of Interest (ROI) is
estimated to be no more than 0.1 nT in the spin-plane, 0.15 nT along the
spin-axis and 0.2 nT in total magnitude.

Modification History

version X=5:  * Y-version number comes from cal file entries. 
              *
Ensures there are 2 ephemeris points before/after data to enable proper spline. 

              * Fix to depend_0 of rdeltahalf:  fixes bug when reading position
data.
              * L-vector for DMPA2GSE transformation is smoothed with a
gaussian filter, instead 
                of using a single average value for
the day.  This short-term filter avoids  
                introduding artificial
jumps at 00:00 UTC and removes 7-minute 'wobble' after  
               
maneuvers in the GSE result.   
              * Fixes error with DEFATT file
selection found when choosing the 
                daily DEFATT files to be used
in Phase 2.
              * Fixed bug where reference Etemp was used for high
range gain.  Now uses measured Etemp.
version X=4:  First version for public
release of L2.
              Renamed variables to conform with new MMS variable
name guidelines 
              (obs_instr_paramName[_coordSys]_mode_level):  
  
             Mag field parameters include 'b' for paramName.  
               
Use 'r' instead of 'pos' for S/C position paramName.  
               
Eliminated 'rate', replaced with 'bdeltahalf'.  Added 'rdeltahalf'.
            
   l1a_mode is now just 'mode'.
version X=3:  fixed removal of overlap between
modes.
              fixed a bug that caused stemp and etemp to be
empty.
version X=2:  flag parameter name corrected: was 'status'
               
        added bits 4, 5, 6 to flag saturation on B1, B2, and B3, respectively
  
                     added bit 7 to flag bad data at range changes
             
Added etemp and l1a_mode parameters.  
              rate, hirange, and stemp
parameters now comply with MMS CDF Guidlelines, e.g.
              FILLVAL now
defined for stemp and etemp, and is set to !values.f_nan
              No longer
use Var_Parents attribute in stemp -- see Parents instead
              In this
version, temperature-corrected gains are applied.  Reference temperatures are
used when 
              stemp or etemp are set to FILLVAL. 
             
Non-linearity correction is applied to high rage DFG data.
version X=1:  added
'flag', rate and hirange parameters (but 'flag' is actually called 'status')

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MMS2_FGM_SRVY_L2 (spase://NASA/NumericalData/MMS/2/FIELDS/FGM/Survey/Level2/PT0.125S)

Description

The Fluxgate Magnetometers (FGM) on Magnetospheric Multiscale consist of a
traditional Analog Fluxgate Magnetometer (AFG), and a Digital Fluxgate
magnetometer (DFG). The dual magnetometers are operated as a single instrument
providing a single intercalibrated data product. Range changes occur at
different times on the two instruments so the gains checked each periapsis can
be carried out unambiguously to apoapsis. Cross correlation of calibration
parameters can separate causes of the any apparent calibration changes. Use of
Electron Drift Instrument (EDI) to determine the field along the rotation axis
allows accurate monitoring of the zero levels along the rotation axis.  Prior to
launch the magnetometers were calibrated at the Technical University,
Braunschweig, except for the AFG magnetometers on MMS3 and MMS4, which were
calibrated at UCLA.  Both sets of sensors are operated for the entire MMS orbit,
with slow survey (8 samples per second) outside of the Region of Interest (ROI),
and fast survey (16 samples per second) inside the ROI. Within the ROI burst
mode data (128 samples per second) are also acquired.  A detailed description of
the MMS fluxgate magnetometers, including science objectives, instrument
description, calibration, magnetic cleanliness program, and data flow can be
found at http://link.springer.com/article/10.1007%2Fs11214-014-0057-3 (DOI 
10.1007/s11214-014-0057-3).Additional information can also be found at
http://www-spc.igpp.ucla.edu/ssc/mms (UCLA),and http://www.iwf.oeaw.ac.at (IWF,
Graz).
For the purpose of creating a unified FGM Level2 data product, burst mode data
is taken from DFG and survey mode data is taken from AFG.  Because AFG and DFG
are cross-calibrated on an orbit-averaged basis, small differences in offset may
be observed between Level2 burst and survey mode data.  Consequently, any
differences are within the error of the measurement. Based on preliminary
analysis of the data, the absolute error within the Region of Interest (ROI) is
estimated to be no more than 0.1 nT in the spin-plane, 0.15 nT along the
spin-axis and 0.2 nT in total magnitude.

Modification History

version X=5:  * Y-version number comes from cal file entries. 
              *
Ensures there are 2 ephemeris points before/after data to enable proper spline. 

              * Fix to depend_0 of rdeltahalf:  fixes bug when reading position
data.
              * L-vector for DMPA2GSE transformation is smoothed with a
gaussian filter, instead 
                of using a single average value for
the day.  This short-term filter avoids  
                introduding artificial
jumps at 00:00 UTC and removes 7-minute 'wobble' after  
               
maneuvers in the GSE result.   
              * Fixes error with DEFATT file
selection found when choosing the 
                daily DEFATT files to be used
in Phase 2.
              * Fixed bug where reference Etemp was used for high
range gain.  Now uses measured Etemp.
version X=4:  First version for public
release of L2.
              Renamed variables to conform with new MMS variable
name guidelines 
              (obs_instr_paramName[_coordSys]_mode_level):  
  
             Mag field parameters include 'b' for paramName.  
               
Use 'r' instead of 'pos' for S/C position paramName.  
               
Eliminated 'rate', replaced with 'bdeltahalf'.  Added 'rdeltahalf'.
            
   l1a_mode is now just 'mode'.
version X=3:  fixed removal of overlap between
modes.
              fixed a bug that caused stemp and etemp to be
empty.
version X=2:  flag parameter name corrected: was 'status'
               
        added bits 4, 5, 6 to flag saturation on B1, B2, and B3, respectively
  
                     added bit 7 to flag bad data at range changes
             
Added etemp and l1a_mode parameters.  
              rate, hirange, and stemp
parameters now comply with MMS CDF Guidlelines, e.g.
              FILLVAL now
defined for stemp and etemp, and is set to !values.f_nan
              No longer
use Var_Parents attribute in stemp -- see Parents instead
              In this
version, temperature-corrected gains are applied.  Reference temperatures are
used when 
              stemp or etemp are set to FILLVAL. 
             
Non-linearity correction is applied to high rage DFG data.
version X=1:  added
'flag', rate and hirange parameters (but 'flag' is actually called 'status')

Data Variable Descriptions

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MMS2_FPI_BRST_L2_DES-DIST (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DES/Burst/Level2/Distribution/PT0.03S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data are taken at burst (30/150 ms for DES/DIS)
resolution in this mode.  Data are also made available at survey (4.5 s, etc)
resolution; these form a separate product from this.  Per mission design, not
all burst-resolution data are downlinked.  This product contains phase-space
distribution maps of those burst-resolution data selected for downlink.  In
particular, the (highest possible quality at the time of release)
corrected/converted "Burst SkyMap" distributions are reported with time-stamps
and other annotation characterizing the state of the instrument system at the
indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

[CDAWeb List/Download/Create ONLY] MMS2 FPI/DES burst sky-map instrument distribution [mms2_des_dist_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 10.9 eV (E1/even) [mms2_des_dist_brst1_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 12.4 eV (E1/odd) [mms2_des_dist_brst1_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~11.6 eV (E1 even-odd) [mms2_des_dist_brst1_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 10.9 eV (E1/even) [mms2_des_dist_brst1_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 12.4 eV (E1/odd) [mms2_des_dist_brst1_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 37.9 eV (E6/even) [mms2_des_dist_brst6_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 42.9 eV (E6/odd) [mms2_des_dist_brst6_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~40.4 eV (E6 even-odd) [mms2_des_dist_brst6_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 37.9 eV (E6/even) [mms2_des_dist_brst6_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 42.9 eV (E6/odd) [mms2_des_dist_brst6_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 80.0 eV (E9/even) [mms2_des_dist_brst9_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 90.6 eV (E9/odd) [mms2_des_dist_brst9_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~85 eV (E9 even-odd) [mms2_des_dist_brst9_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 80.0 eV (E9/even) [mms2_des_dist_brst9_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 90.6 eV (E9/odd) [mms2_des_dist_brst9_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 169 eV (E12/even) [mms2_des_dist_brst12_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 191 eV (E12/odd) [mms2_des_dist_brst12_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~180 eV (E12 even-odd) [mms2_des_dist_brst12_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 169 eV (E12/even) [mms2_des_dist_brst12_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 191 eV (E12/odd) [mms2_des_dist_brst12_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 277 eV (E14/even) [mms2_des_dist_brst14_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 314 eV (E14/odd) [mms2_des_dist_brst14_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~295 eV (E14 even-odd) [mms2_des_dist_brst14_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 277 eV (E14/even) [mms2_des_dist_brst14_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 314 eV (E14/odd) [mms2_des_dist_brst14_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 456 eV (E16/even) [mms2_des_dist_brst16_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 517 eV (E16/odd) [mms2_des_dist_brst16_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~485 eV (E16 even-odd) [mms2_des_dist_brst16_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 456 eV (E16/even) [mms2_des_dist_brst16_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 517 eV (E16/odd) [mms2_des_dist_brst16_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 750 eV (E18/even) [mms2_des_dist_brst18_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 850 eV (E18/odd) [mms2_des_dist_brst18_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~800 eV (E18 even-odd) [mms2_des_dist_brst18_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 750 eV (E18/even) [mms2_des_dist_brst18_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 850 eV (E18/odd) [mms2_des_dist_brst18_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 1230 eV (E20/even) [mms2_des_dist_brst20_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 1400 eV (E20/odd) [mms2_des_dist_brst20_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~1310 eV (E20 even-odd) [mms2_des_dist_brst20_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1230 eV (E20/even) [mms2_des_dist_brst20_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1400 eV (E20/odd) [mms2_des_dist_brst20_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 2600 eV (E23/even) [mms2_des_dist_brst23_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 2950 eV (E23/odd) [mms2_des_dist_brst23_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~2770 eV (E23 even-odd) [mms2_des_dist_brst23_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2600 eV (E23/even) [mms2_des_dist_brst23_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2950 eV (E23/odd) [mms2_des_dist_brst23_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 5490 eV (E26/even) [mms2_des_dist_brst26_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 6210 eV (E26/odd) [mms2_des_dist_brst26_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~5840 eV (E26 even-odd) [mms2_des_dist_brst26_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5490 eV (E26/even) [mms2_des_dist_brst26_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 6210 eV (E26/odd) [mms2_des_dist_brst26_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 24400 eV (E32/even) [mms2_des_dist_brst32_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES burst sky-map instrument distribution - 27600 eV (E32/odd) [mms2_des_dist_brst32_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~26000 eV (E32 even-odd) [mms2_des_dist_brst32_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 24400 eV (E32/even) [mms2_des_dist_brst32_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 27600 eV (E32/odd) [mms2_des_dist_brst32_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[List/Create only in CDAWeb] 1-sigma error: MMS2 FPI/DES burst sky-map instrument distribution [mms2_des_disterr_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES vector of data-quality indicators at burst-start time [mms2_des_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS2 FPI/DES compression lossless/lossy indicator at survey-start time [mms2_des_compressionloss_brst]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

---> MMS2 FPI/DES step table parity, this burst [mms2_des_steptable_parity_brst]

FPI/DES alternates between two tables, designated "even" (0) and "odd" (1).

---> MMS2 FPI/DES Del-Phi (obs spin-phase) count at burst-start time [mms2_des_startdelphi_count_brst]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS2 FPI/DES Del-Phi (obs spin-phase) angle at burst-start time [mms2_des_startdelphi_angle_brst]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS2 FPI/DES burst average f1 count values [mms2_des_avgf1counts_brst]

Average f1-count level as a function of energy

MMS2 FPI/DES burst sky-map microsecond offsets from Epoch [mms2_des_steptimeoffsets_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order. Offsets reflect 128 steps over the 30 msec sweep
period. See FPI docs for details.

---> MMS2 FPI/DES sector de-Spin P value, this burst [mms2_des_sector_despinp_brst]

Records P-value used to de-spin this burst sky-map on board.  See FPI docs for
details.

MMS2 FPI/DES burst sky-map instrument azimuthal angles [mms2_des_phi_brst]

see FPI docs for details

MMS FPI/DES burst sky-map parity 0/1 energies [mms2_des_energy_brst]

Energies (parity 0/1) in the 64-step FPI energy table

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MMS2_FPI_BRST_L2_DES-MOMS (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DES/Burst/Level2/Moments/PT0.03S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode.  Data are also made available at survey (4.5
s, etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked.  Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available.  This product contains results from
integrating the standard moments of phase-space distributions formed from the
indicated data type (DES/DIS burst, FS or SS).  For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS2_FPI_BRST_L2_DES-PARTMOMS (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DES/Burst/Level2/PartialMoments/PT0.03S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s,
etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked. Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available. This product contains partial moments that
come from performing the standard moment integrals over a limited portion of
velocity space. The resulting quantities are named similarly to their
corresponding standard moments, but are decorated with 'part' to differentiate.
For example, density_part is the density moment integrated from a particular
energy step to infinity. These partial moments are formed from the indicated
data type (DES/DIS burst, FS or SS). For convenience, some additional parameters
are included to augment those most commonly found in a moments product of this
sort, plus time-stamps and other annotation characterizing the state of the
instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DES vector of data-quality indicators at burst-start time [mms2_des_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of brst l2pre
magnetic field, Bit-9 = srvy l2pre magnetic field used instead of brst l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS2 FPI/DES partial electron number density during this burst [mms2_des_numberdensity_part_brst]

MMS2 FPI/DES partial electron bulk-velocity vector in DBCS during this burst [mms2_des_bulkv_part_dbcs_brst]

MMS2 FPI/DES partial electron bulk-velocity vector in GSE during this burst [mms2_des_bulkv_part_gse_brst]

MMS2 FPI/DES partial electron pressure tensor in DBCS during this burst [mms2_des_prestensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES partial electron pressure tensor in GSE during this burst [mms2_des_prestensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES partial electron temperature tensor in DBCS during this burst [mms2_des_temptensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES partial electron temperature tensor in GSE during this burst [mms2_des_temptensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES partial electron parallel temperature during this burst [mms2_des_temppara_part_brst]

MMS2 FPI/DES partial electron perpendicular temperature during this burst [mms2_des_tempperp_part_brst]

MMS2 FPI/DES recommended energy index during this burst [mms2_des_part_index_brst]

Recommended energy index during this burst

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MMS2_FPI_BRST_L2_DIS-DIST (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DIS/Burst/Level2/Distribution/PT0.15S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data are taken at burst (30/150 ms for DES/DIS)
resolution in this mode.  Data are also made available at survey (4.5 s, etc)
resolution; these form a separate product from this.  Per mission design, not
all burst-resolution data are downlinked.  This product contains phase-space
distribution maps of those burst-resolution data selected for downlink.  In
particular, the (highest possible quality at the time of release)
corrected/converted "Burst SkyMap" distributions are reported with time-stamps
and other annotation characterizing the state of the instrument system at the
indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

[CDAWeb List/Download/Create ONLY] MMS2 FPI/DIS burst sky-map instrument distribution [mms2_dis_dist_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 10.6 eV (E1/even) [mms2_dis_dist_brst1_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 12.0 eV (E1/odd) [mms2_dis_dist_brst1_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~11.3 eV (E1 even-odd) [mms2_dis_dist_brst1_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 10.6 eV (E1/even) [mms2_dis_dist_brst1_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 12.0 eV (E1/odd) [mms2_dis_dist_brst1_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 37.2 eV (E6/even) [mms2_dis_dist_brst6_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 42.1 eV (E6/odd) [mms2_dis_dist_brst6_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~39.6 eV (E6 even-odd) [mms2_dis_dist_brst6_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 37.2 eV (E6/even) [mms2_dis_dist_brst6_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 42.1 eV (E6/odd) [mms2_dis_dist_brst6_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 78.8 eV (E9/even) [mms2_dis_dist_brst9_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 89.3 eV (E9/odd) [mms2_dis_dist_brst9_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~83.9 eV (E9 even-odd) [mms2_dis_dist_brst9_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 78.8 eV (E9/even) [mms2_dis_dist_brst9_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 89.3 eV (E9/odd) [mms2_dis_dist_brst9_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 167 eV (E12/even) [mms2_dis_dist_brst12_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 189 eV (E12/odd) [mms2_dis_dist_brst12_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~178 eV (E12 even-odd) [mms2_dis_dist_brst12_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 167 eV (E12/even) [mms2_dis_dist_brst12_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 189 eV (E12/odd) [mms2_dis_dist_brst12_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 275 eV (E14/even) [mms2_dis_dist_brst14_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 312 eV (E14/odd) [mms2_dis_dist_brst14_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~293 eV (E14 even-odd) [mms2_dis_dist_brst14_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 275 eV (E14/even) [mms2_dis_dist_brst14_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 312 eV (E14/odd) [mms2_dis_dist_brst14_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 455 eV (E16/even) [mms2_dis_dist_brst16_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 515 eV (E16/odd) [mms2_dis_dist_brst16_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~484 eV (E16 even-odd) [mms2_dis_dist_brst16_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 455 eV (E16/even) [mms2_dis_dist_brst16_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 515 eV (E16/odd) [mms2_dis_dist_brst16_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 750 eV (E18/even) [mms2_dis_dist_brst18_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 850 eV (E18/odd) [mms2_dis_dist_brst18_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~800 eV (E18 even-odd) [mms2_dis_dist_brst18_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 750 eV (E18/even) [mms2_dis_dist_brst18_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 850 eV (E18/odd) [mms2_dis_dist_brst18_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 1240 eV (E20/even) [mms2_dis_dist_brst20_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 1400 eV (E20/odd) [mms2_dis_dist_brst20_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~1320 eV (E20 even-odd) [mms2_dis_dist_brst20_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1240 eV (E20/even) [mms2_dis_dist_brst20_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1400 eV (E20/odd) [mms2_dis_dist_brst20_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 2620 eV (E23/even) [mms2_dis_dist_brst23_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 2970 eV (E23/odd) [mms2_dis_dist_brst23_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~2800 eV (E23 even-odd) [mms2_dis_dist_brst23_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2620 eV (E23/even) [mms2_dis_dist_brst23_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2970 eV (E23/odd) [mms2_dis_dist_brst23_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 5560 eV (E26/even) [mms2_dis_dist_brst26_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 6300 eV (E26/odd) [mms2_dis_dist_brst26_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~5920 eV (E26 even-odd) [mms2_dis_dist_brst26_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5560 eV (E26/even) [mms2_dis_dist_brst26_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 6300 eV (E26/odd) [mms2_dis_dist_brst26_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 25000 eV (E32/even) [mms2_dis_dist_brst32_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS burst sky-map instrument distribution - 28300 eV (E32/odd) [mms2_dis_dist_brst32_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~26600 eV (E32 even-odd) [mms2_dis_dist_brst32_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 25000 eV (E32/even) [mms2_dis_dist_brst32_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 28300 eV (E32/odd) [mms2_dis_dist_brst32_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[List/Create only in CDAWeb] 1-sigma error: MMS2 FPI/DIS burst sky-map instrument distribution [mms2_dis_disterr_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS vector of data-quality indicators at burst-start time [mms2_dis_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS2 FPI/DIS compression lossless/lossy indicator at survey-start time [mms2_dis_compressionloss_brst]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

---> MMS2 FPI/DIS step table parity, this burst [mms2_dis_steptable_parity_brst]

FPI/DIS alternates between two tables, designated "even" (0) and "odd" (1).

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) count at burst-start time [mms2_dis_startdelphi_count_brst]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at burst-start time [mms2_dis_startdelphi_angle_brst]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS2 FPI/DIS burst average f1 count values [mms2_dis_avgf1counts_brst]

Average f1-count level as a function of energy

MMS2 FPI/DIS burst sky-map microsecond offsets from Epoch [mms2_dis_steptimeoffsets_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order. Offsets reflect 128 steps over the 150 msec sweep
period. See FPI docs for details.

---> MMS2 FPI/DIS sector de-Spin P value, this burst [mms2_dis_sector_despinp_brst]

Records P-value used to de-spin this burst sky-map on board.  See FPI docs for
details.

MMS2 FPI/DIS burst sky-map instrument azimuthal angles [mms2_dis_phi_brst]

see FPI docs for details

MMS FPI/DIS burst sky-map parity 0/1 energies [mms2_dis_energy_brst]

Energies (parity 0/1) in the 64-step FPI energy table

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MMS2_FPI_BRST_L2_DIS-MOMS (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DIS/Burst/Level2/Moments/PT0.15S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode.  Data are also made available at survey (4.5
s, etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked.  Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available.  This product contains results from
integrating the standard moments of phase-space distributions formed from the
indicated data type (DES/DIS burst, FS or SS).  For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS2_FPI_BRST_L2_DIS-PARTMOMS (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DIS/Burst/Level2/PartialMoments/PT0.15S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s,
etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked. Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available. This product contains partial moments that
come from performing the standard moment integrals over a limited portion of
velocity space. The resulting quantities are named similarly to their
corresponding standard moments, but are decorated with 'part' to differentiate.
For example, density_part is the density moment integrated from a particular
energy step to infinity. These partial moments are formed from the indicated
data type (DES/DIS burst, FS or SS). For convenience, some additional parameters
are included to augment those most commonly found in a moments product of this
sort, plus time-stamps and other annotation characterizing the state of the
instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DIS vector of data-quality indicators at burst-start time [mms2_dis_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of brst l2pre
magnetic field, Bit-9 = srvy l2pre magnetic field used instead of brst l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS2 FPI/DIS partial ion number density during this burst [mms2_dis_numberdensity_part_brst]

MMS2 FPI/DIS partial ion bulk-velocity vector in DBCS during this burst [mms2_dis_bulkv_part_dbcs_brst]

MMS2 FPI/DIS partial ion bulk-velocity vector in GSE during this burst [mms2_dis_bulkv_part_gse_brst]

MMS2 FPI/DIS partial ion pressure tensor in DBCS during this burst [mms2_dis_prestensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS partial ion pressure tensor in GSE during this burst [mms2_dis_prestensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS partial ion temperature tensor in DBCS during this burst [mms2_dis_temptensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS partial ion temperature tensor in GSE during this burst [mms2_dis_temptensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS partial ion parallel temperature during this burst [mms2_dis_temppara_part_brst]

MMS2 FPI/DIS partial ion perpendicular temperature during this burst [mms2_dis_tempperp_part_brst]

MMS2 FPI/DIS recommended energy index during this burst [mms2_dis_part_index_brst]

Recommended energy index during this burst

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MMS2_FPI_FAST_L2_DES-DIST (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DES/Fast/Level2/Distribution/PT4.5S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data taken at burst (30/150 ms for DES/DIS)
resolution are aggregated on board and made available at survey (4.5 s)
resolution in this mode.  This product contains phase-space distribution maps of
results from surveying the high-resolution observations during each 4.5 s
period.  In particular, the (highest possible quality at the time of release)
corrected/converted "Fast Survey SkyMap" distributions are reported with
time-stamps and other annotation characterizing the state of the instrument
system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DES fast sky-map instrument distribution - 11.6 eV (E1) using averaged even/odd steps [mms2_des_dist_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 11.6 eV [mms2_des_dist_fast1_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES fast sky-map instrument distribution - 40.4 eV (E6) using averaged even/odd steps [mms2_des_dist_fast6]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 40.4 eV [mms2_des_dist_fast6_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES fast sky-map instrument distribution - 85.1 eV (E9) using averaged even/odd steps [mms2_des_dist_fast9]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 85.1 eV [mms2_des_dist_fast9_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES fast sky-map instrument distribution - 179 eV (E12) using averaged even/odd steps [mms2_des_dist_fast12]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 179 eV [mms2_des_dist_fast12_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES fast sky-map instrument distribution - 295 eV (E14) using averaged even/odd steps [mms2_des_dist_fast14]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 295 eV [mms2_des_dist_fast14_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES fast sky-map instrument distribution - 485 eV (E16) using averaged even/odd steps [mms2_des_dist_fast16]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 485 eV [mms2_des_dist_fast16_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES fast sky-map instrument distribution - 798 eV (E18) using averaged even/odd steps [mms2_des_dist_fast18]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 798 eV [mms2_des_dist_fast18_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES fast sky-map instrument distribution - 1310 eV (E20) using averaged even/odd steps [mms2_des_dist_fast20]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1310 eV [mms2_des_dist_fast20_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES fast sky-map instrument distribution - 2770 eV (E23) using averaged even/odd steps [mms2_des_dist_fast23]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2770 eV [mms2_des_dist_fast23_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES fast sky-map instrument distribution - 5840 eV (E26) using averaged even/odd steps [mms2_des_dist_fast26]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5840 eV [mms2_des_dist_fast26_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES fast sky-map instrument distribution - 26000 eV (E32) using averaged even/odd steps [mms2_des_dist_fast32]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 26000 eV [mms2_des_dist_fast32_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[Only List/Create in CDAWeb] MMS2 FPI/DES fast sky-map instrument distribution 1-sigma error [mms2_des_disterr_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES vector of data-quality indicators at fast survey-start time - 32-bit error flags [mms2_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS2 FPI/DES compression lossless/lossy indicator at survey-start time [mms2_des_compressionloss_fast]

FPI/DES compression loss indicator,0=lossless, 1=lossy

---> MMS2 FPI/DES Del-Phi (obs spin-phase) count at fast survey-start time [mms2_des_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS2 FPI/DES Del-Phi (obs spin-phase) angle at fast survey-start time [mms2_des_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS2 FPI/DES fast survey average f1 count values [mms2_des_avgf1counts_fast]

Average f1-count level as a function of energy

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MMS2_FPI_FAST_L2_DES-MOMS (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DES/Fast/Level2/Moments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution.  Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This moments product
contains results from integrating the standard moments of phase-space
distributions formed from the indicated data type (DES/DIS burst, FS or SS). For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotation characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS2_FPI_FAST_L2_DES-MOMSAUX

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DES vector of data-quality indicators at survey-start time [mms2_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS2 FPI/DES partial electron number density during this survey [mms2_des_numberdensity_part_fast]

MMS2 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms2_des_bulkv_part_dbcs_fast]

MMS2 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms2_des_bulkv_part_gse_fast]

MMS2 FPI/DES partial electron pressure tensor in DBCS during this survey [mms2_des_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES partial electron pressure tensor in GSE during this survey [mms2_des_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES partial electron temperature tensor in DBCS during this survey [mms2_des_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES partial electron temperature tensor in GSE during this survey [mms2_des_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES partial electron parallel temperature during this survey [mms2_des_temppara_part_fast]

MMS2 FPI/DES partial electron perpendicular temperature during this survey [mms2_des_tempperp_part_fast]

MMS2 FPI/DES recommended energy index for partial moments during this survey [mms2_des_part_index_fast]

Recommended energy index during this survey

MMS2 FPI/DES compression lossless/lossy indicator at survey-start time [mms2_des_compressionloss_fast]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS2 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms2_des_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS2 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms2_des_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS2 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms2_des_pitchangdist_lowen_fast]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size: 6
deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS2 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms2_des_pitchangdist_miden_fast]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS2 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms2_des_pitchangdist_highen_fast]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS2 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms2_des_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS2 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms2_des_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS2 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms2_des_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS2 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms2_des_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS2 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms2_des_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS2 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms2_des_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS2 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms2_des_energyspectr_par_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS2 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms2_des_energyspectr_anti_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS2 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms2_des_energyspectr_perp_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS2 FPI/DES omni-directional electron energy spectrum during this survey [mms2_des_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS2 FPI/DES electron number density during this survey [mms2_des_numberdensity_fast]

MMS2 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms2_des_densityextrapolation_low_fast]

MMS2 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms2_des_densityextrapolation_high_fast]

MMS2 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms2_des_bulkv_dbcs_fast]

MMS2 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this survey [mms2_des_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS2 FPI/DES electron bulk-velocity vector in GSE during this survey [mms2_des_bulkv_gse_fast]

MMS2 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this survey [mms2_des_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS2 FPI/DES electron pressure tensor in DBCS during this survey [mms2_des_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES electron pressure tensor in GSE during this survey [mms2_des_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES electron temperature tensor in DBCS during this survey [mms2_des_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES electron temperature tensor in GSE during this survey [mms2_des_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES electron heat-flux vector in DBCS during this survey [mms2_des_heatq_dbcs_fast]

MMS2 FPI/DES electron heat-flux vector in GSE during this survey [mms2_des_heatq_gse_fast]

MMS2 FPI/DES electron parallel temperature during this BP [mms2_des_temppara_fast]

MMS2 FPI/DES electron perpendicular temperature during this BP [mms2_des_tempperp_fast]

MMS2 FPI/DES S/C potential mean [mms2_des_scpot_mean_fast]

Average spacecraft potential during this FP used to shift the measure energies.

MMS2 FPI/DES S/C potential max [mms2_des_scpot_max_fast]

Maximum spacecraft potential during this FP used to exclude energies containing
spacecraft photoelectron fluxes.

MMS2 FPI/DES Mag data X,Y,Z,Norm DSC components [nT] at survey-start time [mms2_des_fpibentpipe_dsc_fast]

X, Y, Z are unit vector components.

Magnetic field vector X,Y,Z, and magnitude B [mms2_des_fpib_gse_srvy_fast]

Averaged survey magnetic field data during this FP

Magnetic field vector X,Y,Z, and magnitude B [mms2_des_fpib_dmpa_srvy_fast]

Averaged survey magnetic field data during this FP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms2_des_pos_gse_fast]

Position in GSM coordinates, 30 second [mms2_des_pos_gsm_fast]

MMS2 number density integrands [mms2_des_numberdensity_int_fast]

Integrand terms used in normalized energy integration for number density

number flux [mms2_des_numberflux_int_dbcs_fast]

Integrand terms used in normalized energy integration for number flux

MMS2 pressure tensor integrands [mms2_des_prestensor_int_dbcs_fast]

Integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms2_des_ugrid_int_fast]

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MMS2_FPI_FAST_L2_DES-PARTMOMS (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DES/Fast/Level2/PartialMoments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DES vector of data-quality indicators at survey-start time [mms2_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS2 FPI/DES partial electron number density during this survey [mms2_des_numberdensity_part_fast]

MMS2 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms2_des_bulkv_part_dbcs_fast]

MMS2 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms2_des_bulkv_part_gse_fast]

MMS2 FPI/DES partial electron pressure tensor in DBCS during this survey [mms2_des_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES partial electron pressure tensor in GSE during this survey [mms2_des_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES partial electron temperature tensor in DBCS during this survey [mms2_des_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES partial electron temperature tensor in GSE during this survey [mms2_des_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES partial electron parallel temperature during this survey [mms2_des_temppara_part_fast]

MMS2 FPI/DES partial electron perpendicular temperature during this survey [mms2_des_tempperp_part_fast]

MMS2 FPI/DES recommended energy index during this survey [mms2_des_part_index_fast]

Recommended energy index during this survey

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MMS2_FPI_FAST_L2_DIS-DIST (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DIS/Fast/Level2/Distribution/PT4.5S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data taken at burst (30/150 ms for DES/DIS)
resolution are aggregated on board and made available at survey (4.5 s)
resolution in this mode.  This product contains phase-space distribution maps of
results from surveying the high-resolution observations during each 4.5 s
period.  In particular, the (highest possible quality at the time of release)
corrected/converted "Fast Survey SkyMap" distributions are reported with
time-stamps and other annotation characterizing the state of the instrument
system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DIS fast sky-map instrument distribution - 11.3 eV (E1) using averaged even/odd steps [mms2_dis_dist_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 11.3 eV [mms2_dis_dist_fast1_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS fast sky-map instrument distribution - 39.6 eV (E6) using averaged even/odd steps [mms2_dis_dist_fast6]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 39.6 eV [mms2_dis_dist_fast6_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS fast sky-map instrument distribution - 83.9 eV (E9 using averaged even/odd steps) [mms2_dis_dist_fast9]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 83.9 eV [mms2_dis_dist_fast9_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS fast sky-map instrument distribution - 178 eV (E12) using averaged even/odd steps [mms2_dis_dist_fast12]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 178 eV [mms2_dis_dist_fast12_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS fast sky-map instrument distribution - 293 eV (E14) using averaged even/odd steps [mms2_dis_dist_fast14]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 293 eV [mms2_dis_dist_fast14_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS fast sky-map instrument distribution - 484 eV (E16) using averaged even/odd steps [mms2_dis_dist_fast16]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 484 eV [mms2_dis_dist_fast16_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS fast sky-map instrument distribution - 799 eV (E18) using averaged even/odd steps [mms2_dis_dist_fast18]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 799 eV [mms2_dis_dist_fast18_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS fast sky-map instrument distribution - 1320 eV (E20) using averaged even/odd steps [mms2_dis_dist_fast20]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1320 eV [mms2_dis_dist_fast20_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS fast sky-map instrument distribution - 2800 eV (E23) using averaged even/odd steps [mms2_dis_dist_fast23]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2800 eV [mms2_dis_dist_fast23_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS fast sky-map instrument distribution - 5920 eV (E26) using averaged even/odd steps [mms2_dis_dist_fast26]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5920 eV [mms2_dis_dist_fast26_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS fast sky-map instrument distribution - 26600 eV (E32) using averaged even/odd steps [mms2_dis_dist_fast32]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 26600 eV [mms2_dis_dist_fast32_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[Only List/Create in CDAWeb] MMS2 FPI/DIS fast sky-map instrument distribution 1-sigma error [mms2_dis_disterr_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS vector of data-quality indicators at fast survey-start time - 32-bit error flags [mms2_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS2 FPI/DIS compression lossless/lossy indicator at survey-start time [mms2_dis_compressionloss_fast]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) count at fast survey-start time [mms2_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at fast survey-start time [mms2_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS2 FPI/DIS fast survey average f1 count values [mms2_dis_avgf1counts_fast]

Average f1-count level as a function of energy

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MMS2_FPI_FAST_L2_DIS-MOMS (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DIS/Fast/Level2/Moments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution.  Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This moments product
contains results from integrating the standard moments of phase-space
distributions formed from the indicated data type (DES/DIS burst, FS or SS). For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotation characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DIS vector of data-quality indicators at survey-start time [mms2_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation, Bit-14 =
high MMS3 spintone due to DIS008 anomaly

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms2_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

---> MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms2_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS2 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms2_dis_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

---> MMS2 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms2_dis_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

---> MMS2 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms2_dis_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

---> MMS2 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms2_dis_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

---> MMS2 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms2_dis_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

---> MMS2 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms2_dis_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS2 FPI/DIS omni-directional ion energy spectrum during this survey [mms2_dis_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS2 FPI/DIS ion background energy during this survey [mms2_dis_spectr_bg_fast]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS2 FPI/DIS ion background number density during this survey [mms2_dis_numberdensity_bg_fast]

Background number density derived via integration of the estimated background
differential energy flux.

MMS2 FPI/DIS ion number density during this survey [mms2_dis_numberdensity_fast]

---> (no error bars displayed) MMS2 FPI/DIS ion number density during this survey [mms2_dis_numberdensity_fast_noerr]

MMS2 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms2_dis_densityextrapolation_low_fast]

MMS2 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms2_dis_densityextrapolation_high_fast]

MMS2 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms2_dis_bulkv_dbcs_fast]

---> (no error bars displayed) MMS2 FPI/DIS ion bulk-velocity DBCS vector during this survey [mms2_dis_bulkv_dbcs_fast_noerr]

MMS2 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey [mms2_dis_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS2 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms2_dis_bulkv_gse_fast]

MMS2 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey [mms2_dis_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

---> (no error bars displayed) MMS2 FPI/DIS ion bulk-velocity GSE vector during this survey [mms2_dis_bulkv_gse_fast_noerr]

MMS2 FPI/DIS ion pressure tensor in DBCS during this survey [mms2_dis_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS ion pressure tensor in GSE during this survey [mms2_dis_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS ion background pressure during this survey [mms2_dis_pres_bg_fast]

MMS2 FPI/DIS ion temperature tensor in DBCS during this survey [mms2_dis_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS ion temperature tensor in GSE during this survey [mms2_dis_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS ion heat-flux vector in DBCS during this survey [mms2_dis_heatq_dbcs_fast]

MMS2 FPI/DIS ion heat-flux vector in GSE during this survey [mms2_dis_heatq_gse_fast]

MMS2 FPI/DIS ion parallel temperature during this BP [mms2_dis_temppara_fast]

MMS2 FPI/DIS ion perpendicular temperature during this BP [mms2_dis_tempperp_fast]

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MMS2_FPI_FAST_L2_DIS-MOMSAUX

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DIS vector of data-quality indicators at survey-start time [mms2_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS2 FPI/DIS partial ion number density during this survey [mms2_dis_numberdensity_part_fast]

MMS2 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms2_dis_bulkv_part_dbcs_fast]

MMS2 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms2_dis_bulkv_part_gse_fast]

MMS2 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms2_dis_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS partial ion pressure tensor in GSE during this survey [mms2_dis_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms2_dis_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS partial ion temperature tensor in GSE during this survey [mms2_dis_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS partial ion parallel temperature during this survey [mms2_dis_temppara_part_fast]

MMS2 FPI/DIS partial ion perpendicular temperature during this survey [mms2_dis_tempperp_part_fast]

MMS2 FPI/DIS recommended energy index for partial moments during this survey [mms2_dis_part_index_fast]

Recommended energy index during this survey

MMS2 FPI/DIS compression lossless/lossy indicator at survey-start time [mms2_dis_compressionloss_fast]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS2 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms2_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms2_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS2 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms2_dis_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS2 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms2_dis_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS2 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms2_dis_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS2 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms2_dis_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS2 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms2_dis_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS2 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms2_dis_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS2 FPI/DIS omni-directional ion energy spectrum during this survey [mms2_dis_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS2 FPI/DIS ion background energy during this survey [mms2_dis_spectr_bg_fast]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS2 FPI/DIS ion background number density during this survey [mms2_dis_numberdensity_bg_fast]

Background number density derived via integration of the estimated background
differential energy flux.

MMS2 FPI/DIS ion number density during this survey [mms2_dis_numberdensity_fast]

MMS2 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms2_dis_densityextrapolation_low_fast]

MMS2 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms2_dis_densityextrapolation_high_fast]

MMS2 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms2_dis_bulkv_dbcs_fast]

MMS2 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey [mms2_dis_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS2 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms2_dis_bulkv_gse_fast]

MMS2 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey [mms2_dis_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS2 FPI/DIS ion pressure tensor in DBCS during this survey [mms2_dis_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS ion pressure tensor in GSE during this survey [mms2_dis_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS ion background pressure during this survey [mms2_dis_pres_bg_fast]

MMS2 FPI/DIS ion temperature tensor in DBCS during this survey [mms2_dis_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS ion temperature tensor in GSE during this survey [mms2_dis_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS ion heat-flux vector in DBCS during this survey [mms2_dis_heatq_dbcs_fast]

MMS2 FPI/DIS ion heat-flux vector in GSE during this survey [mms2_dis_heatq_gse_fast]

MMS2 FPI/DIS ion parallel temperature during this BP [mms2_dis_temppara_fast]

MMS2 FPI/DIS ion perpendicular temperature during this BP [mms2_dis_tempperp_fast]

MMS2 FPI/DIS S/C potential mean [mms2_dis_scpot_mean_fast]

Average spacecraft potential during this FP used to shift the measure energies.

MMS2 FPI/DIS S/C potential max [mms2_dis_scpot_max_fast]

Maximum spacecraft potential during this FP used to exclude energies containing
spacecraft photoelectron fluxes.

MMS2 FPI/DIS Mag data X,Y,Z,Norm DSC components [nT] at survey-start time [mms2_dis_fpibentpipe_dsc_fast]

X, Y, Z are unit vector components.

Magnetic field vector X,Y,Z, and magnitude B [mms2_dis_fpib_gse_srvy_fast]

Averaged survey magnetic field data during this FP

Magnetic field vector X,Y,Z, and magnitude B [mms2_dis_fpib_dmpa_srvy_fast]

Averaged survey magnetic field data during this FP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms2_dis_pos_gse_fast]

Position in GSM coordinates, 30 second [mms2_dis_pos_gsm_fast]

MMS2 number density integrands [mms2_dis_numberdensity_int_fast]

integrand terms used in normalized energy integration for number density

number flux [mms2_dis_numberflux_int_dbcs_fast]

integrand terms used in normalized energy integration for number flux

MMS2 pressure tensor integrands [mms2_dis_prestensor_int_dbcs_fast]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms2_dis_ugrid_int_fast]

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MMS2_FPI_FAST_L2_DIS-PARTMOMS (spase://NASA/NumericalData/MMS/2/FastPlasmaInvestigation/DIS/Fast/Level2/PartialMoments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DIS vector of data-quality indicators at survey-start time [mms2_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS2 FPI/DIS partial ion number density during this survey [mms2_dis_numberdensity_part_fast]

MMS2 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms2_dis_bulkv_part_dbcs_fast]

MMS2 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms2_dis_bulkv_part_gse_fast]

MMS2 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms2_dis_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS partial ion pressure tensor in GSE during this survey [mms2_dis_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms2_dis_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS partial ion temperature tensor in GSE during this survey [mms2_dis_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS partial ion parallel temperature during this survey [mms2_dis_temppara_part_fast]

MMS2 FPI/DIS partial ion perpendicular temperature during this survey [mms2_dis_tempperp_part_fast]

MMS2 FPI/DIS recommended energy index during this survey [mms2_dis_part_index_fast]

Recommended energy index during this survey

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MMS2_FPI_SLOW_L2_DES-DIST

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode.  This product contains phase-space distribution maps of those
survey-resolution data from Slow Mode.  In particular, the (highest possible
quality at the time of release) corrected/converted "Slow Survey SkyMap"
distributions are reported with time-stamps and other annotation characterizing
the state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DES vector of data-quality indicators at survey-start time [mms2_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = compression pipeline error

MMS2 FPI/DES compression lossless/lossy indicator at survey-start time [mms2_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS2 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms2_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS2 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms2_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS2 FPI/DES Slow Survey sky-map instrument distribution [mms2_des_dist_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES Slow Survey sky-map instrument distribution 1-sigma error [mms2_des_disterr_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DES slow survey average f1 count values [mms2_des_avgf1counts_slow]

Average f1-count level as a function of energy

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MMS2_FPI_SLOW_L2_DES-MOMS

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DES vector of data-quality indicators at survey-start time [mms2_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only)

MMS2 FPI/DES compression lossless/lossy indicator at survey-start time [mms2_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS2 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms2_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS2 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms2_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS2 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms2_des_pitchangdist_lowen_slow]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS2 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms2_des_pitchangdist_miden_slow]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS2 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms2_des_pitchangdist_highen_slow]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS2 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms2_des_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS2 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms2_des_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS2 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms2_des_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS2 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms2_des_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS2 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms2_des_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS2 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms2_des_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS2 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms2_des_energyspectr_par_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS2 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms2_des_energyspectr_anti_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS2 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms2_des_energyspectr_perp_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS2 FPI/DES omni-directional electron energy spectrum during this survey [mms2_des_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS2 FPI/DES electron number density during this survey [mms2_des_numberdensity_slow]

MMS2 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms2_des_densityextrapolation_low_slow]

MMS2 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms2_des_densityextrapolation_high_slow]

MMS2 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms2_des_bulkv_dbcs_slow]

MMS2 FPI/DES electron bulk-velocity vector in GSE during this survey [mms2_des_bulkv_gse_slow]

MMS2 FPI/DES electron pressure tensor in DBCS during this survey [mms2_des_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES electron pressure tensor in GSE during this survey [mms2_des_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES electron temperature tensor in DBCS during this survey [mms2_des_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES electron temperature tensor in GSE during this survey [mms2_des_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES electron heat-flux vector in DBCS during this survey [mms2_des_heatq_dbcs_slow]

MMS2 FPI/DES electron heat-flux vector in GSE during this survey [mms2_des_heatq_gse_slow]

MMS2 FPI/DES electron parallel temperature during this BP [mms2_des_temppara_slow]

MMS2 FPI/DES electron perpendicular temperature during this BP [mms2_des_tempperp_slow]

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MMS2_FPI_SLOW_L2_DES-MOMSAUX

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DES vector of data-quality indicators at survey-start time [mms2_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only)

MMS2 FPI/DES partial electron number density during this survey [mms2_des_numberdensity_part_slow]

MMS2 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms2_des_bulkv_part_dbcs_slow]

MMS2 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms2_des_bulkv_part_gse_slow]

MMS2 FPI/DES partial electron pressure tensor in DBCS during this survey [mms2_des_prestensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES partial electron pressure tensor in GSE during this survey [mms2_des_prestensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES partial electron temperature tensor in DBCS during this survey [mms2_des_temptensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES partial electron temperature tensor in GSE during this survey [mms2_des_temptensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES partial electron parallel temperature during this survey [mms2_des_temppara_part_slow]

MMS2 FPI/DES partial electron perpendicular temperature during this survey [mms2_des_tempperp_part_slow]

MMS2 FPI/DES recommended energy index for partial moments during this survey [mms2_des_part_index_slow]

Recommended energy index during this survey

MMS2 FPI/DES compression lossless/lossy indicator at survey-start time [mms2_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS2 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms2_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS2 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms2_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS2 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms2_des_pitchangdist_lowen_slow]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS2 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms2_des_pitchangdist_miden_slow]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS2 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms2_des_pitchangdist_highen_slow]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS2 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms2_des_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS2 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms2_des_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS2 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms2_des_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS2 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms2_des_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS2 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms2_des_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS2 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms2_des_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS2 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms2_des_energyspectr_par_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS2 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms2_des_energyspectr_anti_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS2 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms2_des_energyspectr_perp_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS2 FPI/DES omni-directional electron energy spectrum during this survey [mms2_des_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS2 FPI/DES electron number density during this survey [mms2_des_numberdensity_slow]

MMS2 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms2_des_densityextrapolation_low_slow]

MMS2 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms2_des_densityextrapolation_high_slow]

MMS2 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms2_des_bulkv_dbcs_slow]

MMS2 FPI/DES electron bulk-velocity vector in GSE during this survey [mms2_des_bulkv_gse_slow]

MMS2 FPI/DES electron pressure tensor in DBCS during this survey [mms2_des_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES electron pressure tensor in GSE during this survey [mms2_des_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DES electron temperature tensor in DBCS during this survey [mms2_des_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES electron temperature tensor in GSE during this survey [mms2_des_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DES electron heat-flux vector in DBCS during this survey [mms2_des_heatq_dbcs_slow]

MMS2 FPI/DES electron heat-flux vector in GSE during this survey [mms2_des_heatq_gse_slow]

MMS2 FPI/DES electron parallel temperature during this BP [mms2_des_temppara_slow]

MMS2 FPI/DES electron perpendicular temperature during this BP [mms2_des_tempperp_slow]

MMS2 FPI/DES S/C potential mean [mms2_des_scpot_mean_slow]

Average spacecraft potential during this SP used to shift the measure energies.

MMS2 FPI/DES S/C potential max [mms2_des_scpot_max_slow]

Maximum spacecraft potential during this SP used to exclude energies containing
spacecraft photoelectron fluxes.

Magnetic field vector X,Y,Z, and magnitude B [mms2_des_fpib_gse_srvy_slow]

Averaged survey magnetic field data during this SP

Magnetic field vector X,Y,Z, and magnitude B [mms2_des_fpib_dmpa_srvy_slow]

Averaged survey magnetic field data during this SP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms2_des_pos_gse_slow]

Position in GSM coordinates, 30 second [mms2_des_pos_gsm_slow]

MMS2 number density integrands [mms2_des_numberdensity_int_slow]

integrand terms used in normalized energy integration for number density

number flux [mms2_des_numberflux_int_dbcs_slow]

integrand terms used in normalized energy integration for number flux

MMS2 pressure tensor integrands [mms2_des_prestensor_int_dbcs_slow]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms2_des_ugrid_int_slow]

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MMS2_FPI_SLOW_L2_DIS-DIST

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode.  This product contains phase-space distribution maps of those
survey-resolution data from Slow Mode.  In particular, the (highest possible
quality at the time of release) corrected/converted "Slow Survey SkyMap"
distributions are reported with time-stamps and other annotation characterizing
the state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DIS vector of data-quality indicators at survey-start time [mms2_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = compression pipeline error

MMS2 FPI/DIS compression lossless/lossy indicator at survey-start time [mms2_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS2 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms2_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms2_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS2 FPI/DIS Slow Survey sky-map instrument distribution [mms2_dis_dist_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS Slow Survey sky-map instrument distribution 1-sigma error [mms2_dis_disterr_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS2 FPI/DIS slow survey average f1 count values [mms2_dis_avgf1counts_slow]

Average f1-count level as a function of energy

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MMS2_FPI_SLOW_L2_DIS-MOMS

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DIS vector of data-quality indicators at survey-start time [mms2_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only), Bit-13 =
significant (>=20%) penetrating radiation, Bit-14 = high MMS3 spintone due to
DIS008 anomaly

MMS2 FPI/DIS compression lossless/lossy indicator at survey-start time [mms2_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS2 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms2_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms2_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS2 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms2_dis_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS2 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms2_dis_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS2 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms2_dis_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS2 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms2_dis_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS2 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms2_dis_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS2 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms2_dis_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS2 FPI/DIS omni-directional ion energy spectrum during this survey [mms2_dis_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS2 FPI/DIS ion background energy during this survey [mms2_dis_spectr_bg_slow]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS2 FPI/DIS ion background number density during this survey [mms2_dis_numberdensity_bg_slow]

Background number density derived via integration of the estimated background
differential energy flux.

MMS2 FPI/DIS ion number density during this survey [mms2_dis_numberdensity_slow]

MMS2 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms2_dis_densityextrapolation_low_slow]

MMS2 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms2_dis_densityextrapolation_high_slow]

MMS2 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms2_dis_bulkv_dbcs_slow]

MMS2 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms2_dis_bulkv_gse_slow]

MMS2 FPI/DIS ion pressure tensor in DBCS during this survey [mms2_dis_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS ion pressure tensor in GSE during this survey [mms2_dis_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS ion background pressure during this survey [mms2_dis_pres_bg_slow]

MMS2 FPI/DIS ion temperature tensor in DBCS during this survey [mms2_dis_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS ion temperature tensor in GSE during this survey [mms2_dis_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS ion heat-flux vector in DBCS during this survey [mms2_dis_heatq_dbcs_slow]

MMS2 FPI/DIS ion heat-flux vector in GSE during this survey [mms2_dis_heatq_gse_slow]

MMS2 FPI/DIS ion parallel temperature during this BP [mms2_dis_temppara_slow]

MMS2 FPI/DIS ion perpendicular temperature during this BP [mms2_dis_tempperp_slow]

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MMS2_FPI_SLOW_L2_DIS-MOMSAUX

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS2 FPI/DIS vector of data-quality indicators at survey-start time [mms2_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only), Bit-13 =
significant (>=20%) penetrating radiation, Bit-14 = high MMS3 spintone due to
DIS008 anomaly

MMS2 FPI/DIS partial ion number density during this survey [mms2_dis_numberdensity_part_slow]

MMS2 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms2_dis_bulkv_part_dbcs_slow]

MMS2 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms2_dis_bulkv_part_gse_slow]

MMS2 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms2_dis_prestensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS partial ion pressure tensor in GSE during this survey [mms2_dis_prestensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms2_dis_temptensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS partial ion temperature tensor in GSE during this survey [mms2_dis_temptensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS partial ion parallel temperature during this survey [mms2_dis_temppara_part_slow]

MMS2 FPI/DIS partial ion perpendicular temperature during this survey [mms2_dis_tempperp_part_slow]

MMS2 FPI/DIS recommended energy index for partial moments during this survey [mms2_dis_part_index_slow]

Recommended energy index during this survey

MMS2 FPI/DIS compression lossless/lossy indicator at survey-start time [mms2_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS2 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms2_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS2 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms2_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS2 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms2_dis_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS2 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms2_dis_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS2 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms2_dis_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS2 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms2_dis_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS2 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms2_dis_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS2 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms2_dis_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS2 FPI/DIS omni-directional ion energy spectrum during this survey [mms2_dis_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS2 FPI/DIS ion background energy during this survey [mms2_dis_spectr_bg_slow]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS2 FPI/DIS ion background number density during this survey [mms2_dis_numberdensity_bg_slow]

Background number density derived via integration of the estimated background
differential energy flux.

MMS2 FPI/DIS ion number density during this survey [mms2_dis_numberdensity_slow]

MMS2 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms2_dis_densityextrapolation_low_slow]

MMS2 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms2_dis_densityextrapolation_high_slow]

MMS2 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms2_dis_bulkv_dbcs_slow]

MMS2 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms2_dis_bulkv_gse_slow]

MMS2 FPI/DIS ion pressure tensor in DBCS during this survey [mms2_dis_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS ion pressure tensor in GSE during this survey [mms2_dis_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS2 FPI/DIS ion background pressure during this survey [mms2_dis_pres_bg_slow]

MMS2 FPI/DIS ion temperature tensor in DBCS during this survey [mms2_dis_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS ion temperature tensor in GSE during this survey [mms2_dis_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS2 FPI/DIS ion heat-flux vector in DBCS during this survey [mms2_dis_heatq_dbcs_slow]

MMS2 FPI/DIS ion heat-flux vector in GSE during this survey [mms2_dis_heatq_gse_slow]

MMS2 FPI/DIS ion parallel temperature during this BP [mms2_dis_temppara_slow]

MMS2 FPI/DIS ion perpendicular temperature during this BP [mms2_dis_tempperp_slow]

MMS2 FPI/DIS S/C potential mean [mms2_dis_scpot_mean_slow]

Average spacecraft potential during this SP used to shift the measure energies.

MMS2 FPI/DIS S/C potential max [mms2_dis_scpot_max_slow]

Maximum spacecraft potential during this SP used to exclude energies containing
spacecraft photoelectron fluxes.

Magnetic field vector X,Y,Z, and magnitude B [mms2_dis_fpib_gse_srvy_slow]

Averaged survey magnetic field data during this SP

Magnetic field vector X,Y,Z, and magnitude B [mms2_dis_fpib_dmpa_srvy_slow]

Averaged survey magnetic field data during this SP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms2_dis_pos_gse_slow]

Position in GSM coordinates, 30 second [mms2_dis_pos_gsm_slow]

MMS2 number density integrands [mms2_dis_numberdensity_int_slow]

integrand terms used in normalized energy integration for number density

number flux [mms2_dis_numberflux_int_dbcs_slow]

integrand terms used in normalized energy integration for number flux

MMS2 pressure tensor integrands [mms2_dis_prestensor_int_dbcs_slow]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms2_dis_ugrid_int_slow]

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MMS2_HPCA_BRST_L2_ION (spase://NASA/NumericalData/MMS/2/HotPlasmaCompositionAnalyzer/Burst/Level2/Ion/PT0.625S)

Description

References

Modification History

Initial Public Release

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MMS2_HPCA_BRST_L2_MOMENTS (spase://NASA/NumericalData/MMS/2/HotPlasmaCompositionAnalyzer/Burst/Level2/Moments/PT10S)

Description

References

Modification History

Initial Public Release

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MMS2_HPCA_SRVY_L2_ION (spase://NASA/NumericalData/MMS/2/HotPlasmaCompositionAnalyzer/Survey/Level2/Ion/PT0.625S)

Description

References

Modification History

Initial Public Release

Data Variable Descriptions

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MMS2_HPCA_SRVY_L2_MOMENTS (spase://NASA/NumericalData/MMS/2/HotPlasmaCompositionAnalyzer/Survey/Level2/Moments/PT10S)

Description

References

Modification History

Initial Public Release

Data Variable Descriptions

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MMS2_HPCA_SRVY_L2_TOF-COUNTS (spase://NASA/NumericalData/MMS/2/HotPlasmaCompositionAnalyzer/Survey/Level2/TimeOfFlight/Counts/PT0.625S)

Description

References

Modification History

Initial Public Release

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MMS2_MEC_BRST_L2_EPHT89D (spase://NASA/NumericalData/MMS/2/Ephemeris/Burst/Level2/Tsyganenko_89_Dynamic/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS2_MEC_BRST_L2_EPHT89Q (spase://NASA/NumericalData/MMS/2/Ephemeris/Burst/Level2/Tsyganenko_89_Quiet/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS2_MEC_BRST_L2_EPHTS04D (spase://NASA/NumericalData/MMS/2/Ephemeris/Burst/Level2/Tsyganenko_04_Dynamic/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS2_MEC_SRVY_L2_EPHT89D (spase://NASA/NumericalData/MMS/2/Ephemeris/Survey/Level2/Tsyganenko_89_Dynamic/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS2_MEC_SRVY_L2_EPHT89Q (spase://NASA/NumericalData/MMS/2/Ephemeris/Survey/Level2/Tsyganenko_89_Quiet/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS2_MEC_SRVY_L2_EPHTS04D (spase://NASA/NumericalData/MMS/2/Ephemeris/Survey/Level2/Tsyganenko_04_Dynamic/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS2_R0_SUMMARY

Description

Pre-generated MMS Quicklook Summary Plots
File location: https://cdaweb.gsfc.nasa.gov/pub/data/mms/ql_plots/all_mms2_summ

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MMS2_SCM_BRST_L2_SCB (spase://NASA/NumericalData/MMS/2/FIELDS/SCM/Burst/Level2/PT0.0001220703125S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
https://urldefense.proofpoint.com/v2/url?u=http-3A__link.springer.com_article_10
.1007_s11214-2D014-2D0096-2D9&d=DwIFAg&c=c6MrceVCY5m5A_KAUkrdoA&r=bjziExGTRYoZgE
2xb_dDSm9NxNIo0lG6Q-rB0Y6rHS4&m=CMzo0Vv9zPtWSdbdY1Wq9-jIkYS2cOMV9JYZsMV10y0&s=Xb
P9PiEAswHGl5lqgsDVI6zs8ivJx7yek9i2undKl10&e=

Modification History

unpack telemetry, assign sample times
2026-07-10T20:11:42.00002789497058Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-16T12:36:37.00003266334522Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-16T12:36:43.00004035234439Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms2_scm_acb_gse_scb_brst_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 8192S/s.
They are high-pass filtered above 1.00Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide.

(List/Create Only) Quality Factor (one letter per antenna, G=good) [mms2_scm_qf_scm123_scb_brst_l2]

Each letter refers to one SCM physical antenna in the SCM123 order. 'G' stands
for good data, 'Z' for data that are affected or set to zero by convolution
boundary effect, 'S' for saturated data, 'X' for out of range data, 'B' for
fillvalue/bad data.

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MMS2_SCM_BRST_L2_SCHB (spase://NASA/NumericalData/MMS/2/FIELDS/SCM/Burst/Level2/PT0.00006101515625S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
http://link.springer.com/article/10.1007/s11214-014-0096-9

Modification History

unpack telemetry, assign sample times
2026-07-10T20:12:08.00004780292192Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-16T12:41:12.00002968311314Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-16T12:41:17.00004279613499Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms2_scm_acb_gse_schb_brst_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 16384S/s.
They are high-pass filtered above 32.00Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide
(https://lasp.colorado.edu/mms/sdc/public/datasets/fields/Science_Data_Products_ 
Guide_vol2_SCM_v11_20160301.pdf).

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MMS2_SCM_SRVY_L2_SCSRVY (spase://NASA/NumericalData/MMS/2/FIELDS/SCM/Survey/Level2/PT0.03125S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
http://link.springer.com/article/10.1007/s11214-014-0096-9

Modification History

unpack telemetry, assign sample times
2026-07-02T23:56:41.00003331899318Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-15T23:55:18.0000409483875Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-15T23:56:09.00004595517787Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms2_scm_acb_gse_scsrvy_srvy_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 32S/s. They
are high-pass filtered above 0.50Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide
(https://lasp.colorado.edu/mms/sdc/public/datasets/fields/Science_Data_Products_ 
Guide_vol2_SCM_v11_20160301.pdf).

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MMS3_ASPOC_SRVY_L2 (spase://NASA/NumericalData/MMS/3/ASPOC/Survey/Level2/PT1S)

Description

K. Torkar et al, Active Spacecraft Potential Control Investigation
Space Science Reviews, 2014, DOI: 10.1007/s11214-014-0049-3
Further information:
- http://www.iwf.oeaw.ac.at/en/research/near-earth-space/mms/ 
- http://mms.space.swri.edu/

Modification History

150224 Initial version
150831 Minor updates and fixes
160205 CDF file format guide compliant

Data Variable Descriptions

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MMS3_DSP_FAST_L2_BPSD (spase://NASA/NumericalData/MMS/3/FIELDS/DSP/Fast/Level2/MagneticFieldPowerSpectralDensity/PT2S)

Description

BPSD is the low frequency B spectral density covering the frequency range of .2
to 6000 Hz.

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MMS3_DSP_FAST_L2_EPSD (spase://NASA/NumericalData/MMS/3/FIELDS/DSP/Fast/Level2/ElectricFieldPowerSpectralDensity/PT2S)

Description

EPSD combines the low frequency E spectral density covering the frequency range
of 1 to 8000 Hz and the  medium frequency E spectral density covering the
frequency range of .25 to 100 kHz.

Data Variable Descriptions

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MMS3_DSP_SLOW_L2_BPSD (spase://NASA/NumericalData/MMS/3/FIELDS/DSP/Slow/Level2/MagneticFieldPowerSpectralDensity/PT16S)

Description

search coil magnetometer spectral density

Data Variable Descriptions

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MMS3_DSP_SLOW_L2_EPSD (spase://NASA/NumericalData/MMS/3/FIELDS/DSP/Slow/Level2/ElectricFieldPowerSpectralDensity/PT16S)

Description

electric spectral density

Data Variable Descriptions

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MMS3_EDI_BRST_L2_AMB (spase://NASA/NumericalData/MMS/3/FIELDS/EDI/Burst/Level2/ElectronFluxAmbient/ProjectionMethod1/PT0.0009765625S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - Original version.
v1.0.0 - Include trajectory vectors and optics state.
v1.1.0 - Update metadata: counts -> flux.
v1.2.0 - Added flux error.
v1.3.0 - Trajectory vector errors are now deltas.
v1.4.0 - Fixed dead-time correction and error values.
v1.5.0 - Factor of 2 for accumulation time & 2 for abscal factor in srvy mode.
v1.6.0 - No factor of 2 for accumulation time in srvy mode.
v2.0.0 - Reduced file size with scalar errors. Update metadata.
v2.1.0 - Correct fill value for fluxes.
v3.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v4.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.

Data Variable Descriptions

Optics state [mms3_edi_optics_state_brst_l2]

---> GDU1 energy [mms3_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms3_edi_energy_gdu2_brst_l2]

Flux for electrons with trajectories given by Traj-1 0PA [mms3_edi_flux1_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-1 0PA [mms3_edi_flux1_0_brst_l2_noerr]

---> Error for flux1 0-degree pitch angle electron flux. [mms3_edi_flux1_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-2 0PA [mms3_edi_flux2_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-2 0PA [mms3_edi_flux2_0_brst_l2_noerr]

---> Error for flux2 0-degree pitch angle electron flux. [mms3_edi_flux2_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-3 0PA [mms3_edi_flux3_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-3 0PA [mms3_edi_flux3_0_brst_l2_noerr]

---> Error for flux3 0-degree pitch angle electron flux. [mms3_edi_flux3_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-4 0PA [mms3_edi_flux4_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-4 0PA [mms3_edi_flux4_0_brst_l2_noerr]

---> Error for flux4 0-degree pitch angle electron flux. [mms3_edi_flux4_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-1 180PA [mms3_edi_flux1_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-1 180PA [mms3_edi_flux1_180_brst_l2_noerr]

---> Error for flux1 180-degree pitch angle electron flux. [mms3_edi_flux1_180_delta_brst_l2]

Flux for electrons with trajectories given by traj2 180PA [mms3_edi_flux2_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-2 180PA [mms3_edi_flux2_180_brst_l2_noerr]

---> Error for flux2 180-degree pitch angle electron flux. [mms3_edi_flux2_180_delta_brst_l2]

Flux for electrons with trajectories given by traj3 180PA [mms3_edi_flux3_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-3 180PA [mms3_edi_flux3_180_brst_l2_noerr]

---> Error for flux3 180-degree pitch angle electron flux. [mms3_edi_flux3_180_delta_brst_l2]

Flux for electrons with trajectories given by traj4 180PA [mms3_edi_flux4_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-4 180PA [mms3_edi_flux4_180_brst_l2_noerr]

---> Error for flux4 180-degree pitch angle electron flux. [mms3_edi_flux4_180_delta_brst_l2]

Trajectory of flux1 0-degree pitch angle electrons in GSE coordinates. [mms3_edi_traj1_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 0-degree pitch angle electrons in GSE coordinates. [mms3_edi_traj2_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 0-degree pitch angle electrons in GSE coordinates. [mms3_edi_traj3_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 0-degree pitch angle electrons in GSE coordinates. [mms3_edi_traj4_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 180-degree pitch angle electrons in GSE coordinates. [mms3_edi_traj1_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 180-degree pitch angle electrons in GSE coordinates. [mms3_edi_traj2_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 180-degree pitch angle electrons in GSE coordinates. [mms3_edi_traj3_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 180-degree pitch angle electrons in GSE coordinates. [mms3_edi_traj4_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj1_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 0-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj2_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 0-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj3_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 0-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj4_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj1_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 180-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj2_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 180-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj3_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 180-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj4_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms3_edi_traj1_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms3_edi_traj2_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms3_edi_traj3_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms3_edi_traj4_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms3_edi_traj1_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms3_edi_traj2_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms3_edi_traj3_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms3_edi_traj4_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS3_EDI_BRST_L2_AMB-PM2 (spase://NASA/NumericalData/MMS/3/FIELDS/EDI/Burst/Level2/AmbientElectronFlux/ProjectionMethod2/PT0.0009765625S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v1.0.0 - Original version.
v1.1.0 - Correct fill value for fluxes.
v2.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v3.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.
v4.0.0 - Each trajectory has its own LABL_PTR_1 variable.

Data Variable Descriptions

Optics state [mms3_edi_optics_state_brst_l2]

---> GDU1 energy [mms3_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms3_edi_energy_gdu2_brst_l2]

Field-aligned electron flux from channel 1 of both GDUs [mms3_edi_flux1_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 1 of both GDUs [mms3_edi_flux1_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 1 of both GDUs. [mms3_edi_flux1_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 1 of both GDUs [mms3_edi_flux1_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 1 of both GDUs [mms3_edi_flux1_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 1 of both GDUs. [mms3_edi_flux1_180_delta_brst_l2]

Field-aligned electron flux from channel 2 of both GDUs [mms3_edi_flux2_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 2 of both GDUs [mms3_edi_flux2_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 2 of both GDUs. [mms3_edi_flux2_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 2 of both GDUs [mms3_edi_flux2_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 2 of both GDUs [mms3_edi_flux2_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 2 of both GDUs. [mms3_edi_flux2_180_delta_brst_l2]

Field-aligned electron flux from channel 3 of both GDUs [mms3_edi_flux3_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 3 of both GDUs [mms3_edi_flux3_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 3 of both GDUs. [mms3_edi_flux3_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 3 of both GDUs [mms3_edi_flux3_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 3 of both GDUs [mms3_edi_flux3_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 3 of both GDUs. [mms3_edi_flux3_180_delta_brst_l2]

Field-aligned electron flux from channel 4 of both GDUs [mms3_edi_flux4_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 4 of both GDUs [mms3_edi_flux4_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 4 of both GDUs. [mms3_edi_flux4_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 4 of both GDUs [mms3_edi_flux4_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 4 of both GDUs [mms3_edi_flux4_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 4 of both GDUs. [mms3_edi_flux4_180_delta_brst_l2]

Trajectory of field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms3_edi_traj1_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms3_edi_traj1_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 1 of both GDUs in GSE coordinates. [mms3_edi_traj1_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs, in GSE coordinates. [mms3_edi_traj1_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms3_edi_traj2_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms3_edi_traj2_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in GSE coordinates. [mms3_edi_traj2_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs, in GSE coordinates. [mms3_edi_traj2_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms3_edi_traj3_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms3_edi_traj3_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in GSE coordinates. [mms3_edi_traj3_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs, in GSE coordinates. [mms3_edi_traj3_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms3_edi_traj4_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms3_edi_traj4_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in GSE coordinates. [mms3_edi_traj4_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs, in GSE coordinates. [mms3_edi_traj4_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj1_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj1_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS3_EDI_BRST_L2_EFIELD (spase://NASA/NumericalData/MMS/3/FIELDS/EDI/Burst/Level2/ElectricField/PT0.0009765625S)

Description

EDI electric field data. Instrument papers for EDI can be found at:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7

Modification History

v1.0.0 - First version. TRI-TOF selection based on smallest error.
v1.1.0 - TRI-TOF merged by weighted average.
v1.2.0 - Fixed t_delta_plus/minus CDF_type.
v1.3.0 - Fixed Fixed vdrift SI conversion.
v1.4.0 - Fixed data duplication caused by multiple l2pre file locations.
v1.5.0 - Inplemented baseline*beams*Bmag filter for triangulation.
v1.6.0 - Inplemented null files for no or low quality data.

Data Variable Descriptions

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MMS3_EDI_BRST_L2_Q0 (spase://NASA/NumericalData/MMS/3/FIELDS/EDI/Burst/Level2/QualityZero/PT0.0078125S)

Description

EDI Q0 data. The EDI instrument paper and data products guidescan be found at
the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - First version.
v0.0.1 - Filled energy variables.
v0.0.2 - Energy written properly.
v1.0.0 - Update variable names.
v1.1.0 - Added optics state.
v2.0.0 - Added electron trajectories.
v2.1.0 - Deltas on trajectory vectors are now deltas.
v3.0.0 - Reduced file size with scalar errors. Add VAR_NOTES.
v3.1.0 - Fixed optics datatype.
v4.0.0 - Removed unused Epoch variable.
v5.0.0 - Trajectories are provided in DBCS coordinates.

Data Variable Descriptions

Optics state [mms3_edi_optics_state_brst_l2]

---> GDU1 energy [mms3_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms3_edi_energy_gdu2_brst_l2]

GDU1 quality 0 counts. [mms3_edi_counts_gdu1_brst_l2]

Q0 data consists of raw electron counts. The error at any one time is the
square-root of the counts. Note that there may be contamination from the EDI
electron beams. See the data products guide or contact an EDI team member to
learn about beam contamination.

GDU2 quality 0 counts. [mms3_edi_counts_gdu2_brst_l2]

GDU1 electron incident trajectory vectors in spherical BCS coordinates. [mms3_edi_traj_bcs_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical BCS coordinates. [mms3_edi_traj_bcs_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical DBCS coordinates. [mms3_edi_traj_dbcs_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical DBCS coordinates. [mms3_edi_traj_dbcs_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSE coordinates. [mms3_edi_traj_gse_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSE coordinates. [mms3_edi_traj_gse_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSM coordinates. [mms3_edi_traj_gsm_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSM coordinates. [mms3_edi_traj_gsm_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS3_EDI_SRVY_L2_AMB (spase://NASA/NumericalData/MMS/3/FIELDS/EDI/Survey/Level2/ElectronFluxAmbient/ProjectionMethod1/PT0.03125S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - Original version.
v1.0.0 - Include trajectory vectors and optics state.
v1.1.0 - Update metadata: counts -> flux.
v1.2.0 - Added flux error.
v1.3.0 - Trajectory vector errors are now deltas.
v1.4.0 - Fixed dead-time correction and error values.
v1.5.0 - Factor of 2 for accumulation time & 2 for abscal factor in srvy mode.
v1.6.0 - No factor of 2 for accumulation time in srvy mode.
v2.0.0 - Reduced file size with scalar errors. Update metadata.
v2.1.0 - Correct fill value for fluxes.
v3.0.0 - Omni-directional error for trajectories. Correct time deltas. Y-Version
linked to cal file. Single epoch for counts.
v4.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.

Data Variable Descriptions

Optics state [mms3_edi_optics_state_srvy_l2]

---> GDU1 energy [mms3_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms3_edi_energy_gdu2_srvy_l2]

Field-aligned electron flux from both GDUs [mms3_edi_flux1_0_srvy_l2]

---> (no error bars displayed) Field-aligned electron flux from both GDUs [mms3_edi_flux1_0_srvy_l2_noerr]

---> Error in field-aligned electron flux from both GDUs. [mms3_edi_flux1_0_delta_srvy_l2]

Anti-field-aligned electron flux from both GDUs [mms3_edi_flux1_180_srvy_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from both GDUs [mms3_edi_flux1_180_srvy_l2_noerr]

---> Error in anti-field-aligned electron flux from both GDUs. [mms3_edi_flux1_180_delta_srvy_l2]

Trajectory of field-aligned electrons from both GDUs in DBCS coordinates. [mms3_edi_traj1_dbcs_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs in DBCS coordinates. [mms3_edi_traj1_dbcs_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from both GDUs in GSE coordinates. [mms3_edi_traj1_gse_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs, in GSE coordinates. [mms3_edi_traj1_gse_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj1_gsm_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj1_gsm_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS3_EDI_SRVY_L2_AMB-PM2 (spase://NASA/NumericalData/MMS/3/FIELDS/EDI/Survey/Level2/ElectronFluxAmbient/ProjectionMethod2/PT0.03125S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v1.0.0 - Original version.
v1.1.0 - Correct fill value for fluxes.
v2.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v3.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.
v4.0.0 - Each trajectory has its own LABL_PTR_1 variable.

Data Variable Descriptions

Optics state [mms3_edi_optics_state_srvy_l2]

---> GDU1 energy [mms3_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms3_edi_energy_gdu2_srvy_l2]

Field-aligned electron flux from both GDUs [mms3_edi_flux1_0_srvy_l2]

---> (no error bars displayed) Field-aligned electron flux from both GDUs [mms3_edi_flux1_0_srvy_l2_noerr]

---> Error in field-aligned electron flux from both GDUs. [mms3_edi_flux1_0_delta_srvy_l2]

Anti-field-aligned electron flux from both GDUs [mms3_edi_flux1_180_srvy_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from both GDUs [mms3_edi_flux1_180_srvy_l2_noerr]

---> Error in anti-field-aligned electron flux from both GDUs. [mms3_edi_flux1_180_delta_srvy_l2]

Trajectory of field-aligned electrons from both GDUs in DBCS coordinates. [mms3_edi_traj1_dbcs_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs in DBCS coordinates. [mms3_edi_traj1_dbcs_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from both GDUs in GSE coordinates. [mms3_edi_traj1_gse_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs, in GSE coordinates. [mms3_edi_traj1_gse_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj1_gsm_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms3_edi_traj1_gsm_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS3_EDI_SRVY_L2_EFIELD (spase://NASA/NumericalData/MMS/3/FIELDS/EDI/Survey/Level2/ElectricField/PT5S)

Description

EDI electric field data. Instrument papers for EDI can be found at:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7

Modification History

v1.0.0 - First version. TRI-TOF selection based on smallest error.
v1.1.0 - TRI-TOF merged by weighted average.
v1.2.0 - Fixed t_delta_plus/minus CDF_type.
v1.3.0 - Fixed Fixed vdrift SI conversion.
v1.4.0 - Fixed data duplication caused by multiple l2pre file locations.
v1.5.0 - Inplemented baseline*beams*Bmag filter for triangulation.
v1.6.0 - Inplemented null files for no or low quality data.

Data Variable Descriptions

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MMS3_EDI_SRVY_L2_Q0 (spase://NASA/NumericalData/MMS/3/FIELDS/EDI/Survey/Level2/QualityZero/PT0.125S)

Description

EDI Q0 data. The EDI instrument paper and data products guidescan be found at
the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - First version.
v0.0.1 - Filled energy variables.
v0.0.2 - Energy written properly.
v1.0.0 - Update variable names.
v1.1.0 - Added optics state.
v2.0.0 - Added electron trajectories.
v2.1.0 - Deltas on trajectory vectors are now deltas.
v3.0.0 - Reduced file size with scalar errors. Add VAR_NOTES.
v4.0.0 - Removed unused Epoch variable.
v5.0.0 - Trajectories are provided in DBCS coordinates.

Data Variable Descriptions

Optics state [mms3_edi_optics_state_srvy_l2]

---> GDU1 energy [mms3_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms3_edi_energy_gdu2_srvy_l2]

GDU1 quality 0 counts. [mms3_edi_counts_gdu1_srvy_l2]

Q0 data consists of raw electron counts. The error at any one time is the
square-root of the counts. Note that there may be contamination from the EDI
electron beams. See the data products guide or contact an EDI team member to
learn about beam contamination.

GDU2 quality 0 counts. [mms3_edi_counts_gdu2_srvy_l2]

GDU1 electron incident trajectory vectors in spherical BCS coordinates. [mms3_edi_traj_bcs_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical BCS coordinates. [mms3_edi_traj_bcs_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical DBCS coordinates. [mms3_edi_traj_dbcs_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical DBCS coordinates. [mms3_edi_traj_dbcs_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSE coordinates. [mms3_edi_traj_gse_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSE coordinates. [mms3_edi_traj_gse_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSM coordinates. [mms3_edi_traj_gsm_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSM coordinates. [mms3_edi_traj_gsm_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS3_EDP_BRST_L2_DCE (spase://NASA/NumericalData/MMS/3/FIELDS/EDP/Burst/Level2/DCElectricField/PT0.0001220703125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS3_EDP_BRST_L2_HMFE (spase://NASA/NumericalData/MMS/3/FIELDS/EDP/Burst/Level2Pre/HMFE/PT0.00001525878906S)

Description

Data Variable Descriptions

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MMS3_EDP_BRST_L2_SCPOT doi:10.48322/x3td-gh63
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

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MMS3_EDP_FAST_L2_DCE (spase://NASA/NumericalData/MMS/3/FIELDS/EDP/Fast/Level2/DCElectricField/PT0.03125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS3_EDP_FAST_L2_SCPOT doi:10.48322/kzh6-vf67
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

Data Variable Descriptions

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MMS3_EDP_SLOW_L2_DCE (spase://NASA/NumericalData/MMS/3/FIELDS/EDP/Slow/Level2/DCElectricField/PT0.125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS3_EDP_SLOW_L2_SCPOT doi:10.48322/5vc4-ys82
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

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MMS3_EDP_SRVY_L2_HFESP (spase://NASA/NumericalData/MMS/3/FIELDS/EDP/Survey/Level2/HighFrequencyElectricFieldSpectra/PT16S)

Description

 AC Electric Field

Data Variable Descriptions

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MMS3_EPD-EIS_BRST_L2_EXTOF (spase://NASA/NumericalData/MMS/3/EnergeticParticleDetector/EIS/Burst/Level2/EnergyByTimeOfFlight/PT0.605S)

Description

empty

Modification History

Constantly modifying this code

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MMS3_EPD-EIS_BRST_L2_PHXTOF (spase://NASA/NumericalData/MMS/3/EnergeticParticleDetector/EIS/Burst/Level2/PulseHeightByTimeOfFlight/PT0.605S)

Description

empty

Modification History

Constantly modifying this code

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MMS3_EPD-EIS_SRVY_L2_ELECTRONENERGY (spase://NASA/NumericalData/MMS/3/EnergeticParticleDetector/EIS/Survey/Level2/ElectronEnergySpectra/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS3_EPD-EIS_SRVY_L2_EXTOF (spase://NASA/NumericalData/MMS/3/EnergeticParticleDetector/EIS/Survey/Level2/EnergyByTimeOfFlight/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS3_EPD-EIS_SRVY_L2_PHXTOF (spase://NASA/NumericalData/MMS/3/EnergeticParticleDetector/EIS/Survey/Level2/PulseHeightByTimeOfFlight/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS3_FEEPS_BRST_L2_ELECTRON (spase://NASA/NumericalData/MMS/3/EnergeticParticleDetector/FEEPS/Burst/Level2/Electron/PT0.3025S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS3_FEEPS_BRST_L2_ION (spase://NASA/NumericalData/MMS/3/EnergeticParticleDetector/FEEPS/Burst/Level2/Ion/PT0.3025S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS3_FEEPS_SRVY_L2_ELECTRON (spase://NASA/NumericalData/MMS/3/EnergeticParticleDetector/FEEPS/Survey/Level2/Electron/PT2.42S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS3_FEEPS_SRVY_L2_ION (spase://NASA/NumericalData/MMS/3/EnergeticParticleDetector/FEEPS/Survey/Level2/Ion/PT2.42S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS3_FGM_BRST_L2 (spase://NASA/NumericalData/MMS/3/FIELDS/FGM/Burst/Level2/PT0.0078125S)

Description

The Fluxgate Magnetometers (FGM) on Magnetospheric Multiscale consist of a
traditional Analog Fluxgate Magnetometer (AFG), and a Digital Fluxgate
magnetometer (DFG). The dual magnetometers are operated as a single instrument
providing a single intercalibrated data product. Range changes occur at
different times on the two instruments so the gains checked each periapsis can
be carried out unambiguously to apoapsis. Cross correlation of calibration
parameters can separate causes of the any apparent calibration changes. Use of
Electron Drift Instrument (EDI) to determine the field along the rotation axis
allows accurate monitoring of the zero levels along the rotation axis.  Prior to
launch the magnetometers were calibrated at the Technical University,
Braunschweig, except for the AFG magnetometers on MMS3 and MMS4, which were
calibrated at UCLA.  Both sets of sensors are operated for the entire MMS orbit,
with slow survey (8 samples per second) outside of the Region of Interest (ROI),
and fast survey (16 samples per second) inside the ROI. Within the ROI burst
mode data (128 samples per second) are also acquired.  A detailed description of
the MMS fluxgate magnetometers, including science objectives, instrument
description, calibration, magnetic cleanliness program, and data flow can be
found at http://link.springer.com/article/10.1007%2Fs11214-014-0057-3 (DOI 
10.1007/s11214-014-0057-3).Additional information can also be found at
http://www-spc.igpp.ucla.edu/ssc/mms (UCLA),and http://www.iwf.oeaw.ac.at (IWF,
Graz).
For the purpose of creating a unified FGM Level2 data product, burst mode data
is taken from DFG and survey mode data is taken from AFG.  Because AFG and DFG
are cross-calibrated on an orbit-averaged basis, small differences in offset may
be observed between Level2 burst and survey mode data.  Consequently, any
differences are within the error of the measurement. Based on preliminary
analysis of the data, the absolute error within the Region of Interest (ROI) is
estimated to be no more than 0.1 nT in the spin-plane, 0.15 nT along the
spin-axis and 0.2 nT in total magnitude.

Modification History

version X=5:  * Y-version number comes from cal file entries. 
              *
Ensures there are 2 ephemeris points before/after data to enable proper spline. 

              * Fix to depend_0 of rdeltahalf:  fixes bug when reading position
data.
              * L-vector for DMPA2GSE transformation is smoothed with a
gaussian filter, instead 
                of using a single average value for
the day.  This short-term filter avoids  
                introduding artificial
jumps at 00:00 UTC and removes 7-minute 'wobble' after  
               
maneuvers in the GSE result.   
              * Fixes error with DEFATT file
selection found when choosing the 
                daily DEFATT files to be used
in Phase 2.
              * Fixed bug where reference Etemp was used for high
range gain.  Now uses measured Etemp.
version X=4:  First version for public
release of L2.
              Renamed variables to conform with new MMS variable
name guidelines 
              (obs_instr_paramName[_coordSys]_mode_level):  
  
             Mag field parameters include 'b' for paramName.  
               
Use 'r' instead of 'pos' for S/C position paramName.  
               
Eliminated 'rate', replaced with 'bdeltahalf'.  Added 'rdeltahalf'.
            
   l1a_mode is now just 'mode'.
version X=3:  fixed removal of overlap between
modes.
              fixed a bug that caused stemp and etemp to be
empty.
version X=2:  flag parameter name corrected: was 'status'
               
        added bits 4, 5, 6 to flag saturation on B1, B2, and B3, respectively
  
                     added bit 7 to flag bad data at range changes
             
Added etemp and l1a_mode parameters.  
              rate, hirange, and stemp
parameters now comply with MMS CDF Guidlelines, e.g.
              FILLVAL now
defined for stemp and etemp, and is set to !values.f_nan
              No longer
use Var_Parents attribute in stemp -- see Parents instead
              In this
version, temperature-corrected gains are applied.  Reference temperatures are
used when 
              stemp or etemp are set to FILLVAL. 
             
Non-linearity correction is applied to high rage DFG data.
version X=1:  added
'flag', rate and hirange parameters (but 'flag' is actually called 'status')

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MMS3_FGM_SRVY_L2 (spase://NASA/NumericalData/MMS/3/FIELDS/FGM/Survey/Level2/PT0.125S)

Description

The Fluxgate Magnetometers (FGM) on Magnetospheric Multiscale consist of a
traditional Analog Fluxgate Magnetometer (AFG), and a Digital Fluxgate
magnetometer (DFG). The dual magnetometers are operated as a single instrument
providing a single intercalibrated data product. Range changes occur at
different times on the two instruments so the gains checked each periapsis can
be carried out unambiguously to apoapsis. Cross correlation of calibration
parameters can separate causes of the any apparent calibration changes. Use of
Electron Drift Instrument (EDI) to determine the field along the rotation axis
allows accurate monitoring of the zero levels along the rotation axis.  Prior to
launch the magnetometers were calibrated at the Technical University,
Braunschweig, except for the AFG magnetometers on MMS3 and MMS4, which were
calibrated at UCLA.  Both sets of sensors are operated for the entire MMS orbit,
with slow survey (8 samples per second) outside of the Region of Interest (ROI),
and fast survey (16 samples per second) inside the ROI. Within the ROI burst
mode data (128 samples per second) are also acquired.  A detailed description of
the MMS fluxgate magnetometers, including science objectives, instrument
description, calibration, magnetic cleanliness program, and data flow can be
found at http://link.springer.com/article/10.1007%2Fs11214-014-0057-3 (DOI 
10.1007/s11214-014-0057-3).Additional information can also be found at
http://www-spc.igpp.ucla.edu/ssc/mms (UCLA),and http://www.iwf.oeaw.ac.at (IWF,
Graz).
For the purpose of creating a unified FGM Level2 data product, burst mode data
is taken from DFG and survey mode data is taken from AFG.  Because AFG and DFG
are cross-calibrated on an orbit-averaged basis, small differences in offset may
be observed between Level2 burst and survey mode data.  Consequently, any
differences are within the error of the measurement. Based on preliminary
analysis of the data, the absolute error within the Region of Interest (ROI) is
estimated to be no more than 0.1 nT in the spin-plane, 0.15 nT along the
spin-axis and 0.2 nT in total magnitude.

Modification History

version X=5:  * Y-version number comes from cal file entries. 
              *
Ensures there are 2 ephemeris points before/after data to enable proper spline. 

              * Fix to depend_0 of rdeltahalf:  fixes bug when reading position
data.
              * L-vector for DMPA2GSE transformation is smoothed with a
gaussian filter, instead 
                of using a single average value for
the day.  This short-term filter avoids  
                introduding artificial
jumps at 00:00 UTC and removes 7-minute 'wobble' after  
               
maneuvers in the GSE result.   
              * Fixes error with DEFATT file
selection found when choosing the 
                daily DEFATT files to be used
in Phase 2.
              * Fixed bug where reference Etemp was used for high
range gain.  Now uses measured Etemp.
version X=4:  First version for public
release of L2.
              Renamed variables to conform with new MMS variable
name guidelines 
              (obs_instr_paramName[_coordSys]_mode_level):  
  
             Mag field parameters include 'b' for paramName.  
               
Use 'r' instead of 'pos' for S/C position paramName.  
               
Eliminated 'rate', replaced with 'bdeltahalf'.  Added 'rdeltahalf'.
            
   l1a_mode is now just 'mode'.
version X=3:  fixed removal of overlap between
modes.
              fixed a bug that caused stemp and etemp to be
empty.
version X=2:  flag parameter name corrected: was 'status'
               
        added bits 4, 5, 6 to flag saturation on B1, B2, and B3, respectively
  
                     added bit 7 to flag bad data at range changes
             
Added etemp and l1a_mode parameters.  
              rate, hirange, and stemp
parameters now comply with MMS CDF Guidlelines, e.g.
              FILLVAL now
defined for stemp and etemp, and is set to !values.f_nan
              No longer
use Var_Parents attribute in stemp -- see Parents instead
              In this
version, temperature-corrected gains are applied.  Reference temperatures are
used when 
              stemp or etemp are set to FILLVAL. 
             
Non-linearity correction is applied to high rage DFG data.
version X=1:  added
'flag', rate and hirange parameters (but 'flag' is actually called 'status')

Data Variable Descriptions

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MMS3_FPI_BRST_L2_DES-DIST (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DES/Burst/Level2/Distribution/PT0.03S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data are taken at burst (30/150 ms for DES/DIS)
resolution in this mode.  Data are also made available at survey (4.5 s, etc)
resolution; these form a separate product from this.  Per mission design, not
all burst-resolution data are downlinked.  This product contains phase-space
distribution maps of those burst-resolution data selected for downlink.  In
particular, the (highest possible quality at the time of release)
corrected/converted "Burst SkyMap" distributions are reported with time-stamps
and other annotation characterizing the state of the instrument system at the
indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

[CDAWeb List/Download/Create ONLY] MMS3 FPI/DES burst sky-map instrument distribution [mms3_des_dist_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 10.9 eV (E1/even) [mms3_des_dist_brst1_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 12.4 eV (E1/odd) [mms3_des_dist_brst1_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~11.6 eV (E1 even-odd) [mms3_des_dist_brst1_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 10.9 eV (E1/even) [mms3_des_dist_brst1_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 12.4 eV (E1/odd) [mms3_des_dist_brst1_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 37.9 eV (E6/even) [mms3_des_dist_brst6_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 42.9 eV (E6/odd) [mms3_des_dist_brst6_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~40.4 eV (E6 even-odd) [mms3_des_dist_brst6_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 37.9 eV (E6/even) [mms3_des_dist_brst6_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 42.9 eV (E6/odd) [mms3_des_dist_brst6_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 80.0 eV (E9/even) [mms3_des_dist_brst9_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 90.6 eV (E9/odd) [mms3_des_dist_brst9_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~85 eV (E9 even-odd) [mms3_des_dist_brst9_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 80.0 eV (E9/even) [mms3_des_dist_brst9_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 90.6 eV (E9/odd) [mms3_des_dist_brst9_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 169 eV (E12/even) [mms3_des_dist_brst12_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 191 eV (E12/odd) [mms3_des_dist_brst12_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~180 eV (E12 even-odd) [mms3_des_dist_brst12_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 169 eV (E12/even) [mms3_des_dist_brst12_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 191 eV (E12/odd) [mms3_des_dist_brst12_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 277 eV (E14/even) [mms3_des_dist_brst14_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 314 eV (E14/odd) [mms3_des_dist_brst14_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~295 eV (E14 even-odd) [mms3_des_dist_brst14_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 277 eV (E14/even) [mms3_des_dist_brst14_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 314 eV (E14/odd) [mms3_des_dist_brst14_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 456 eV (E16/even) [mms3_des_dist_brst16_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 517 eV (E16/odd) [mms3_des_dist_brst16_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~485 eV (E16 even-odd) [mms3_des_dist_brst16_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 456 eV (E16/even) [mms3_des_dist_brst16_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 517 eV (E16/odd) [mms3_des_dist_brst16_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 750 eV (E18/even) [mms3_des_dist_brst18_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 850 eV (E18/odd) [mms3_des_dist_brst18_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~800 eV (E18 even-odd) [mms3_des_dist_brst18_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 750 eV (E18/even) [mms3_des_dist_brst18_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 850 eV (E18/odd) [mms3_des_dist_brst18_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 1230 eV (E20/even) [mms3_des_dist_brst20_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 1400 eV (E20/odd) [mms3_des_dist_brst20_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~1310 eV (E20 even-odd) [mms3_des_dist_brst20_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1230 eV (E20/even) [mms3_des_dist_brst20_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1400 eV (E20/odd) [mms3_des_dist_brst20_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 2600 eV (E23/even) [mms3_des_dist_brst23_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 2950 eV (E23/odd) [mms3_des_dist_brst23_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~2770 eV (E23 even-odd) [mms3_des_dist_brst23_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2600 eV (E23/even) [mms3_des_dist_brst23_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2950 eV (E23/odd) [mms3_des_dist_brst23_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 5490 eV (E26/even) [mms3_des_dist_brst26_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 6210 eV (E26/odd) [mms3_des_dist_brst26_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~5840 eV (E26 even-odd) [mms3_des_dist_brst26_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5490 eV (E26/even) [mms3_des_dist_brst26_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 6210 eV (E26/odd) [mms3_des_dist_brst26_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 24400 eV (E32/even) [mms3_des_dist_brst32_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES burst sky-map instrument distribution - 27600 eV (E32/odd) [mms3_des_dist_brst32_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~26000 eV (E32 even-odd) [mms3_des_dist_brst32_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 24400 eV (E32/even) [mms3_des_dist_brst32_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 27600 eV (E32/odd) [mms3_des_dist_brst32_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[List/Create only in CDAWeb] 1-sigma error: MMS3 FPI/DES burst sky-map instrument distribution [mms3_des_disterr_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES vector of data-quality indicators at burst-start time [mms3_des_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS3 FPI/DES compression lossless/lossy indicator at survey-start time [mms3_des_compressionloss_brst]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

---> MMS3 FPI/DES step table parity, this burst [mms3_des_steptable_parity_brst]

FPI/DES alternates between two tables, designated "even" (0) and "odd" (1).

---> MMS3 FPI/DES Del-Phi (obs spin-phase) count at burst-start time [mms3_des_startdelphi_count_brst]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS3 FPI/DES Del-Phi (obs spin-phase) angle at burst-start time [mms3_des_startdelphi_angle_brst]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS3 FPI/DES burst average f1 count values [mms3_des_avgf1counts_brst]

Average f1-count level as a function of energy

MMS3 FPI/DES burst sky-map microsecond offsets from Epoch [mms3_des_steptimeoffsets_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order. Offsets reflect 128 steps over the 30 msec sweep
period. See FPI docs for details.

---> MMS3 FPI/DES sector de-Spin P value, this burst [mms3_des_sector_despinp_brst]

Records P-value used to de-spin this burst sky-map on board.  See FPI docs for
details.

MMS3 FPI/DES burst sky-map instrument azimuthal angles [mms3_des_phi_brst]

see FPI docs for details

MMS FPI/DES burst sky-map parity 0/1 energies [mms3_des_energy_brst]

Energies (parity 0/1) in the 64-step FPI energy table

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MMS3_FPI_BRST_L2_DES-MOMS (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DES/Burst/Level2/Moments/PT0.03S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode.  Data are also made available at survey (4.5
s, etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked.  Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available.  This product contains results from
integrating the standard moments of phase-space distributions formed from the
indicated data type (DES/DIS burst, FS or SS).  For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS3_FPI_BRST_L2_DES-PARTMOMS (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DES/Burst/Level2/PartialMoments/PT0.03S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s,
etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked. Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available. This product contains partial moments that
come from performing the standard moment integrals over a limited portion of
velocity space. The resulting quantities are named similarly to their
corresponding standard moments, but are decorated with 'part' to differentiate.
For example, density_part is the density moment integrated from a particular
energy step to infinity. These partial moments are formed from the indicated
data type (DES/DIS burst, FS or SS). For convenience, some additional parameters
are included to augment those most commonly found in a moments product of this
sort, plus time-stamps and other annotation characterizing the state of the
instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DES vector of data-quality indicators at burst-start time [mms3_des_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of brst l2pre
magnetic field, Bit-9 = srvy l2pre magnetic field used instead of brst l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS3 FPI/DES partial electron number density during this burst [mms3_des_numberdensity_part_brst]

MMS3 FPI/DES partial electron bulk-velocity vector in DBCS during this burst [mms3_des_bulkv_part_dbcs_brst]

MMS3 FPI/DES partial electron bulk-velocity vector in GSE during this burst [mms3_des_bulkv_part_gse_brst]

MMS3 FPI/DES partial electron pressure tensor in DBCS during this burst [mms3_des_prestensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES partial electron pressure tensor in GSE during this burst [mms3_des_prestensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES partial electron temperature tensor in DBCS during this burst [mms3_des_temptensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES partial electron temperature tensor in GSE during this burst [mms3_des_temptensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES partial electron parallel temperature during this burst [mms3_des_temppara_part_brst]

MMS3 FPI/DES partial electron perpendicular temperature during this burst [mms3_des_tempperp_part_brst]

MMS3 FPI/DES recommended energy index during this burst [mms3_des_part_index_brst]

Recommended energy index during this burst

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MMS3_FPI_BRST_L2_DIS-DIST (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DIS/Burst/Level2/Distribution/PT0.15S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data are taken at burst (30/150 ms for DES/DIS)
resolution in this mode.  Data are also made available at survey (4.5 s, etc)
resolution; these form a separate product from this.  Per mission design, not
all burst-resolution data are downlinked.  This product contains phase-space
distribution maps of those burst-resolution data selected for downlink.  In
particular, the (highest possible quality at the time of release)
corrected/converted "Burst SkyMap" distributions are reported with time-stamps
and other annotation characterizing the state of the instrument system at the
indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

[CDAWeb List/Download/Create ONLY] MMS3 FPI/DIS burst sky-map instrument distribution [mms3_dis_dist_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 10.6 eV (E1/even) [mms3_dis_dist_brst1_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 12.0 eV (E1/odd) [mms3_dis_dist_brst1_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~11.3 eV (E1 even-odd) [mms3_dis_dist_brst1_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 10.6 eV (E1/even) [mms3_dis_dist_brst1_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 12.0 eV (E1/odd) [mms3_dis_dist_brst1_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 37.2 eV (E6/even) [mms3_dis_dist_brst6_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 42.1 eV (E6/odd) [mms3_dis_dist_brst6_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~39.6 eV (E6 even-odd) [mms3_dis_dist_brst6_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 37.2 eV (E6/even) [mms3_dis_dist_brst6_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 42.1 eV (E6/odd) [mms3_dis_dist_brst6_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 78.8 eV (E9/even) [mms3_dis_dist_brst9_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 89.3 eV (E9/odd) [mms3_dis_dist_brst9_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~83.9 eV (E9 even-odd) [mms3_dis_dist_brst9_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 78.8 eV (E9/even) [mms3_dis_dist_brst9_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 89.3 eV (E9/odd) [mms3_dis_dist_brst9_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 167 eV (E12/even) [mms3_dis_dist_brst12_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 189 eV (E12/odd) [mms3_dis_dist_brst12_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~178 eV (E12 even-odd) [mms3_dis_dist_brst12_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 167 eV (E12/even) [mms3_dis_dist_brst12_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 189 eV (E12/odd) [mms3_dis_dist_brst12_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 275 eV (E14/even) [mms3_dis_dist_brst14_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 312 eV (E14/odd) [mms3_dis_dist_brst14_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~293 eV (E14 even-odd) [mms3_dis_dist_brst14_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 275 eV (E14/even) [mms3_dis_dist_brst14_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 312 eV (E14/odd) [mms3_dis_dist_brst14_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 455 eV (E16/even) [mms3_dis_dist_brst16_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 515 eV (E16/odd) [mms3_dis_dist_brst16_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~484 eV (E16 even-odd) [mms3_dis_dist_brst16_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 455 eV (E16/even) [mms3_dis_dist_brst16_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 515 eV (E16/odd) [mms3_dis_dist_brst16_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 750 eV (E18/even) [mms3_dis_dist_brst18_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 850 eV (E18/odd) [mms3_dis_dist_brst18_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~800 eV (E18 even-odd) [mms3_dis_dist_brst18_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 750 eV (E18/even) [mms3_dis_dist_brst18_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 850 eV (E18/odd) [mms3_dis_dist_brst18_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 1240 eV (E20/even) [mms3_dis_dist_brst20_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 1400 eV (E20/odd) [mms3_dis_dist_brst20_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~1320 eV (E20 even-odd) [mms3_dis_dist_brst20_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1240 eV (E20/even) [mms3_dis_dist_brst20_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1400 eV (E20/odd) [mms3_dis_dist_brst20_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 2620 eV (E23/even) [mms3_dis_dist_brst23_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 2970 eV (E23/odd) [mms3_dis_dist_brst23_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~2800 eV (E23 even-odd) [mms3_dis_dist_brst23_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2620 eV (E23/even) [mms3_dis_dist_brst23_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2970 eV (E23/odd) [mms3_dis_dist_brst23_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 5560 eV (E26/even) [mms3_dis_dist_brst26_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 6300 eV (E26/odd) [mms3_dis_dist_brst26_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~5920 eV (E26 even-odd) [mms3_dis_dist_brst26_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5560 eV (E26/even) [mms3_dis_dist_brst26_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 6300 eV (E26/odd) [mms3_dis_dist_brst26_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 25000 eV (E32/even) [mms3_dis_dist_brst32_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS burst sky-map instrument distribution - 28300 eV (E32/odd) [mms3_dis_dist_brst32_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~26600 eV (E32 even-odd) [mms3_dis_dist_brst32_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 25000 eV (E32/even) [mms3_dis_dist_brst32_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 28300 eV (E32/odd) [mms3_dis_dist_brst32_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[List/Create only in CDAWeb] 1-sigma error: MMS3 FPI/DIS burst sky-map instrument distribution [mms3_dis_disterr_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS vector of data-quality indicators at burst-start time [mms3_dis_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS3 FPI/DIS compression lossless/lossy indicator at survey-start time [mms3_dis_compressionloss_brst]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

---> MMS3 FPI/DIS step table parity, this burst [mms3_dis_steptable_parity_brst]

FPI/DIS alternates between two tables, designated "even" (0) and "odd" (1).

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) count at burst-start time [mms3_dis_startdelphi_count_brst]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at burst-start time [mms3_dis_startdelphi_angle_brst]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS3 FPI/DIS burst average f1 count values [mms3_dis_avgf1counts_brst]

Average f1-count level as a function of energy

MMS3 FPI/DIS burst sky-map microsecond offsets from Epoch [mms3_dis_steptimeoffsets_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order. Offsets reflect 128 steps over the 150 msec sweep
period. See FPI docs for details.

---> MMS3 FPI/DIS sector de-Spin P value, this burst [mms3_dis_sector_despinp_brst]

Records P-value used to de-spin this burst sky-map on board.  See FPI docs for
details.

MMS3 FPI/DIS burst sky-map instrument azimuthal angles [mms3_dis_phi_brst]

see FPI docs for details

MMS FPI/DIS burst sky-map parity 0/1 energies [mms3_dis_energy_brst]

Energies (parity 0/1) in the 64-step FPI energy table

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MMS3_FPI_BRST_L2_DIS-MOMS (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DIS/Burst/Level2/Moments/PT0.15S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode.  Data are also made available at survey (4.5
s, etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked.  Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available.  This product contains results from
integrating the standard moments of phase-space distributions formed from the
indicated data type (DES/DIS burst, FS or SS).  For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS3_FPI_BRST_L2_DIS-PARTMOMS (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DIS/Burst/Level2/PartialMoments/PT0.15S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s,
etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked. Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available. This product contains partial moments that
come from performing the standard moment integrals over a limited portion of
velocity space. The resulting quantities are named similarly to their
corresponding standard moments, but are decorated with 'part' to differentiate.
For example, density_part is the density moment integrated from a particular
energy step to infinity. These partial moments are formed from the indicated
data type (DES/DIS burst, FS or SS). For convenience, some additional parameters
are included to augment those most commonly found in a moments product of this
sort, plus time-stamps and other annotation characterizing the state of the
instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DIS vector of data-quality indicators at burst-start time [mms3_dis_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of brst l2pre
magnetic field, Bit-9 = srvy l2pre magnetic field used instead of brst l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS3 FPI/DIS partial ion number density during this burst [mms3_dis_numberdensity_part_brst]

MMS3 FPI/DIS partial ion bulk-velocity vector in DBCS during this burst [mms3_dis_bulkv_part_dbcs_brst]

MMS3 FPI/DIS partial ion bulk-velocity vector in GSE during this burst [mms3_dis_bulkv_part_gse_brst]

MMS3 FPI/DIS partial ion pressure tensor in DBCS during this burst [mms3_dis_prestensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS partial ion pressure tensor in GSE during this burst [mms3_dis_prestensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS partial ion temperature tensor in DBCS during this burst [mms3_dis_temptensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS partial ion temperature tensor in GSE during this burst [mms3_dis_temptensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS partial ion parallel temperature during this burst [mms3_dis_temppara_part_brst]

MMS3 FPI/DIS partial ion perpendicular temperature during this burst [mms3_dis_tempperp_part_brst]

MMS3 FPI/DIS recommended energy index during this burst [mms3_dis_part_index_brst]

Recommended energy index during this burst

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MMS3_FPI_FAST_L2_DES-DIST (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DES/Fast/Level2/Distribution/PT4.5S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data taken at burst (30/150 ms for DES/DIS)
resolution are aggregated on board and made available at survey (4.5 s)
resolution in this mode.  This product contains phase-space distribution maps of
results from surveying the high-resolution observations during each 4.5 s
period.  In particular, the (highest possible quality at the time of release)
corrected/converted "Fast Survey SkyMap" distributions are reported with
time-stamps and other annotation characterizing the state of the instrument
system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DES fast sky-map instrument distribution - 11.6 eV (E1) using averaged even/odd steps [mms3_des_dist_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 11.6 eV [mms3_des_dist_fast1_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES fast sky-map instrument distribution - 40.4 eV (E6) using averaged even/odd steps [mms3_des_dist_fast6]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 40.4 eV [mms3_des_dist_fast6_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES fast sky-map instrument distribution - 85.1 eV (E9) using averaged even/odd steps [mms3_des_dist_fast9]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 85.1 eV [mms3_des_dist_fast9_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES fast sky-map instrument distribution - 179 eV (E12) using averaged even/odd steps [mms3_des_dist_fast12]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 179 eV [mms3_des_dist_fast12_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES fast sky-map instrument distribution - 295 eV (E14) using averaged even/odd steps [mms3_des_dist_fast14]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 295 eV [mms3_des_dist_fast14_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES fast sky-map instrument distribution - 485 eV (E16) using averaged even/odd steps [mms3_des_dist_fast16]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 485 eV [mms3_des_dist_fast16_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES fast sky-map instrument distribution - 798 eV (E18) using averaged even/odd steps [mms3_des_dist_fast18]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 798 eV [mms3_des_dist_fast18_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES fast sky-map instrument distribution - 1310 eV (E20) using averaged even/odd steps [mms3_des_dist_fast20]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1310 eV [mms3_des_dist_fast20_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES fast sky-map instrument distribution - 2770 eV (E23) using averaged even/odd steps [mms3_des_dist_fast23]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2770 eV [mms3_des_dist_fast23_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES fast sky-map instrument distribution - 5840 eV (E26) using averaged even/odd steps [mms3_des_dist_fast26]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5840 eV [mms3_des_dist_fast26_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES fast sky-map instrument distribution - 26000 eV (E32) using averaged even/odd steps [mms3_des_dist_fast32]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 26000 eV [mms3_des_dist_fast32_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[Only List/Create in CDAWeb] MMS3 FPI/DES fast sky-map instrument distribution 1-sigma error [mms3_des_disterr_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES vector of data-quality indicators at fast survey-start time - 32-bit error flags [mms3_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS3 FPI/DES compression lossless/lossy indicator at survey-start time [mms3_des_compressionloss_fast]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

---> MMS3 FPI/DES Del-Phi (obs spin-phase) count at fast survey-start time [mms3_des_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS3 FPI/DES Del-Phi (obs spin-phase) angle at fast survey-start time [mms3_des_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS3 FPI/DES fast survey average f1 count values [mms3_des_avgf1counts_fast]

Average f1-count level as a function of energy

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MMS3_FPI_FAST_L2_DES-MOMS (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DES/Fast/Level2/Moments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution.  Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This moments product
contains results from integrating the standard moments of phase-space
distributions formed from the indicated data type (DES/DIS burst, FS or SS). For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotation characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS3_FPI_FAST_L2_DES-MOMSAUX

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DES vector of data-quality indicators at survey-start time [mms3_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS3 FPI/DES partial electron number density during this survey [mms3_des_numberdensity_part_fast]

MMS3 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms3_des_bulkv_part_dbcs_fast]

MMS3 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms3_des_bulkv_part_gse_fast]

MMS3 FPI/DES partial electron pressure tensor in DBCS during this survey [mms3_des_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES partial electron pressure tensor in GSE during this survey [mms3_des_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES partial electron temperature tensor in DBCS during this survey [mms3_des_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES partial electron temperature tensor in GSE during this survey [mms3_des_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES partial electron parallel temperature during this survey [mms3_des_temppara_part_fast]

MMS3 FPI/DES partial electron perpendicular temperature during this survey [mms3_des_tempperp_part_fast]

MMS3 FPI/DES recommended energy index for partial moments during this survey [mms3_des_part_index_fast]

Recommended energy index during this survey

MMS3 FPI/DES compression lossless/lossy indicator at survey-start time [mms3_des_compressionloss_fast]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS3 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms3_des_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS3 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms3_des_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS3 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms3_des_pitchangdist_lowen_fast]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size: 6
deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS3 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms3_des_pitchangdist_miden_fast]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS3 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms3_des_pitchangdist_highen_fast]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS3 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms3_des_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS3 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms3_des_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS3 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms3_des_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS3 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms3_des_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS3 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms3_des_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS3 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms3_des_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS3 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms3_des_energyspectr_par_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS3 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms3_des_energyspectr_anti_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS3 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms3_des_energyspectr_perp_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS3 FPI/DES omni-directional electron energy spectrum during this survey [mms3_des_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS3 FPI/DES electron number density during this survey [mms3_des_numberdensity_fast]

MMS3 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms3_des_densityextrapolation_low_fast]

MMS3 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms3_des_densityextrapolation_high_fast]

MMS3 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms3_des_bulkv_dbcs_fast]

MMS3 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this survey [mms3_des_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS3 FPI/DES electron bulk-velocity vector in GSE during this survey [mms3_des_bulkv_gse_fast]

MMS3 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this survey [mms3_des_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS3 FPI/DES electron pressure tensor in DBCS during this survey [mms3_des_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES electron pressure tensor in GSE during this survey [mms3_des_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES electron temperature tensor in DBCS during this survey [mms3_des_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES electron temperature tensor in GSE during this survey [mms3_des_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES electron heat-flux vector in DBCS during this survey [mms3_des_heatq_dbcs_fast]

MMS3 FPI/DES electron heat-flux vector in GSE during this survey [mms3_des_heatq_gse_fast]

MMS3 FPI/DES electron parallel temperature during this BP [mms3_des_temppara_fast]

MMS3 FPI/DES electron perpendicular temperature during this BP [mms3_des_tempperp_fast]

MMS3 FPI/DES S/C potential mean [mms3_des_scpot_mean_fast]

Average spacecraft potential during this FP used to shift the measure energies.

MMS3 FPI/DES S/C potential max [mms3_des_scpot_max_fast]

Maximum spacecraft potential during this FP used to exclude energies containing
spacecraft photoelectron fluxes.

MMS3 FPI/DES Mag data X,Y,Z,Norm DSC components [nT] at survey-start time [mms3_des_fpibentpipe_dsc_fast]

X, Y, Z are unit vector components.

Magnetic field vector X,Y,Z, and magnitude B [mms3_des_fpib_gse_srvy_fast]

Averaged survey magnetic field data during this FP

Magnetic field vector X,Y,Z, and magnitude B [mms3_des_fpib_dmpa_srvy_fast]

Averaged survey magnetic field data during this FP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms3_des_pos_gse_fast]

Position in GSM coordinates, 30 second [mms3_des_pos_gsm_fast]

MMS3 number density integrands [mms3_des_numberdensity_int_fast]

Integrand terms used in normalized energy integration for number density

number flux [mms3_des_numberflux_int_dbcs_fast]

Integrand terms used in normalized energy integration for number flux

MMS3 pressure tensor integrands [mms3_des_prestensor_int_dbcs_fast]

Integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms3_des_ugrid_int_fast]

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MMS3_FPI_FAST_L2_DES-PARTMOMS (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DES/Fast/Level2/PartialMoments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DES vector of data-quality indicators at survey-start time [mms3_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS3 FPI/DES partial electron number density during this survey [mms3_des_numberdensity_part_fast]

MMS3 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms3_des_bulkv_part_dbcs_fast]

MMS3 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms3_des_bulkv_part_gse_fast]

MMS3 FPI/DES partial electron pressure tensor in DBCS during this survey [mms3_des_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES partial electron pressure tensor in GSE during this survey [mms3_des_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES partial electron temperature tensor in DBCS during this survey [mms3_des_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES partial electron temperature tensor in GSE during this survey [mms3_des_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES partial electron parallel temperature during this survey [mms3_des_temppara_part_fast]

MMS3 FPI/DES partial electron perpendicular temperature during this survey [mms3_des_tempperp_part_fast]

MMS3 FPI/DES recommended energy index during this survey [mms3_des_part_index_fast]

Recommended energy index during this survey

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MMS3_FPI_FAST_L2_DIS-DIST (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DIS/Fast/Level2/Distribution/PT4.5S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data taken at burst (30/150 ms for DES/DIS)
resolution are aggregated on board and made available at survey (4.5 s)
resolution in this mode.  This product contains phase-space distribution maps of
results from surveying the high-resolution observations during each 4.5 s
period.  In particular, the (highest possible quality at the time of release)
corrected/converted "Fast Survey SkyMap" distributions are reported with
time-stamps and other annotation characterizing the state of the instrument
system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DIS fast sky-map instrument distribution - 11.3 eV (E1) using averaged even/odd steps [mms3_dis_dist_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 11.3 eV [mms3_dis_dist_fast1_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS fast sky-map instrument distribution - 39.6 eV (E6) using averaged even/odd steps [mms3_dis_dist_fast6]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 39.6 eV [mms3_dis_dist_fast6_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS fast sky-map instrument distribution - 83.9 eV (E9 using averaged even/odd steps) [mms3_dis_dist_fast9]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 83.9 eV [mms3_dis_dist_fast9_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS fast sky-map instrument distribution - 178 eV (E12) using averaged even/odd steps [mms3_dis_dist_fast12]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 178 eV [mms3_dis_dist_fast12_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS fast sky-map instrument distribution - 293 eV (E14) using averaged even/odd steps [mms3_dis_dist_fast14]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 293 eV [mms3_dis_dist_fast14_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS fast sky-map instrument distribution - 484 eV (E16) using averaged even/odd steps [mms3_dis_dist_fast16]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 484 eV [mms3_dis_dist_fast16_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS fast sky-map instrument distribution - 799 eV (E18) using averaged even/odd steps [mms3_dis_dist_fast18]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 799 eV [mms3_dis_dist_fast18_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS fast sky-map instrument distribution - 1320 eV (E20) using averaged even/odd steps [mms3_dis_dist_fast20]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1320 eV [mms3_dis_dist_fast20_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS fast sky-map instrument distribution - 2800 eV (E23) using averaged even/odd steps [mms3_dis_dist_fast23]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2800 eV [mms3_dis_dist_fast23_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS fast sky-map instrument distribution - 5920 eV (E26) using averaged even/odd steps [mms3_dis_dist_fast26]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5920 eV [mms3_dis_dist_fast26_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS fast sky-map instrument distribution - 26600 eV (E32) using averaged even/odd steps [mms3_dis_dist_fast32]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 26600 eV [mms3_dis_dist_fast32_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[Only List/Create in CDAWeb] MMS3 FPI/DIS fast sky-map instrument distribution 1-sigma error [mms3_dis_disterr_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS vector of data-quality indicators at fast survey-start time - 32-bit error flags [mms3_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS3 FPI/DIS compression lossless/lossy indicator at survey-start time [mms3_dis_compressionloss_fast]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) count at fast survey-start time [mms3_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at fast survey-start time [mms3_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS3 FPI/DIS fast survey average f1 count values [mms3_dis_avgf1counts_fast]

Average f1-count level as a function of energy

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MMS3_FPI_FAST_L2_DIS-MOMS (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DIS/Fast/Level2/Moments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution.  Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This moments product
contains results from integrating the standard moments of phase-space
distributions formed from the indicated data type (DES/DIS burst, FS or SS). For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotation characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DIS vector of data-quality indicators at survey-start time [mms3_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation, Bit-14 =
high MMS3 spintone due to DIS008 anomaly

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms3_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

---> MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms3_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS3 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms3_dis_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

---> MMS3 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms3_dis_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

---> MMS3 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms3_dis_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

---> MMS3 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms3_dis_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

---> MMS3 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms3_dis_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

---> MMS3 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms3_dis_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS3 FPI/DIS omni-directional ion energy spectrum during this survey [mms3_dis_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS3 FPI/DIS ion background energy during this survey [mms3_dis_spectr_bg_fast]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS3 FPI/DIS ion background number density during this survey [mms3_dis_numberdensity_bg_fast]

Background number density derived via integration of the estimated background
differential energy flux.

MMS3 FPI/DIS ion number density during this survey [mms3_dis_numberdensity_fast]

---> (no error bars displayed) MMS3 FPI/DIS ion number density during this survey [mms3_dis_numberdensity_fast_noerr]

MMS3 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms3_dis_densityextrapolation_low_fast]

MMS3 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms3_dis_densityextrapolation_high_fast]

MMS3 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms3_dis_bulkv_dbcs_fast]

---> (no error bars displayed) MMS3 FPI/DIS ion bulk-velocity DBCS vector during this survey [mms3_dis_bulkv_dbcs_fast_noerr]

MMS3 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey [mms3_dis_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS3 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms3_dis_bulkv_gse_fast]

MMS3 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey [mms3_dis_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

---> (no error bars displayed) MMS3 FPI/DIS ion bulk-velocity GSE vector during this survey [mms3_dis_bulkv_gse_fast_noerr]

MMS3 FPI/DIS ion pressure tensor in DBCS during this survey [mms3_dis_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS ion pressure tensor in GSE during this survey [mms3_dis_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS ion background pressure during this survey [mms3_dis_pres_bg_fast]

MMS3 FPI/DIS ion temperature tensor in DBCS during this survey [mms3_dis_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS ion temperature tensor in GSE during this survey [mms3_dis_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS ion heat-flux vector in DBCS during this survey [mms3_dis_heatq_dbcs_fast]

MMS3 FPI/DIS ion heat-flux vector in GSE during this survey [mms3_dis_heatq_gse_fast]

MMS3 FPI/DIS ion parallel temperature during this BP [mms3_dis_temppara_fast]

MMS3 FPI/DIS ion perpendicular temperature during this BP [mms3_dis_tempperp_fast]

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MMS3_FPI_FAST_L2_DIS-MOMSAUX

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DIS vector of data-quality indicators at survey-start time [mms3_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS3 FPI/DIS partial ion number density during this survey [mms3_dis_numberdensity_part_fast]

MMS3 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms3_dis_bulkv_part_dbcs_fast]

MMS3 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms3_dis_bulkv_part_gse_fast]

MMS3 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms3_dis_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS partial ion pressure tensor in GSE during this survey [mms3_dis_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms3_dis_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS partial ion temperature tensor in GSE during this survey [mms3_dis_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS partial ion parallel temperature during this survey [mms3_dis_temppara_part_fast]

MMS3 FPI/DIS partial ion perpendicular temperature during this survey [mms3_dis_tempperp_part_fast]

MMS3 FPI/DIS recommended energy index for partial moments during this survey [mms3_dis_part_index_fast]

Recommended energy index during this survey

MMS3 FPI/DIS compression lossless/lossy indicator at survey-start time [mms3_dis_compressionloss_fast]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS3 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms3_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms3_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS3 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms3_dis_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS3 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms3_dis_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS3 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms3_dis_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS3 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms3_dis_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS3 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms3_dis_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS3 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms3_dis_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS3 FPI/DIS omni-directional ion energy spectrum during this survey [mms3_dis_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS3 FPI/DIS ion background energy during this survey [mms3_dis_spectr_bg_fast]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS3 FPI/DIS ion background number density during this survey [mms3_dis_numberdensity_bg_fast]

Background number density derived via integration of the estimated background
differential energy flux.

MMS3 FPI/DIS ion number density during this survey [mms3_dis_numberdensity_fast]

MMS3 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms3_dis_densityextrapolation_low_fast]

MMS3 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms3_dis_densityextrapolation_high_fast]

MMS3 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms3_dis_bulkv_dbcs_fast]

MMS3 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey [mms3_dis_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS3 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms3_dis_bulkv_gse_fast]

MMS3 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey [mms3_dis_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS3 FPI/DIS ion pressure tensor in DBCS during this survey [mms3_dis_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS ion pressure tensor in GSE during this survey [mms3_dis_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS ion background pressure during this survey [mms3_dis_pres_bg_fast]

MMS3 FPI/DIS ion temperature tensor in DBCS during this survey [mms3_dis_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS ion temperature tensor in GSE during this survey [mms3_dis_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS ion heat-flux vector in DBCS during this survey [mms3_dis_heatq_dbcs_fast]

MMS3 FPI/DIS ion heat-flux vector in GSE during this survey [mms3_dis_heatq_gse_fast]

MMS3 FPI/DIS ion parallel temperature during this BP [mms3_dis_temppara_fast]

MMS3 FPI/DIS ion perpendicular temperature during this BP [mms3_dis_tempperp_fast]

MMS3 FPI/DIS S/C potential mean [mms3_dis_scpot_mean_fast]

Average spacecraft potential during this FP used to shift the measure energies.

MMS3 FPI/DIS S/C potential max [mms3_dis_scpot_max_fast]

Maximum spacecraft potential during this FP used to exclude energies containing
spacecraft photoelectron fluxes.

MMS3 FPI/DIS Mag data X,Y,Z,Norm DSC components [nT] at survey-start time [mms3_dis_fpibentpipe_dsc_fast]

X, Y, Z are unit vector components.

Magnetic field vector X,Y,Z, and magnitude B [mms3_dis_fpib_gse_srvy_fast]

Averaged survey magnetic field data during this FP

Magnetic field vector X,Y,Z, and magnitude B [mms3_dis_fpib_dmpa_srvy_fast]

Averaged survey magnetic field data during this FP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms3_dis_pos_gse_fast]

Position in GSM coordinates, 30 second [mms3_dis_pos_gsm_fast]

MMS3 number density integrands [mms3_dis_numberdensity_int_fast]

integrand terms used in normalized energy integration for number density

number flux [mms3_dis_numberflux_int_dbcs_fast]

integrand terms used in normalized energy integration for number flux

MMS3 pressure tensor integrands [mms3_dis_prestensor_int_dbcs_fast]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms3_dis_ugrid_int_fast]

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MMS3_FPI_FAST_L2_DIS-PARTMOMS (spase://NASA/NumericalData/MMS/3/FastPlasmaInvestigation/DIS/Fast/Level2/PartialMoments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DIS vector of data-quality indicators at survey-start time [mms3_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS3 FPI/DIS partial ion number density during this survey [mms3_dis_numberdensity_part_fast]

MMS3 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms3_dis_bulkv_part_dbcs_fast]

MMS3 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms3_dis_bulkv_part_gse_fast]

MMS3 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms3_dis_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS partial ion pressure tensor in GSE during this survey [mms3_dis_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms3_dis_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS partial ion temperature tensor in GSE during this survey [mms3_dis_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS partial ion parallel temperature during this survey [mms3_dis_temppara_part_fast]

MMS3 FPI/DIS partial ion perpendicular temperature during this survey [mms3_dis_tempperp_part_fast]

MMS3 FPI/DIS recommended energy index during this survey [mms3_dis_part_index_fast]

Recommended energy index during this survey

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MMS3_FPI_SLOW_L2_DES-DIST

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode.  This product contains phase-space distribution maps of those
survey-resolution data from Slow Mode.  In particular, the (highest possible
quality at the time of release) corrected/converted "Slow Survey SkyMap"
distributions are reported with time-stamps and other annotation characterizing
the state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DES vector of data-quality indicators at survey-start time [mms3_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = compression pipeline error

MMS3 FPI/DES compression lossless/lossy indicator at survey-start time [mms3_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS3 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms3_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS3 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms3_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS3 FPI/DES Slow Survey sky-map instrument distribution [mms3_des_dist_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES Slow Survey sky-map instrument distribution 1-sigma error [mms3_des_disterr_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DES slow survey average f1 count values [mms3_des_avgf1counts_slow]

Average f1-count level as a function of energy

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MMS3_FPI_SLOW_L2_DES-MOMS

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DES vector of data-quality indicators at survey-start time [mms3_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only)

MMS3 FPI/DES compression lossless/lossy indicator at survey-start time [mms3_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS3 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms3_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS3 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms3_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS3 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms3_des_pitchangdist_lowen_slow]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS3 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms3_des_pitchangdist_miden_slow]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS3 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms3_des_pitchangdist_highen_slow]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS3 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms3_des_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS3 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms3_des_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS3 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms3_des_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS3 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms3_des_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS3 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms3_des_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS3 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms3_des_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS3 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms3_des_energyspectr_par_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS3 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms3_des_energyspectr_anti_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS3 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms3_des_energyspectr_perp_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS3 FPI/DES omni-directional electron energy spectrum during this survey [mms3_des_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS3 FPI/DES electron number density during this survey [mms3_des_numberdensity_slow]

MMS3 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms3_des_densityextrapolation_low_slow]

MMS3 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms3_des_densityextrapolation_high_slow]

MMS3 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms3_des_bulkv_dbcs_slow]

MMS3 FPI/DES electron bulk-velocity vector in GSE during this survey [mms3_des_bulkv_gse_slow]

MMS3 FPI/DES electron pressure tensor in DBCS during this survey [mms3_des_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES electron pressure tensor in GSE during this survey [mms3_des_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES electron temperature tensor in DBCS during this survey [mms3_des_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES electron temperature tensor in GSE during this survey [mms3_des_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES electron heat-flux vector in DBCS during this survey [mms3_des_heatq_dbcs_slow]

MMS3 FPI/DES electron heat-flux vector in GSE during this survey [mms3_des_heatq_gse_slow]

MMS3 FPI/DES electron parallel temperature during this BP [mms3_des_temppara_slow]

MMS3 FPI/DES electron perpendicular temperature during this BP [mms3_des_tempperp_slow]

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MMS3_FPI_SLOW_L2_DES-MOMSAUX

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DES vector of data-quality indicators at survey-start time [mms3_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only)

MMS3 FPI/DES partial electron number density during this survey [mms3_des_numberdensity_part_slow]

MMS3 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms3_des_bulkv_part_dbcs_slow]

MMS3 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms3_des_bulkv_part_gse_slow]

MMS3 FPI/DES partial electron pressure tensor in DBCS during this survey [mms3_des_prestensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES partial electron pressure tensor in GSE during this survey [mms3_des_prestensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES partial electron temperature tensor in DBCS during this survey [mms3_des_temptensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES partial electron temperature tensor in GSE during this survey [mms3_des_temptensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES partial electron parallel temperature during this survey [mms3_des_temppara_part_slow]

MMS3 FPI/DES partial electron perpendicular temperature during this survey [mms3_des_tempperp_part_slow]

MMS3 FPI/DES recommended energy index for partial moments during this survey [mms3_des_part_index_slow]

Recommended energy index during this survey

MMS3 FPI/DES compression lossless/lossy indicator at survey-start time [mms3_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS3 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms3_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS3 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms3_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS3 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms3_des_pitchangdist_lowen_slow]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS3 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms3_des_pitchangdist_miden_slow]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS3 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms3_des_pitchangdist_highen_slow]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS3 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms3_des_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS3 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms3_des_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS3 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms3_des_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS3 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms3_des_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS3 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms3_des_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS3 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms3_des_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS3 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms3_des_energyspectr_par_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS3 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms3_des_energyspectr_anti_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS3 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms3_des_energyspectr_perp_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS3 FPI/DES omni-directional electron energy spectrum during this survey [mms3_des_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS3 FPI/DES electron number density during this survey [mms3_des_numberdensity_slow]

MMS3 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms3_des_densityextrapolation_low_slow]

MMS3 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms3_des_densityextrapolation_high_slow]

MMS3 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms3_des_bulkv_dbcs_slow]

MMS3 FPI/DES electron bulk-velocity vector in GSE during this survey [mms3_des_bulkv_gse_slow]

MMS3 FPI/DES electron pressure tensor in DBCS during this survey [mms3_des_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES electron pressure tensor in GSE during this survey [mms3_des_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DES electron temperature tensor in DBCS during this survey [mms3_des_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES electron temperature tensor in GSE during this survey [mms3_des_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DES electron heat-flux vector in DBCS during this survey [mms3_des_heatq_dbcs_slow]

MMS3 FPI/DES electron heat-flux vector in GSE during this survey [mms3_des_heatq_gse_slow]

MMS3 FPI/DES electron parallel temperature during this BP [mms3_des_temppara_slow]

MMS3 FPI/DES electron perpendicular temperature during this BP [mms3_des_tempperp_slow]

MMS3 FPI/DES S/C potential mean [mms3_des_scpot_mean_slow]

Average spacecraft potential during this SP used to shift the measure energies.

MMS3 FPI/DES S/C potential max [mms3_des_scpot_max_slow]

Maximum spacecraft potential during this SP used to exclude energies containing
spacecraft photoelectron fluxes.

Magnetic field vector X,Y,Z, and magnitude B [mms3_des_fpib_gse_srvy_slow]

Averaged survey magnetic field data during this SP

Magnetic field vector X,Y,Z, and magnitude B [mms3_des_fpib_dmpa_srvy_slow]

Averaged survey magnetic field data during this SP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms3_des_pos_gse_slow]

Position in GSM coordinates, 30 second [mms3_des_pos_gsm_slow]

MMS3 number density integrands [mms3_des_numberdensity_int_slow]

integrand terms used in normalized energy integration for number density

number flux [mms3_des_numberflux_int_dbcs_slow]

integrand terms used in normalized energy integration for number flux

MMS3 pressure tensor integrands [mms3_des_prestensor_int_dbcs_slow]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms3_des_ugrid_int_slow]

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MMS3_FPI_SLOW_L2_DIS-DIST

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode.  This product contains phase-space distribution maps of those
survey-resolution data from Slow Mode.  In particular, the (highest possible
quality at the time of release) corrected/converted "Slow Survey SkyMap"
distributions are reported with time-stamps and other annotation characterizing
the state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DIS vector of data-quality indicators at survey-start time [mms3_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = compression pipeline error

MMS3 FPI/DIS compression lossless/lossy indicator at survey-start time [mms3_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS3 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms3_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms3_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS3 FPI/DIS Slow Survey sky-map instrument distribution [mms3_dis_dist_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS Slow Survey sky-map instrument distribution 1-sigma error [mms3_dis_disterr_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS3 FPI/DIS slow survey average f1 count values [mms3_dis_avgf1counts_slow]

Average f1-count level as a function of energy

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MMS3_FPI_SLOW_L2_DIS-MOMS

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DIS vector of data-quality indicators at survey-start time [mms3_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only), Bit-13 =
significant (>=20%) penetrating radiation, Bit-14 = high MMS3 spintone due to
DIS008 anomaly

MMS3 FPI/DIS compression lossless/lossy indicator at survey-start time [mms3_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS3 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms3_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms3_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS3 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms3_dis_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS3 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms3_dis_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS3 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms3_dis_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS3 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms3_dis_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS3 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms3_dis_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS3 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms3_dis_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS3 FPI/DIS omni-directional ion energy spectrum during this survey [mms3_dis_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS3 FPI/DIS ion background energy during this survey [mms3_dis_spectr_bg_slow]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS3 FPI/DIS ion background number density during this survey [mms3_dis_numberdensity_bg_slow]

Background number density derived via integration of the estimated background
differential energy flux.

MMS3 FPI/DIS ion number density during this survey [mms3_dis_numberdensity_slow]

MMS3 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms3_dis_densityextrapolation_low_slow]

MMS3 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms3_dis_densityextrapolation_high_slow]

MMS3 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms3_dis_bulkv_dbcs_slow]

MMS3 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms3_dis_bulkv_gse_slow]

MMS3 FPI/DIS ion pressure tensor in DBCS during this survey [mms3_dis_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS ion pressure tensor in GSE during this survey [mms3_dis_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS ion background pressure during this survey [mms3_dis_pres_bg_slow]

MMS3 FPI/DIS ion temperature tensor in DBCS during this survey [mms3_dis_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS ion temperature tensor in GSE during this survey [mms3_dis_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS ion heat-flux vector in DBCS during this survey [mms3_dis_heatq_dbcs_slow]

MMS3 FPI/DIS ion heat-flux vector in GSE during this survey [mms3_dis_heatq_gse_slow]

MMS3 FPI/DIS ion parallel temperature during this BP [mms3_dis_temppara_slow]

MMS3 FPI/DIS ion perpendicular temperature during this BP [mms3_dis_tempperp_slow]

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MMS3_FPI_SLOW_L2_DIS-MOMSAUX

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS3 FPI/DIS vector of data-quality indicators at survey-start time [mms3_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only), Bit-13 =
significant (>=20%) penetrating radiation, Bit-14 = high MMS3 spintone due to
DIS008 anomaly

MMS3 FPI/DIS partial ion number density during this survey [mms3_dis_numberdensity_part_slow]

MMS3 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms3_dis_bulkv_part_dbcs_slow]

MMS3 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms3_dis_bulkv_part_gse_slow]

MMS3 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms3_dis_prestensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS partial ion pressure tensor in GSE during this survey [mms3_dis_prestensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms3_dis_temptensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS partial ion temperature tensor in GSE during this survey [mms3_dis_temptensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS partial ion parallel temperature during this survey [mms3_dis_temppara_part_slow]

MMS3 FPI/DIS partial ion perpendicular temperature during this survey [mms3_dis_tempperp_part_slow]

MMS3 FPI/DIS recommended energy index for partial moments during this survey [mms3_dis_part_index_slow]

Recommended energy index during this survey

MMS3 FPI/DIS compression lossless/lossy indicator at survey-start time [mms3_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS3 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms3_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS3 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms3_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS3 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms3_dis_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS3 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms3_dis_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS3 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms3_dis_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS3 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms3_dis_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS3 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms3_dis_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS3 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms3_dis_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS3 FPI/DIS omni-directional ion energy spectrum during this survey [mms3_dis_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS3 FPI/DIS ion background energy during this survey [mms3_dis_spectr_bg_slow]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS3 FPI/DIS ion background number density during this survey [mms3_dis_numberdensity_bg_slow]

Background number density derived via integration of the estimated background
differential energy flux.

MMS3 FPI/DIS ion number density during this survey [mms3_dis_numberdensity_slow]

MMS3 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms3_dis_densityextrapolation_low_slow]

MMS3 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms3_dis_densityextrapolation_high_slow]

MMS3 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms3_dis_bulkv_dbcs_slow]

MMS3 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms3_dis_bulkv_gse_slow]

MMS3 FPI/DIS ion pressure tensor in DBCS during this survey [mms3_dis_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS ion pressure tensor in GSE during this survey [mms3_dis_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS3 FPI/DIS ion background pressure during this survey [mms3_dis_pres_bg_slow]

MMS3 FPI/DIS ion temperature tensor in DBCS during this survey [mms3_dis_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS ion temperature tensor in GSE during this survey [mms3_dis_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS3 FPI/DIS ion heat-flux vector in DBCS during this survey [mms3_dis_heatq_dbcs_slow]

MMS3 FPI/DIS ion heat-flux vector in GSE during this survey [mms3_dis_heatq_gse_slow]

MMS3 FPI/DIS ion parallel temperature during this BP [mms3_dis_temppara_slow]

MMS3 FPI/DIS ion perpendicular temperature during this BP [mms3_dis_tempperp_slow]

MMS3 FPI/DIS S/C potential mean [mms3_dis_scpot_mean_slow]

Average spacecraft potential during this SP used to shift the measure energies.

MMS3 FPI/DIS S/C potential max [mms3_dis_scpot_max_slow]

Maximum spacecraft potential during this SP used to exclude energies containing
spacecraft photoelectron fluxes.

Magnetic field vector X,Y,Z, and magnitude B [mms3_dis_fpib_gse_srvy_slow]

Averaged survey magnetic field data during this SP

Magnetic field vector X,Y,Z, and magnitude B [mms3_dis_fpib_dmpa_srvy_slow]

Averaged survey magnetic field data during this SP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms3_dis_pos_gse_slow]

Position in GSM coordinates, 30 second [mms3_dis_pos_gsm_slow]

MMS3 number density integrands [mms3_dis_numberdensity_int_slow]

integrand terms used in normalized energy integration for number density

number flux [mms3_dis_numberflux_int_dbcs_slow]

integrand terms used in normalized energy integration for number flux

MMS3 pressure tensor integrands [mms3_dis_prestensor_int_dbcs_slow]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms3_dis_ugrid_int_slow]

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MMS3_HPCA_BRST_L2_ION (spase://NASA/NumericalData/MMS/3/HotPlasmaCompositionAnalyzer/Burst/Level2/Ion/PT0.625S)

Description

References

Modification History

Initial Public Release

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MMS3_HPCA_BRST_L2_MOMENTS (spase://NASA/NumericalData/MMS/3/HotPlasmaCompositionAnalyzer/Burst/Level2/Moments/PT10S)

Description

References

Modification History

Initial Public Release

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MMS3_HPCA_SRVY_L2_ION (spase://NASA/NumericalData/MMS/3/HotPlasmaCompositionAnalyzer/Survey/Level2/Ion/PT0.625S)

Description

References

Modification History

Initial Public Release

Data Variable Descriptions

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MMS3_HPCA_SRVY_L2_MOMENTS (spase://NASA/NumericalData/MMS/3/HotPlasmaCompositionAnalyzer/Survey/Level2/Moments/PT10S)

Description

References

Modification History

Initial Public Release

Data Variable Descriptions

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MMS3_HPCA_SRVY_L2_TOF-COUNTS (spase://NASA/NumericalData/MMS/3/HotPlasmaCompositionAnalyzer/Survey/Level2/TimeOfFlight/Counts/PT0.625S)

Description

References

Modification History

Initial Public Release

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MMS3_MEC_BRST_L2_EPHT89D (spase://NASA/NumericalData/MMS/3/Ephemeris/Burst/Level2/Tsyganenko_89_Dynamic/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS3_MEC_BRST_L2_EPHT89Q (spase://NASA/NumericalData/MMS/3/Ephemeris/Burst/Level2/Tsyganenko_89_Quiet/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS3_MEC_BRST_L2_EPHTS04D (spase://NASA/NumericalData/MMS/3/Ephemeris/Burst/Level2/Tsyganenko_04_Dynamic/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS3_MEC_SRVY_L2_EPHT89D (spase://NASA/NumericalData/MMS/3/Ephemeris/Survey/Level2/Tsyganenko_89_Dynamic/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS3_MEC_SRVY_L2_EPHT89Q (spase://NASA/NumericalData/MMS/3/Ephemeris/Survey/Level2/Tsyganenko_89_Quiet/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS3_MEC_SRVY_L2_EPHTS04D (spase://NASA/NumericalData/MMS/3/Ephemeris/Survey/Level2/Tsyganenko_04_Dynamic/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS3_R0_SUMMARY

Description

Pre-generated MMS Quicklook Summary Plots
File location: https://cdaweb.gsfc.nasa.gov/pub/data/mms/ql_plots/all_mms3_summ

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MMS3_SCM_BRST_L2_SCB (spase://NASA/NumericalData/MMS/3/FIELDS/SCM/Burst/Level2/PT0.0001220703125S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
https://urldefense.proofpoint.com/v2/url?u=http-3A__link.springer.com_article_10
.1007_s11214-2D014-2D0096-2D9&d=DwIFAg&c=c6MrceVCY5m5A_KAUkrdoA&r=bjziExGTRYoZgE
2xb_dDSm9NxNIo0lG6Q-rB0Y6rHS4&m=CMzo0Vv9zPtWSdbdY1Wq9-jIkYS2cOMV9JYZsMV10y0&s=Xb
P9PiEAswHGl5lqgsDVI6zs8ivJx7yek9i2undKl10&e=

Modification History

unpack telemetry, assign sample times
2026-07-10T20:11:42.00002789497058Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-16T12:36:48.00005346536624Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-16T12:36:54.00006115436542Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms3_scm_acb_gse_scb_brst_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 8192S/s.
They are high-pass filtered above 1.00Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide.

(List/Create Only) Quality Factor (one letter per antenna, G=good) [mms3_scm_qf_scm123_scb_brst_l2]

Each letter refers to one SCM physical antenna in the SCM123 order. 'G' stands
for good data, 'Z' for data that are affected or set to zero by convolution
boundary effect, 'S' for saturated data, 'X' for out of range data, 'B' for
fillvalue/bad data.

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MMS3_SCM_BRST_L2_SCHB (spase://NASA/NumericalData/MMS/3/FIELDS/SCM/Burst/Level2/PT0.00006101515625S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
http://link.springer.com/article/10.1007/s11214-014-0096-9

Modification History

unpack telemetry, assign sample times
2026-07-10T20:12:07.0000532269446Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-16T12:41:22.00005590915685Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-16T12:41:26.00003421306615Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms3_scm_acb_gse_schb_brst_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 16384S/s.
They are high-pass filtered above 32.00Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide
(https://lasp.colorado.edu/mms/sdc/public/datasets/fields/Science_Data_Products_ 
Guide_vol2_SCM_v11_20160301.pdf).

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MMS3_SCM_SRVY_L2_SCSRVY (spase://NASA/NumericalData/MMS/3/FIELDS/SCM/Survey/Level2/PT0.03125S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
http://link.springer.com/article/10.1007/s11214-014-0096-9

Modification History

unpack telemetry, assign sample times
2026-07-02T23:58:23.00004333257333Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-15T23:56:24.0000450611082Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-15T23:57:09.0000423788994Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms3_scm_acb_gse_scsrvy_srvy_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 32S/s. They
are high-pass filtered above 0.50Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide
(https://lasp.colorado.edu/mms/sdc/public/datasets/fields/Science_Data_Products_ 
Guide_vol2_SCM_v11_20160301.pdf).

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MMS4_ASPOC_SRVY_L2 (spase://NASA/NumericalData/MMS/4/ASPOC/Survey/Level2/PT1S)

Description

K. Torkar et al, Active Spacecraft Potential Control Investigation
Space Science Reviews, 2014, DOI: 10.1007/s11214-014-0049-3
Further information:
- http://www.iwf.oeaw.ac.at/en/research/near-earth-space/mms/ 
- http://mms.space.swri.edu/

Modification History

150224 Initial version
150831 Minor updates and fixes
160205 CDF file format guide compliant

Data Variable Descriptions

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MMS4_DSP_FAST_L2_BPSD (spase://NASA/NumericalData/MMS/4/FIELDS/DSP/Fast/Level2/MagneticFieldPowerSpectralDensity/PT2S)

Description

BPSD is the low frequency B spectral density covering the frequency range of .2
to 6000 Hz.

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MMS4_DSP_FAST_L2_EPSD (spase://NASA/NumericalData/MMS/4/FIELDS/DSP/Fast/Level2/ElectricFieldPowerSpectralDensity/PT2S)

Description

EPSD combines the low frequency E spectral density covering the frequency range
of 1 to 8000 Hz and the  medium frequency E spectral density covering the
frequency range of .25 to 100 kHz.

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MMS4_DSP_SLOW_L2_BPSD (spase://NASA/NumericalData/MMS/4/FIELDS/DSP/Slow/Level2/MagneticFieldPowerSpectralDensity/PT16S)

Description

search coil magnetometer spectral density

Data Variable Descriptions

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MMS4_DSP_SLOW_L2_EPSD (spase://NASA/NumericalData/MMS/4/FIELDS/DSP/Slow/Level2/ElectricFieldPowerSpectralDensity/PT16S)

Description

electric spectral density

Data Variable Descriptions

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MMS4_EDI_BRST_L2_AMB (spase://NASA/NumericalData/MMS/4/FIELDS/EDI/Burst/Level2/ElectronFluxAmbient/ProjectionMethod1/PT0.0009765625S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - Original version.
v1.0.0 - Include trajectory vectors and optics state.
v1.1.0 - Update metadata: counts -> flux.
v1.2.0 - Added flux error.
v1.3.0 - Trajectory vector errors are now deltas.
v1.4.0 - Fixed dead-time correction and error values.
v1.5.0 - Factor of 2 for accumulation time & 2 for abscal factor in srvy mode.
v1.6.0 - No factor of 2 for accumulation time in srvy mode.
v2.0.0 - Reduced file size with scalar errors. Update metadata.
v2.1.0 - Correct fill value for fluxes.
v3.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v4.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.

Data Variable Descriptions

Optics state [mms4_edi_optics_state_brst_l2]

---> GDU1 energy [mms4_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms4_edi_energy_gdu2_brst_l2]

Flux for electrons with trajectories given by Traj-1 0PA [mms4_edi_flux1_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-1 0PA [mms4_edi_flux1_0_brst_l2_noerr]

---> Error for flux1 0-degree pitch angle electron flux. [mms4_edi_flux1_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-2 0PA [mms4_edi_flux2_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-2 0PA [mms4_edi_flux2_0_brst_l2_noerr]

---> Error for flux2 0-degree pitch angle electron flux. [mms4_edi_flux2_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-3 0PA [mms4_edi_flux3_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-3 0PA [mms4_edi_flux3_0_brst_l2_noerr]

---> Error for flux3 0-degree pitch angle electron flux. [mms4_edi_flux3_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-4 0PA [mms4_edi_flux4_0_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-4 0PA [mms4_edi_flux4_0_brst_l2_noerr]

---> Error for flux4 0-degree pitch angle electron flux. [mms4_edi_flux4_0_delta_brst_l2]

Flux for electrons with trajectories given by Traj-1 180PA [mms4_edi_flux1_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-1 180PA [mms4_edi_flux1_180_brst_l2_noerr]

---> Error for flux1 180-degree pitch angle electron flux. [mms4_edi_flux1_180_delta_brst_l2]

Flux for electrons with trajectories given by traj2 180PA [mms4_edi_flux2_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-2 180PA [mms4_edi_flux2_180_brst_l2_noerr]

---> Error for flux2 180-degree pitch angle electron flux. [mms4_edi_flux2_180_delta_brst_l2]

Flux for electrons with trajectories given by traj3 180PA [mms4_edi_flux3_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-3 180PA [mms4_edi_flux3_180_brst_l2_noerr]

---> Error for flux3 180-degree pitch angle electron flux. [mms4_edi_flux3_180_delta_brst_l2]

Flux for electrons with trajectories given by traj4 180PA [mms4_edi_flux4_180_brst_l2]

---> (no error bars displayed) Flux for electrons with trajectories given by Traj-4 180PA [mms4_edi_flux4_180_brst_l2_noerr]

---> Error for flux4 180-degree pitch angle electron flux. [mms4_edi_flux4_180_delta_brst_l2]

Trajectory of flux1 0-degree pitch angle electrons in GSE coordinates. [mms4_edi_traj1_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 0-degree pitch angle electrons in GSE coordinates. [mms4_edi_traj2_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 0-degree pitch angle electrons in GSE coordinates. [mms4_edi_traj3_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 0-degree pitch angle electrons in GSE coordinates. [mms4_edi_traj4_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 180-degree pitch angle electrons in GSE coordinates. [mms4_edi_traj1_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 180-degree pitch angle electrons in GSE coordinates. [mms4_edi_traj2_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 180-degree pitch angle electrons in GSE coordinates. [mms4_edi_traj3_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 180-degree pitch angle electrons in GSE coordinates. [mms4_edi_traj4_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj1_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 0-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj2_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 0-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj3_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 0-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj4_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj1_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux2 180-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj2_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux3 180-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj3_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

---> Trajectory of flux4 180-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj4_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms4_edi_traj1_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms4_edi_traj2_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms4_edi_traj3_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms4_edi_traj4_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms4_edi_traj1_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms4_edi_traj2_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms4_edi_traj3_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms4_edi_traj4_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS4_EDI_BRST_L2_AMB-PM2 (spase://NASA/NumericalData/MMS/4/FIELDS/EDI/Burst/Level2/AmbientElectronFlux/ProjectionMethod2/PT0.0009765625S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v1.0.0 - Original version.
v1.1.0 - Correct fill value for fluxes.
v2.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v3.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.
v4.0.0 - Each trajectory has its own LABL_PTR_1 variable.

Data Variable Descriptions

Optics state [mms4_edi_optics_state_brst_l2]

---> GDU1 energy [mms4_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms4_edi_energy_gdu2_brst_l2]

Field-aligned electron flux from channel 1 of both GDUs [mms4_edi_flux1_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 1 of both GDUs [mms4_edi_flux1_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 1 of both GDUs. [mms4_edi_flux1_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 1 of both GDUs [mms4_edi_flux1_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 1 of both GDUs [mms4_edi_flux1_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 1 of both GDUs. [mms4_edi_flux1_180_delta_brst_l2]

Field-aligned electron flux from channel 2 of both GDUs [mms4_edi_flux2_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 2 of both GDUs [mms4_edi_flux2_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 2 of both GDUs. [mms4_edi_flux2_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 2 of both GDUs [mms4_edi_flux2_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 2 of both GDUs [mms4_edi_flux2_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 2 of both GDUs. [mms4_edi_flux2_180_delta_brst_l2]

Field-aligned electron flux from channel 3 of both GDUs [mms4_edi_flux3_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 3 of both GDUs [mms4_edi_flux3_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 3 of both GDUs. [mms4_edi_flux3_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 3 of both GDUs [mms4_edi_flux3_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 3 of both GDUs [mms4_edi_flux3_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 3 of both GDUs. [mms4_edi_flux3_180_delta_brst_l2]

Field-aligned electron flux from channel 4 of both GDUs [mms4_edi_flux4_0_brst_l2]

---> (no error bars displayed) Field-aligned electron flux from channel 4 of both GDUs [mms4_edi_flux4_0_brst_l2_noerr]

---> Error in field-aligned electron flux from channel 4 of both GDUs. [mms4_edi_flux4_0_delta_brst_l2]

Anti-field-aligned electron flux from channel 4 of both GDUs [mms4_edi_flux4_180_brst_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from channel 4 of both GDUs [mms4_edi_flux4_180_brst_l2_noerr]

---> Error in anti-field-aligned electron flux from channel 4 of both GDUs. [mms4_edi_flux4_180_delta_brst_l2]

Trajectory of field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms4_edi_traj1_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs in DBCS coordinates. [mms4_edi_traj1_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 1 of both GDUs in GSE coordinates. [mms4_edi_traj1_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 1 of both GDUs, in GSE coordinates. [mms4_edi_traj1_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms4_edi_traj2_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs in DBCS coordinates. [mms4_edi_traj2_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 2 of both GDUs in GSE coordinates. [mms4_edi_traj2_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 2 of both GDUs, in GSE coordinates. [mms4_edi_traj2_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms4_edi_traj3_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs in DBCS coordinates. [mms4_edi_traj3_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 3 of both GDUs in GSE coordinates. [mms4_edi_traj3_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 3 of both GDUs, in GSE coordinates. [mms4_edi_traj3_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms4_edi_traj4_dbcs_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs in DBCS coordinates. [mms4_edi_traj4_dbcs_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from channel 4 of both GDUs in GSE coordinates. [mms4_edi_traj4_gse_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from channel 4 of both GDUs, in GSE coordinates. [mms4_edi_traj4_gse_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj1_gsm_0_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj1_gsm_180_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS4_EDI_BRST_L2_EFIELD (spase://NASA/NumericalData/MMS/4/FIELDS/EDI/Burst/Level2/ElectricField/PT0.0009765625S)

Description

EDI electric field data. Instrument papers for EDI can be found at:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7

Modification History

v1.0.0 - First version. TRI-TOF selection based on smallest error.
v1.1.0 - TRI-TOF merged by weighted average.
v1.2.0 - Fixed t_delta_plus/minus CDF_type.
v1.3.0 - Fixed Fixed vdrift SI conversion.
v1.4.0 - Fixed data duplication caused by multiple l2pre file locations.
v1.5.0 - Inplemented baseline*beams*Bmag filter for triangulation.
v1.6.0 - Inplemented null files for no or low quality data.

Data Variable Descriptions

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MMS4_EDI_BRST_L2_Q0 (spase://NASA/NumericalData/MMS/4/FIELDS/EDI/Burst/Level2/QualityZero/PT0.0078125S)

Description

EDI Q0 data. The EDI instrument paper and data products guidescan be found at
the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - First version.
v0.0.1 - Filled energy variables.
v0.0.2 - Energy written properly.
v1.0.0 - Update variable names.
v1.1.0 - Added optics state.
v2.0.0 - Added electron trajectories.
v2.1.0 - Deltas on trajectory vectors are now deltas.
v3.0.0 - Reduced file size with scalar errors. Add VAR_NOTES.
v3.1.0 - Fixed optics datatype.
v4.0.0 - Removed unused Epoch variable.
v5.0.0 - Trajectories are provided in DBCS coordinates.

Data Variable Descriptions

Optics state [mms4_edi_optics_state_brst_l2]

---> GDU1 energy [mms4_edi_energy_gdu1_brst_l2]

---> GDU2 energy [mms4_edi_energy_gdu2_brst_l2]

GDU1 quality 0 counts. [mms4_edi_counts_gdu1_brst_l2]

Q0 data consists of raw electron counts. The error at any one time is the
square-root of the counts. Note that there may be contamination from the EDI
electron beams. See the data products guide or contact an EDI team member to
learn about beam contamination.

GDU2 quality 0 counts. [mms4_edi_counts_gdu2_brst_l2]

GDU1 electron incident trajectory vectors in spherical BCS coordinates. [mms4_edi_traj_bcs_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical BCS coordinates. [mms4_edi_traj_bcs_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical DBCS coordinates. [mms4_edi_traj_dbcs_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical DBCS coordinates. [mms4_edi_traj_dbcs_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSE coordinates. [mms4_edi_traj_gse_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSE coordinates. [mms4_edi_traj_gse_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSM coordinates. [mms4_edi_traj_gsm_gdu1_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSM coordinates. [mms4_edi_traj_gsm_gdu2_brst_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS4_EDI_SRVY_L2_AMB (spase://NASA/NumericalData/MMS/4/FIELDS/EDI/Survey/Level2/ElectronFluxAmbient/ProjectionMethod1/PT0.03125S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - Original version.
v1.0.0 - Include trajectory vectors and optics state.
v1.1.0 - Update metadata: counts -> flux.
v1.2.0 - Added flux error.
v1.3.0 - Trajectory vector errors are now deltas.
v1.4.0 - Fixed dead-time correction and error values.
v1.5.0 - Factor of 2 for accumulation time & 2 for abscal factor in srvy mode.
v1.6.0 - No factor of 2 for accumulation time in srvy mode.
v2.0.0 - Reduced file size with scalar errors. Update metadata.
v2.1.0 - Correct fill value for fluxes.
v3.0.0 - Omni-directional error for trajectories. Correct time deltas. Y-Version
linked to cal file. Single epoch for counts.
v4.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.

Data Variable Descriptions

Optics state [mms4_edi_optics_state_srvy_l2]

---> GDU1 energy [mms4_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms4_edi_energy_gdu2_srvy_l2]

Field-aligned electron flux from both GDUs [mms4_edi_flux1_0_srvy_l2]

---> (no error bars displayed) Field-aligned electron flux from both GDUs [mms4_edi_flux1_0_srvy_l2_noerr]

---> Error in field-aligned electron flux from both GDUs. [mms4_edi_flux1_0_delta_srvy_l2]

Anti-field-aligned electron flux from both GDUs [mms4_edi_flux1_180_srvy_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from both GDUs [mms4_edi_flux1_180_srvy_l2_noerr]

---> Error in anti-field-aligned electron flux from both GDUs. [mms4_edi_flux1_180_delta_srvy_l2]

Trajectory of field-aligned electrons from both GDUs in DBCS coordinates. [mms4_edi_traj1_dbcs_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs in DBCS coordinates. [mms4_edi_traj1_dbcs_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from both GDUs in GSE coordinates. [mms4_edi_traj1_gse_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs, in GSE coordinates. [mms4_edi_traj1_gse_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj1_gsm_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj1_gsm_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS4_EDI_SRVY_L2_AMB-PM2 (spase://NASA/NumericalData/MMS/4/FIELDS/EDI/Survey/Level2/ElectronFluxAmbient/ProjectionMethod2/PT0.03125S)

Description

EDI ambient data. The EDI instrument paper and data products guide can be found
at the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v1.0.0 - Original version.
v1.1.0 - Correct fill value for fluxes.
v2.0.0 - Omni-directional error for trajectories. Y-Version linked to cal file.
Single epoch for counts.
v3.0.0 - Replace data in GSM coordinates with data in DBCS to be consistent with
other particle instruments.
v4.0.0 - Each trajectory has its own LABL_PTR_1 variable.

Data Variable Descriptions

Optics state [mms4_edi_optics_state_srvy_l2]

---> GDU1 energy [mms4_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms4_edi_energy_gdu2_srvy_l2]

Field-aligned electron flux from both GDUs [mms4_edi_flux1_0_srvy_l2]

---> (no error bars displayed) Field-aligned electron flux from both GDUs [mms4_edi_flux1_0_srvy_l2_noerr]

---> Error in field-aligned electron flux from both GDUs. [mms4_edi_flux1_0_delta_srvy_l2]

Anti-field-aligned electron flux from both GDUs [mms4_edi_flux1_180_srvy_l2]

---> (no error bars displayed) Anti-field-aligned electron flux from both GDUs [mms4_edi_flux1_180_srvy_l2_noerr]

---> Error in anti-field-aligned electron flux from both GDUs. [mms4_edi_flux1_180_delta_srvy_l2]

Trajectory of field-aligned electrons from both GDUs in DBCS coordinates. [mms4_edi_traj1_dbcs_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs in DBCS coordinates. [mms4_edi_traj1_dbcs_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of field-aligned electrons from both GDUs in GSE coordinates. [mms4_edi_traj1_gse_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

Trajectory of anti-field-aligned electrons from both GDUs, in GSE coordinates. [mms4_edi_traj1_gse_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 0-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj1_gsm_0_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

[OUTDATED] Trajectory of flux1 180-degree pitch angle electrons in GSM coordinates. [mms4_edi_traj1_gsm_180_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS4_EDI_SRVY_L2_EFIELD (spase://NASA/NumericalData/MMS/4/FIELDS/EDI/Survey/Level2/ElectricField/PT5S)

Description

EDI electric field data. Instrument papers for EDI can be found at:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7

Modification History

v1.0.0 - First version. TRI-TOF selection based on smallest error.
v1.1.0 - TRI-TOF merged by weighted average.
v1.2.0 - Fixed t_delta_plus/minus CDF_type.
v1.3.0 - Fixed Fixed vdrift SI conversion.
v1.4.0 - Fixed data duplication caused by multiple l2pre file locations.
v1.5.0 - Inplemented baseline*beams*Bmag filter for triangulation.
v1.6.0 - Inplemented null files for no or low quality data.

Data Variable Descriptions

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MMS4_EDI_SRVY_L2_Q0 (spase://NASA/NumericalData/MMS/4/FIELDS/EDI/Survey/Level2/QualityZero/PT0.125S)

Description

EDI Q0 data. The EDI instrument paper and data products guidescan be found at
the following two links:
http://link.springer.com/article/10.1007%2Fs11214-015-0182-7,
https://lasp.colorado.edu/mms/sdc/public/datasets/fields/

Modification History

v0.0.0 - First version.
v0.0.1 - Filled energy variables.
v0.0.2 - Energy written properly.
v1.0.0 - Update variable names.
v1.1.0 - Added optics state.
v2.0.0 - Added electron trajectories.
v2.1.0 - Deltas on trajectory vectors are now deltas.
v3.0.0 - Reduced file size with scalar errors. Add VAR_NOTES.
v4.0.0 - Removed unused Epoch variable.
v5.0.0 - Trajectories are provided in DBCS coordinates.

Data Variable Descriptions

Optics state [mms4_edi_optics_state_srvy_l2]

---> GDU1 energy [mms4_edi_energy_gdu1_srvy_l2]

---> GDU2 energy [mms4_edi_energy_gdu2_srvy_l2]

GDU1 quality 0 counts. [mms4_edi_counts_gdu1_srvy_l2]

Q0 data consists of raw electron counts. The error at any one time is the
square-root of the counts. Note that there may be contamination from the EDI
electron beams. See the data products guide or contact an EDI team member to
learn about beam contamination.

GDU2 quality 0 counts. [mms4_edi_counts_gdu2_srvy_l2]

GDU1 electron incident trajectory vectors in spherical BCS coordinates. [mms4_edi_traj_bcs_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical BCS coordinates. [mms4_edi_traj_bcs_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical DBCS coordinates. [mms4_edi_traj_dbcs_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical DBCS coordinates. [mms4_edi_traj_dbcs_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSE coordinates. [mms4_edi_traj_gse_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSE coordinates. [mms4_edi_traj_gse_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU1 electron incident trajectory vectors in spherical GSM coordinates. [mms4_edi_traj_gsm_gdu1_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

GDU2 Electron incident trajectory vectors in spherical GSM coordinates. [mms4_edi_traj_gsm_gdu2_srvy_l2]

Trajectories are given as unit vectors in spherical coordinates, with phi
(theta) representing the azimuthal (polar) directions, in the indicated
coordinate system. They are opposite to the nominal look-direction of the
instrument. Errors represent an omni-directional error. For more details about
errors, contact the EDI instrument team.

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MMS4_EDP_BRST_L2_DCE (spase://NASA/NumericalData/MMS/4/FIELDS/EDP/Burst/Level2/DCElectricField/PT0.0001220703125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS4_EDP_BRST_L2_HMFE (spase://NASA/NumericalData/MMS/4/FIELDS/EDP/Burst/Level2Pre/HMFE/PT0.00001525878906S)

Description

Data Variable Descriptions

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MMS4_EDP_BRST_L2_SCPOT doi:10.48322/j5ge-t096
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

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MMS4_EDP_FAST_L2_DCE (spase://NASA/NumericalData/MMS/4/FIELDS/EDP/Fast/Level2/DCElectricField/PT0.03125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS4_EDP_FAST_L2_SCPOT doi:10.48322/194m-pq72
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

Data Variable Descriptions

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MMS4_EDP_SLOW_L2_DCE (spase://NASA/NumericalData/MMS/4/FIELDS/EDP/Slow/Level2/DCElectricField/PT0.125S)

Description

http://mms.gsfc.nasa.gov/

Modification History

V.0. Initial release.

Data Variable Descriptions

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MMS4_EDP_SLOW_L2_SCPOT doi:10.48322/t44j-x227
Proper citations should include the "Accessed on date" in the form .

Description

http://mms.gsfc.nasa.gov/
The full name of PI affiliations: SWRI - Southwest Research Institute. LASP -
Laboratory for Atmospheric and Space Physics. KTH - Kungliga Tekniska Hogskolan
(Swedish Royal Institute of Technology).

Modification History

V.0. Initial release.
V.1. QL (v1.0.z), SCPOT (v1.0.z), L2A (v0.1.z) now uses ASPOC srvy l2 and
DEFATT, if these are available. Brst QL uses intermediate L2A file from Fast
mode for delta offsets. Bitmask changed to uint16 and Quality to uint8.
V.2. SCPOT (v2.0.z), L2A (v1.0.z) now uses variable names in accordance with new
recommended standard for FIELDS, All products change shortening factor to 1.25
on SDP, offsets applied indicated by GlobalAttribute Calibration_file.
V.2. L2a (v2.0.z), QL (v1.6.z) now try to remove solar wind wake which
previously left a clear sinusodial signal in the data.
V.3. L2a (v3.0.z) Slow Mode probe Gain set to 1.0 when orbital radius less than
5 RE (1.25 otherwise), L2pre (v2.0.z) DSL offsets removed from field is now
included in the file as the Slow mode is dependent on scpot product (Fast/Brst
is simply based on offset in Calibration_file).

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MMS4_EDP_SRVY_L2_HFESP (spase://NASA/NumericalData/MMS/4/FIELDS/EDP/Survey/Level2/HighFrequencyElectricFieldSpectra/PT16S)

Description

 AC Electric Field

Data Variable Descriptions

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MMS4_EPD-EIS_BRST_L2_EXTOF (spase://NASA/NumericalData/MMS/4/EnergeticParticleDetector/EIS/Burst/Level2/EnergyByTimeOfFlight/PT0.605S)

Description

empty

Modification History

Constantly modifying this code

Data Variable Descriptions

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MMS4_EPD-EIS_BRST_L2_PHXTOF (spase://NASA/NumericalData/MMS/4/EnergeticParticleDetector/EIS/Burst/Level2/PulseHeightByTimeOfFlight/PT0.605S)

Description

empty

Modification History

Constantly modifying this code

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MMS4_EPD-EIS_SRVY_L2_ELECTRONENERGY (spase://NASA/NumericalData/MMS/4/EnergeticParticleDetector/EIS/Survey/Level2/ElectronEnergySpectra/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS4_EPD-EIS_SRVY_L2_EXTOF (spase://NASA/NumericalData/MMS/4/EnergeticParticleDetector/EIS/Survey/Level2/EnergyByTimeOfFlight/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS4_EPD-EIS_SRVY_L2_PHXTOF (spase://NASA/NumericalData/MMS/4/EnergeticParticleDetector/EIS/Survey/Level2/PulseHeightByTimeOfFlight/PT2.42S)

Description

empty

Modification History

Constantly modifying this code

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MMS4_FEEPS_BRST_L2_ELECTRON (spase://NASA/NumericalData/MMS/4/EnergeticParticleDetector/FEEPS/Burst/Level2/Electron/PT0.3025S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS4_FEEPS_BRST_L2_ION (spase://NASA/NumericalData/MMS/4/EnergeticParticleDetector/FEEPS/Burst/Level2/Ion/PT0.3025S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS4_FEEPS_SRVY_L2_ELECTRON (spase://NASA/NumericalData/MMS/4/EnergeticParticleDetector/FEEPS/Survey/Level2/Electron/PT2.42S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS4_FEEPS_SRVY_L2_ION (spase://NASA/NumericalData/MMS/4/EnergeticParticleDetector/FEEPS/Survey/Level2/Ion/PT2.42S)

Description

http://www.lasp.colorado.edu

Modification History

Generated at LASP

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MMS4_FGM_BRST_L2 (spase://NASA/NumericalData/MMS/4/FIELDS/FGM/Burst/Level2/PT0.0078125S)

Description

The Fluxgate Magnetometers (FGM) on Magnetospheric Multiscale consist of a
traditional Analog Fluxgate Magnetometer (AFG), and a Digital Fluxgate
magnetometer (DFG). The dual magnetometers are operated as a single instrument
providing a single intercalibrated data product. Range changes occur at
different times on the two instruments so the gains checked each periapsis can
be carried out unambiguously to apoapsis. Cross correlation of calibration
parameters can separate causes of the any apparent calibration changes. Use of
Electron Drift Instrument (EDI) to determine the field along the rotation axis
allows accurate monitoring of the zero levels along the rotation axis.  Prior to
launch the magnetometers were calibrated at the Technical University,
Braunschweig, except for the AFG magnetometers on MMS3 and MMS4, which were
calibrated at UCLA.  Both sets of sensors are operated for the entire MMS orbit,
with slow survey (8 samples per second) outside of the Region of Interest (ROI),
and fast survey (16 samples per second) inside the ROI. Within the ROI burst
mode data (128 samples per second) are also acquired.  A detailed description of
the MMS fluxgate magnetometers, including science objectives, instrument
description, calibration, magnetic cleanliness program, and data flow can be
found at http://link.springer.com/article/10.1007%2Fs11214-014-0057-3 (DOI 
10.1007/s11214-014-0057-3).Additional information can also be found at
http://www-spc.igpp.ucla.edu/ssc/mms (UCLA),and http://www.iwf.oeaw.ac.at (IWF,
Graz).
For the purpose of creating a unified FGM Level2 data product, burst mode data
is taken from DFG and survey mode data is taken from AFG.  Because AFG and DFG
are cross-calibrated on an orbit-averaged basis, small differences in offset may
be observed between Level2 burst and survey mode data.  Consequently, any
differences are within the error of the measurement. Based on preliminary
analysis of the data, the absolute error within the Region of Interest (ROI) is
estimated to be no more than 0.1 nT in the spin-plane, 0.15 nT along the
spin-axis and 0.2 nT in total magnitude.

Modification History

version X=5:  * Y-version number comes from cal file entries. 
              *
Ensures there are 2 ephemeris points before/after data to enable proper spline. 

              * Fix to depend_0 of rdeltahalf:  fixes bug when reading position
data.
              * L-vector for DMPA2GSE transformation is smoothed with a
gaussian filter, instead 
                of using a single average value for
the day.  This short-term filter avoids  
                introduding artificial
jumps at 00:00 UTC and removes 7-minute 'wobble' after  
               
maneuvers in the GSE result.   
              * Fixes error with DEFATT file
selection found when choosing the 
                daily DEFATT files to be used
in Phase 2.
              * Fixed bug where reference Etemp was used for high
range gain.  Now uses measured Etemp.
version X=4:  First version for public
release of L2.
              Renamed variables to conform with new MMS variable
name guidelines 
              (obs_instr_paramName[_coordSys]_mode_level):  
  
             Mag field parameters include 'b' for paramName.  
               
Use 'r' instead of 'pos' for S/C position paramName.  
               
Eliminated 'rate', replaced with 'bdeltahalf'.  Added 'rdeltahalf'.
            
   l1a_mode is now just 'mode'.
version X=3:  fixed removal of overlap between
modes.
              fixed a bug that caused stemp and etemp to be
empty.
version X=2:  flag parameter name corrected: was 'status'
               
        added bits 4, 5, 6 to flag saturation on B1, B2, and B3, respectively
  
                     added bit 7 to flag bad data at range changes
             
Added etemp and l1a_mode parameters.  
              rate, hirange, and stemp
parameters now comply with MMS CDF Guidlelines, e.g.
              FILLVAL now
defined for stemp and etemp, and is set to !values.f_nan
              No longer
use Var_Parents attribute in stemp -- see Parents instead
              In this
version, temperature-corrected gains are applied.  Reference temperatures are
used when 
              stemp or etemp are set to FILLVAL. 
             
Non-linearity correction is applied to high rage DFG data.
version X=1:  added
'flag', rate and hirange parameters (but 'flag' is actually called 'status')

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MMS4_FGM_SRVY_L2 (spase://NASA/NumericalData/MMS/4/FIELDS/FGM/Survey/Level2/PT0.125S)

Description

The Fluxgate Magnetometers (FGM) on Magnetospheric Multiscale consist of a
traditional Analog Fluxgate Magnetometer (AFG), and a Digital Fluxgate
magnetometer (DFG). The dual magnetometers are operated as a single instrument
providing a single intercalibrated data product. Range changes occur at
different times on the two instruments so the gains checked each periapsis can
be carried out unambiguously to apoapsis. Cross correlation of calibration
parameters can separate causes of the any apparent calibration changes. Use of
Electron Drift Instrument (EDI) to determine the field along the rotation axis
allows accurate monitoring of the zero levels along the rotation axis.  Prior to
launch the magnetometers were calibrated at the Technical University,
Braunschweig, except for the AFG magnetometers on MMS3 and MMS4, which were
calibrated at UCLA.  Both sets of sensors are operated for the entire MMS orbit,
with slow survey (8 samples per second) outside of the Region of Interest (ROI),
and fast survey (16 samples per second) inside the ROI. Within the ROI burst
mode data (128 samples per second) are also acquired.  A detailed description of
the MMS fluxgate magnetometers, including science objectives, instrument
description, calibration, magnetic cleanliness program, and data flow can be
found at http://link.springer.com/article/10.1007%2Fs11214-014-0057-3 (DOI 
10.1007/s11214-014-0057-3).Additional information can also be found at
http://www-spc.igpp.ucla.edu/ssc/mms (UCLA),and http://www.iwf.oeaw.ac.at (IWF,
Graz).
For the purpose of creating a unified FGM Level2 data product, burst mode data
is taken from DFG and survey mode data is taken from AFG.  Because AFG and DFG
are cross-calibrated on an orbit-averaged basis, small differences in offset may
be observed between Level2 burst and survey mode data.  Consequently, any
differences are within the error of the measurement. Based on preliminary
analysis of the data, the absolute error within the Region of Interest (ROI) is
estimated to be no more than 0.1 nT in the spin-plane, 0.15 nT along the
spin-axis and 0.2 nT in total magnitude.

Modification History

version X=5:  * Y-version number comes from cal file entries. 
              *
Ensures there are 2 ephemeris points before/after data to enable proper spline. 

              * Fix to depend_0 of rdeltahalf:  fixes bug when reading position
data.
              * L-vector for DMPA2GSE transformation is smoothed with a
gaussian filter, instead 
                of using a single average value for
the day.  This short-term filter avoids  
                introduding artificial
jumps at 00:00 UTC and removes 7-minute 'wobble' after  
               
maneuvers in the GSE result.   
              * Fixes error with DEFATT file
selection found when choosing the 
                daily DEFATT files to be used
in Phase 2.
              * Fixed bug where reference Etemp was used for high
range gain.  Now uses measured Etemp.
version X=4:  First version for public
release of L2.
              Renamed variables to conform with new MMS variable
name guidelines 
              (obs_instr_paramName[_coordSys]_mode_level):  
  
             Mag field parameters include 'b' for paramName.  
               
Use 'r' instead of 'pos' for S/C position paramName.  
               
Eliminated 'rate', replaced with 'bdeltahalf'.  Added 'rdeltahalf'.
            
   l1a_mode is now just 'mode'.
version X=3:  fixed removal of overlap between
modes.
              fixed a bug that caused stemp and etemp to be
empty.
version X=2:  flag parameter name corrected: was 'status'
               
        added bits 4, 5, 6 to flag saturation on B1, B2, and B3, respectively
  
                     added bit 7 to flag bad data at range changes
             
Added etemp and l1a_mode parameters.  
              rate, hirange, and stemp
parameters now comply with MMS CDF Guidlelines, e.g.
              FILLVAL now
defined for stemp and etemp, and is set to !values.f_nan
              No longer
use Var_Parents attribute in stemp -- see Parents instead
              In this
version, temperature-corrected gains are applied.  Reference temperatures are
used when 
              stemp or etemp are set to FILLVAL. 
             
Non-linearity correction is applied to high rage DFG data.
version X=1:  added
'flag', rate and hirange parameters (but 'flag' is actually called 'status')

Data Variable Descriptions

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MMS4_FPI_BRST_L2_DES-DIST (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DES/Burst/Level2/Distribution/PT0.03S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data are taken at burst (30/150 ms for DES/DIS)
resolution in this mode.  Data are also made available at survey (4.5 s, etc)
resolution; these form a separate product from this.  Per mission design, not
all burst-resolution data are downlinked.  This product contains phase-space
distribution maps of those burst-resolution data selected for downlink.  In
particular, the (highest possible quality at the time of release)
corrected/converted "Burst SkyMap" distributions are reported with time-stamps
and other annotation characterizing the state of the instrument system at the
indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

[CDAWeb List/Download/Create ONLY] MMS4 FPI/DES burst sky-map instrument distribution [mms4_des_dist_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 10.9 eV (E1/even) [mms4_des_dist_brst1_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 12.4 eV (E1/odd) [mms4_des_dist_brst1_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~11.6 eV (E1 even-odd) [mms4_des_dist_brst1_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 10.9 eV (E1/even) [mms4_des_dist_brst1_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 12.4 eV (E1/odd) [mms4_des_dist_brst1_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 37.9 eV (E6/even) [mms4_des_dist_brst6_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 42.9 eV (E6/odd) [mms4_des_dist_brst6_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~40.4 eV (E6 even-odd) [mms4_des_dist_brst6_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 37.9 eV (E6/even) [mms4_des_dist_brst6_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 42.9 eV (E6/odd) [mms4_des_dist_brst6_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 80.0 eV (E9/even) [mms4_des_dist_brst9_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 90.6 eV (E9/odd) [mms4_des_dist_brst9_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~85 eV (E9 even-odd) [mms4_des_dist_brst9_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 80.0 eV (E9/even) [mms4_des_dist_brst9_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 90.6 eV (E9/odd) [mms4_des_dist_brst9_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 169 eV (E12/even) [mms4_des_dist_brst12_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 191 eV (E12/odd) [mms4_des_dist_brst12_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~180 eV (E12 even-odd) [mms4_des_dist_brst12_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 169 eV (E12/even) [mms4_des_dist_brst12_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 191 eV (E12/odd) [mms4_des_dist_brst12_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 277 eV (E14/even) [mms4_des_dist_brst14_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 314 eV (E14/odd) [mms4_des_dist_brst14_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~295 eV (E14 even-odd) [mms4_des_dist_brst14_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 277 eV (E14/even) [mms4_des_dist_brst14_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 314 eV (E14/odd) [mms4_des_dist_brst14_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 456 eV (E16/even) [mms4_des_dist_brst16_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 517 eV (E16/odd) [mms4_des_dist_brst16_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~485 eV (E16 even-odd) [mms4_des_dist_brst16_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 456 eV (E16/even) [mms4_des_dist_brst16_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 517 eV (E16/odd) [mms4_des_dist_brst16_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 750 eV (E18/even) [mms4_des_dist_brst18_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 850 eV (E18/odd) [mms4_des_dist_brst18_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~800 eV (E18 even-odd) [mms4_des_dist_brst18_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 750 eV (E18/even) [mms4_des_dist_brst18_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 850 eV (E18/odd) [mms4_des_dist_brst18_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 1230 eV (E20/even) [mms4_des_dist_brst20_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 1400 eV (E20/odd) [mms4_des_dist_brst20_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~1310 eV (E20 even-odd) [mms4_des_dist_brst20_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1230 eV (E20/even) [mms4_des_dist_brst20_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1400 eV (E20/odd) [mms4_des_dist_brst20_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 2600 eV (E23/even) [mms4_des_dist_brst23_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 2950 eV (E23/odd) [mms4_des_dist_brst23_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~2770 eV (E23 even-odd) [mms4_des_dist_brst23_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2600 eV (E23/even) [mms4_des_dist_brst23_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2950 eV (E23/odd) [mms4_des_dist_brst23_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 5490 eV (E26/even) [mms4_des_dist_brst26_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 6210 eV (E26/odd) [mms4_des_dist_brst26_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~5840 eV (E26 even-odd) [mms4_des_dist_brst26_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5490 eV (E26/even) [mms4_des_dist_brst26_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 6210 eV (E26/odd) [mms4_des_dist_brst26_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 24400 eV (E32/even) [mms4_des_dist_brst32_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES burst sky-map instrument distribution - 27600 eV (E32/odd) [mms4_des_dist_brst32_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~26000 eV (E32 even-odd) [mms4_des_dist_brst32_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 24400 eV (E32/even) [mms4_des_dist_brst32_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 27600 eV (E32/odd) [mms4_des_dist_brst32_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[List/Create only in CDAWeb] 1-sigma error: MMS4 FPI/DES burst sky-map instrument distribution [mms4_des_disterr_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES vector of data-quality indicators at burst-start time [mms4_des_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS4 FPI/DES compression lossless/lossy indicator at survey-start time [mms4_des_compressionloss_brst]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

---> MMS4 FPI/DES step table parity, this burst [mms4_des_steptable_parity_brst]

FPI/DES alternates between two tables, designated "even" (0) and "odd" (1).

---> MMS4 FPI/DES Del-Phi (obs spin-phase) count at burst-start time [mms4_des_startdelphi_count_brst]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS4 FPI/DES Del-Phi (obs spin-phase) angle at burst-start time [mms4_des_startdelphi_angle_brst]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS4 FPI/DES burst average f1 count values [mms4_des_avgf1counts_brst]

Average f1-count level as a function of energy

MMS4 FPI/DES burst sky-map microsecond offsets from Epoch [mms4_des_steptimeoffsets_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order. Offsets reflect 128 steps over the 30 msec sweep
period. See FPI docs for details.

---> MMS4 FPI/DES sector de-Spin P value, this burst [mms4_des_sector_despinp_brst]

Records P-value used to de-spin this burst sky-map on board.  See FPI docs for
details.

MMS4 FPI/DES burst sky-map instrument azimuthal angles [mms4_des_phi_brst]

see FPI docs for details

MMS FPI/DES burst sky-map parity 0/1 energies [mms4_des_energy_brst]

Energies (parity 0/1) in the 64-step FPI energy table

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MMS4_FPI_BRST_L2_DES-MOMS (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DES/Burst/Level2/Moments/PT0.03S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode.  Data are also made available at survey (4.5
s, etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked.  Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available.  This product contains results from
integrating the standard moments of phase-space distributions formed from the
indicated data type (DES/DIS burst, FS or SS).  For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS4_FPI_BRST_L2_DES-PARTMOMS (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DES/Burst/Level2/PartialMoments/PT0.03S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s,
etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked. Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available. This product contains partial moments that
come from performing the standard moment integrals over a limited portion of
velocity space. The resulting quantities are named similarly to their
corresponding standard moments, but are decorated with 'part' to differentiate.
For example, density_part is the density moment integrated from a particular
energy step to infinity. These partial moments are formed from the indicated
data type (DES/DIS burst, FS or SS). For convenience, some additional parameters
are included to augment those most commonly found in a moments product of this
sort, plus time-stamps and other annotation characterizing the state of the
instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DES vector of data-quality indicators at burst-start time [mms4_des_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of brst l2pre
magnetic field, Bit-9 = srvy l2pre magnetic field used instead of brst l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS4 FPI/DES partial electron number density during this burst [mms4_des_numberdensity_part_brst]

MMS4 FPI/DES partial electron bulk-velocity vector in DBCS during this burst [mms4_des_bulkv_part_dbcs_brst]

MMS4 FPI/DES partial electron bulk-velocity vector in GSE during this burst [mms4_des_bulkv_part_gse_brst]

MMS4 FPI/DES partial electron pressure tensor in DBCS during this burst [mms4_des_prestensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES partial electron pressure tensor in GSE during this burst [mms4_des_prestensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES partial electron temperature tensor in DBCS during this burst [mms4_des_temptensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES partial electron temperature tensor in GSE during this burst [mms4_des_temptensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES partial electron parallel temperature during this burst [mms4_des_temppara_part_brst]

MMS4 FPI/DES partial electron perpendicular temperature during this burst [mms4_des_tempperp_part_brst]

MMS4 FPI/DES recommended energy index during this burst [mms4_des_part_index_brst]

Recommended energy index during this burst

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MMS4_FPI_BRST_L2_DIS-DIST (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DIS/Burst/Level2/Distribution/PT0.15S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data are taken at burst (30/150 ms for DES/DIS)
resolution in this mode.  Data are also made available at survey (4.5 s, etc)
resolution; these form a separate product from this.  Per mission design, not
all burst-resolution data are downlinked.  This product contains phase-space
distribution maps of those burst-resolution data selected for downlink.  In
particular, the (highest possible quality at the time of release)
corrected/converted "Burst SkyMap" distributions are reported with time-stamps
and other annotation characterizing the state of the instrument system at the
indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

[CDAWeb List/Download/Create ONLY] MMS4 FPI/DIS burst sky-map instrument distribution [mms4_dis_dist_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 10.6 eV (E1/even) [mms4_dis_dist_brst1_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 12.0 eV (E1/odd) [mms4_dis_dist_brst1_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~11.3 eV (E1 even-odd) [mms4_dis_dist_brst1_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 10.6 eV (E1/even) [mms4_dis_dist_brst1_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 12.0 eV (E1/odd) [mms4_dis_dist_brst1_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 37.2 eV (E6/even) [mms4_dis_dist_brst6_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 42.1 eV (E6/odd) [mms4_dis_dist_brst6_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~39.6 eV (E6 even-odd) [mms4_dis_dist_brst6_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 37.2 eV (E6/even) [mms4_dis_dist_brst6_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 42.1 eV (E6/odd) [mms4_dis_dist_brst6_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 78.8 eV (E9/even) [mms4_dis_dist_brst9_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 89.3 eV (E9/odd) [mms4_dis_dist_brst9_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~83.9 eV (E9 even-odd) [mms4_dis_dist_brst9_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 78.8 eV (E9/even) [mms4_dis_dist_brst9_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 89.3 eV (E9/odd) [mms4_dis_dist_brst9_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 167 eV (E12/even) [mms4_dis_dist_brst12_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 189 eV (E12/odd) [mms4_dis_dist_brst12_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~178 eV (E12 even-odd) [mms4_dis_dist_brst12_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 167 eV (E12/even) [mms4_dis_dist_brst12_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 189 eV (E12/odd) [mms4_dis_dist_brst12_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 275 eV (E14/even) [mms4_dis_dist_brst14_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 312 eV (E14/odd) [mms4_dis_dist_brst14_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~293 eV (E14 even-odd) [mms4_dis_dist_brst14_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 275 eV (E14/even) [mms4_dis_dist_brst14_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 312 eV (E14/odd) [mms4_dis_dist_brst14_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 455 eV (E16/even) [mms4_dis_dist_brst16_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 515 eV (E16/odd) [mms4_dis_dist_brst16_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~484 eV (E16 even-odd) [mms4_dis_dist_brst16_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 455 eV (E16/even) [mms4_dis_dist_brst16_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 515 eV (E16/odd) [mms4_dis_dist_brst16_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 750 eV (E18/even) [mms4_dis_dist_brst18_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 850 eV (E18/odd) [mms4_dis_dist_brst18_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~800 eV (E18 even-odd) [mms4_dis_dist_brst18_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 750 eV (E18/even) [mms4_dis_dist_brst18_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 850 eV (E18/odd) [mms4_dis_dist_brst18_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 1240 eV (E20/even) [mms4_dis_dist_brst20_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 1400 eV (E20/odd) [mms4_dis_dist_brst20_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~1320 eV (E20 even-odd) [mms4_dis_dist_brst20_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1240 eV (E20/even) [mms4_dis_dist_brst20_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1400 eV (E20/odd) [mms4_dis_dist_brst20_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 2620 eV (E23/even) [mms4_dis_dist_brst23_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 2970 eV (E23/odd) [mms4_dis_dist_brst23_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~2800 eV (E23 even-odd) [mms4_dis_dist_brst23_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2620 eV (E23/even) [mms4_dis_dist_brst23_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2970 eV (E23/odd) [mms4_dis_dist_brst23_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 5560 eV (E26/even) [mms4_dis_dist_brst26_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 6300 eV (E26/odd) [mms4_dis_dist_brst26_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~5920 eV (E26 even-odd) [mms4_dis_dist_brst26_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5560 eV (E26/even) [mms4_dis_dist_brst26_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 6300 eV (E26/odd) [mms4_dis_dist_brst26_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 25000 eV (E32/even) [mms4_dis_dist_brst32_even]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS burst sky-map instrument distribution - 28300 eV (E32/odd) [mms4_dis_dist_brst32_odd]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - ~26600 eV (E32 even-odd) [mms4_dis_dist_brst32_evenodd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 25000 eV (E32/even) [mms4_dis_dist_brst32_even_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 28300 eV (E32/odd) [mms4_dis_dist_brst32_odd_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[List/Create only in CDAWeb] 1-sigma error: MMS4 FPI/DIS burst sky-map instrument distribution [mms4_dis_disterr_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS vector of data-quality indicators at burst-start time [mms4_dis_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS4 FPI/DIS compression lossless/lossy indicator at survey-start time [mms4_dis_compressionloss_brst]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

---> MMS4 FPI/DIS step table parity, this burst [mms4_dis_steptable_parity_brst]

FPI/DIS alternates between two tables, designated "even" (0) and "odd" (1).

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) count at burst-start time [mms4_dis_startdelphi_count_brst]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at burst-start time [mms4_dis_startdelphi_angle_brst]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS4 FPI/DIS burst average f1 count values [mms4_dis_avgf1counts_brst]

Average f1-count level as a function of energy

MMS4 FPI/DIS burst sky-map microsecond offsets from Epoch [mms4_dis_steptimeoffsets_brst]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order. Offsets reflect 128 steps over the 150 msec sweep
period. See FPI docs for details.

---> MMS4 FPI/DIS sector de-Spin P value, this burst [mms4_dis_sector_despinp_brst]

Records P-value used to de-spin this burst sky-map on board.  See FPI docs for
details.

MMS4 FPI/DIS burst sky-map instrument azimuthal angles [mms4_dis_phi_brst]

see FPI docs for details

MMS FPI/DIS burst sky-map parity 0/1 energies [mms4_dis_energy_brst]

Energies (parity 0/1) in the 64-step FPI energy table

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MMS4_FPI_BRST_L2_DIS-MOMS (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DIS/Burst/Level2/Moments/PT0.15S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode.  Data are also made available at survey (4.5
s, etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked.  Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available.  This product contains results from
integrating the standard moments of phase-space distributions formed from the
indicated data type (DES/DIS burst, FS or SS).  For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS4_FPI_BRST_L2_DIS-PARTMOMS (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DIS/Burst/Level2/PartialMoments/PT0.15S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s,
etc) resolution.  Per mission design, not all burst-resolution data are
downlinked, but all survey data are downlinked. Planning around calibration
activities, avoidance of Earth radiation belts, etc, when possible, FPI usually
operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s
resolution survey data are available. This product contains partial moments that
come from performing the standard moment integrals over a limited portion of
velocity space. The resulting quantities are named similarly to their
corresponding standard moments, but are decorated with 'part' to differentiate.
For example, density_part is the density moment integrated from a particular
energy step to infinity. These partial moments are formed from the indicated
data type (DES/DIS burst, FS or SS). For convenience, some additional parameters
are included to augment those most commonly found in a moments product of this
sort, plus time-stamps and other annotation characterizing the state of the
instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DIS vector of data-quality indicators at burst-start time [mms4_dis_errorflags_brst]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of brst l2pre
magnetic field, Bit-9 = srvy l2pre magnetic field used instead of brst l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS4 FPI/DIS partial ion number density during this burst [mms4_dis_numberdensity_part_brst]

MMS4 FPI/DIS partial ion bulk-velocity vector in DBCS during this burst [mms4_dis_bulkv_part_dbcs_brst]

MMS4 FPI/DIS partial ion bulk-velocity vector in GSE during this burst [mms4_dis_bulkv_part_gse_brst]

MMS4 FPI/DIS partial ion pressure tensor in DBCS during this burst [mms4_dis_prestensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS partial ion pressure tensor in GSE during this burst [mms4_dis_prestensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS partial ion temperature tensor in DBCS during this burst [mms4_dis_temptensor_part_dbcs_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS partial ion temperature tensor in GSE during this burst [mms4_dis_temptensor_part_gse_brst]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS partial ion parallel temperature during this burst [mms4_dis_temppara_part_brst]

MMS4 FPI/DIS partial ion perpendicular temperature during this burst [mms4_dis_tempperp_part_brst]

MMS4 FPI/DIS recommended energy index during this burst [mms4_dis_part_index_brst]

Recommended energy index during this burst

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MMS4_FPI_FAST_L2_DES-DIST (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DES/Fast/Level2/Distribution/PT4.5S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data taken at burst (30/150 ms for DES/DIS)
resolution are aggregated on board and made available at survey (4.5 s)
resolution in this mode.  This product contains phase-space distribution maps of
results from surveying the high-resolution observations during each 4.5 s
period.  In particular, the (highest possible quality at the time of release)
corrected/converted "Fast Survey SkyMap" distributions are reported with
time-stamps and other annotation characterizing the state of the instrument
system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DES fast sky-map instrument distribution - 11.6 eV (E1) using averaged even/odd steps [mms4_des_dist_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 11.6 eV [mms4_des_dist_fast1_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES fast sky-map instrument distribution - 40.4 eV (E6) using averaged even/odd steps [mms4_des_dist_fast6]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 40.4 eV [mms4_des_dist_fast6_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES fast sky-map instrument distribution - 85.1 eV (E9) using averaged even/odd steps [mms4_des_dist_fast9]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 85.1 eV [mms4_des_dist_fast9_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES fast sky-map instrument distribution - 179 eV (E12) using averaged even/odd steps [mms4_des_dist_fast12]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 179 eV [mms4_des_dist_fast12_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES fast sky-map instrument distribution - 295 eV (E14) using averaged even/odd steps [mms4_des_dist_fast14]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 295 eV [mms4_des_dist_fast14_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES fast sky-map instrument distribution - 485 eV (E16) using averaged even/odd steps [mms4_des_dist_fast16]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 485 eV [mms4_des_dist_fast16_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES fast sky-map instrument distribution - 798 eV (E18) using averaged even/odd steps [mms4_des_dist_fast18]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 798 eV [mms4_des_dist_fast18_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES fast sky-map instrument distribution - 1310 eV (E20) using averaged even/odd steps [mms4_des_dist_fast20]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1310 eV [mms4_des_dist_fast20_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES fast sky-map instrument distribution - 2770 eV (E23) using averaged even/odd steps [mms4_des_dist_fast23]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2770 eV [mms4_des_dist_fast23_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES fast sky-map instrument distribution - 5840 eV (E26) using averaged even/odd steps [mms4_des_dist_fast26]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5840 eV [mms4_des_dist_fast26_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES fast sky-map instrument distribution - 26000 eV (E32) using averaged even/odd steps [mms4_des_dist_fast32]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 26000 eV [mms4_des_dist_fast32_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[Only List/Create in CDAWeb] MMS4 FPI/DES fast sky-map instrument distribution 1-sigma error [mms4_des_disterr_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES vector of data-quality indicators at fast survey-start time - 32-bit error flags [mms4_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS4 FPI/DES compression lossless/lossy indicator at survey-start time [mms4_des_compressionloss_fast]

FPI/DES compression loss indicator,0=lossless, 1=lossy

---> MMS4 FPI/DES Del-Phi (obs spin-phase) count at fast survey-start time [mms4_des_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS4 FPI/DES Del-Phi (obs spin-phase) angle at fast survey-start time [mms4_des_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS4 FPI/DES fast survey average f1 count values [mms4_des_avgf1counts_fast]

Average f1-count level as a function of energy

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MMS4_FPI_FAST_L2_DES-MOMS (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DES/Fast/Level2/Moments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution.  Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This moments product
contains results from integrating the standard moments of phase-space
distributions formed from the indicated data type (DES/DIS burst, FS or SS). For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotation characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

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MMS4_FPI_FAST_L2_DES-MOMSAUX

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DES vector of data-quality indicators at survey-start time [mms4_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS4 FPI/DES partial electron number density during this survey [mms4_des_numberdensity_part_fast]

MMS4 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms4_des_bulkv_part_dbcs_fast]

MMS4 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms4_des_bulkv_part_gse_fast]

MMS4 FPI/DES partial electron pressure tensor in DBCS during this survey [mms4_des_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES partial electron pressure tensor in GSE during this survey [mms4_des_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES partial electron temperature tensor in DBCS during this survey [mms4_des_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES partial electron temperature tensor in GSE during this survey [mms4_des_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES partial electron parallel temperature during this survey [mms4_des_temppara_part_fast]

MMS4 FPI/DES partial electron perpendicular temperature during this survey [mms4_des_tempperp_part_fast]

MMS4 FPI/DES recommended energy index for partial moments during this survey [mms4_des_part_index_fast]

Recommended energy index during this survey

MMS4 FPI/DES compression lossless/lossy indicator at survey-start time [mms4_des_compressionloss_fast]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS4 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms4_des_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS4 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms4_des_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS4 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms4_des_pitchangdist_lowen_fast]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size: 6
deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS4 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms4_des_pitchangdist_miden_fast]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS4 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms4_des_pitchangdist_highen_fast]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS4 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms4_des_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS4 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms4_des_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS4 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms4_des_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS4 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms4_des_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS4 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms4_des_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS4 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms4_des_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS4 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms4_des_energyspectr_par_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS4 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms4_des_energyspectr_anti_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS4 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms4_des_energyspectr_perp_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS4 FPI/DES omni-directional electron energy spectrum during this survey [mms4_des_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS4 FPI/DES electron number density during this survey [mms4_des_numberdensity_fast]

MMS4 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms4_des_densityextrapolation_low_fast]

MMS4 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms4_des_densityextrapolation_high_fast]

MMS4 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms4_des_bulkv_dbcs_fast]

MMS4 FPI/DES electron bulk-velocity estimated spintone vector in DBCS during this survey [mms4_des_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS4 FPI/DES electron bulk-velocity vector in GSE during this survey [mms4_des_bulkv_gse_fast]

MMS4 FPI/DES electron bulk-velocity estimated spintone vector in GSE during this survey [mms4_des_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS4 FPI/DES electron pressure tensor in DBCS during this survey [mms4_des_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES electron pressure tensor in GSE during this survey [mms4_des_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES electron temperature tensor in DBCS during this survey [mms4_des_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES electron temperature tensor in GSE during this survey [mms4_des_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES electron heat-flux vector in DBCS during this survey [mms4_des_heatq_dbcs_fast]

MMS4 FPI/DES electron heat-flux vector in GSE during this survey [mms4_des_heatq_gse_fast]

MMS4 FPI/DES electron parallel temperature during this BP [mms4_des_temppara_fast]

MMS4 FPI/DES electron perpendicular temperature during this BP [mms4_des_tempperp_fast]

MMS4 FPI/DES S/C potential mean [mms4_des_scpot_mean_fast]

Average spacecraft potential during this FP used to shift the measure energies.

MMS4 FPI/DES S/C potential max [mms4_des_scpot_max_fast]

Maximum spacecraft potential during this FP used to exclude energies containing
spacecraft photoelectron fluxes.

MMS4 FPI/DES Mag data X,Y,Z,Norm DSC components [nT] at survey-start time [mms4_des_fpibentpipe_dsc_fast]

X, Y, Z are unit vector components.

Magnetic field vector X,Y,Z, and magnitude B [mms4_des_fpib_gse_srvy_fast]

Averaged survey magnetic field data during this FP

Magnetic field vector X,Y,Z, and magnitude B [mms4_des_fpib_dmpa_srvy_fast]

Averaged survey magnetic field data during this FP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms4_des_pos_gse_fast]

Position in GSM coordinates, 30 second [mms4_des_pos_gsm_fast]

MMS4 number density integrands [mms4_des_numberdensity_int_fast]

Integrand terms used in normalized energy integration for number density

number flux [mms4_des_numberflux_int_dbcs_fast]

Integrand terms used in normalized energy integration for number flux

MMS4 pressure tensor integrands [mms4_des_prestensor_int_dbcs_fast]

Integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms4_des_ugrid_int_fast]

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MMS4_FPI_FAST_L2_DES-PARTMOMS (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DES/Fast/Level2/PartialMoments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DES vector of data-quality indicators at survey-start time [mms4_des_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only)

MMS4 FPI/DES partial electron number density during this survey [mms4_des_numberdensity_part_fast]

MMS4 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms4_des_bulkv_part_dbcs_fast]

MMS4 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms4_des_bulkv_part_gse_fast]

MMS4 FPI/DES partial electron pressure tensor in DBCS during this survey [mms4_des_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES partial electron pressure tensor in GSE during this survey [mms4_des_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES partial electron temperature tensor in DBCS during this survey [mms4_des_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES partial electron temperature tensor in GSE during this survey [mms4_des_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES partial electron parallel temperature during this survey [mms4_des_temppara_part_fast]

MMS4 FPI/DES partial electron perpendicular temperature during this survey [mms4_des_tempperp_part_fast]

MMS4 FPI/DES recommended energy index during this survey [mms4_des_part_index_fast]

Recommended energy index during this survey

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MMS4_FPI_FAST_L2_DIS-DIST (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DIS/Fast/Level2/Distribution/PT4.5S)

Description

FPI usually operates in Fast Survey Mode in the MMS Region Of Interest (ROI) for
the current Mission Phase.  Data taken at burst (30/150 ms for DES/DIS)
resolution are aggregated on board and made available at survey (4.5 s)
resolution in this mode.  This product contains phase-space distribution maps of
results from surveying the high-resolution observations during each 4.5 s
period.  In particular, the (highest possible quality at the time of release)
corrected/converted "Fast Survey SkyMap" distributions are reported with
time-stamps and other annotation characterizing the state of the instrument
system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DIS fast sky-map instrument distribution - 11.3 eV (E1) using averaged even/odd steps [mms4_dis_dist_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 11.3 eV [mms4_dis_dist_fast1_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS fast sky-map instrument distribution - 39.6 eV (E6) using averaged even/odd steps [mms4_dis_dist_fast6]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 39.6 eV [mms4_dis_dist_fast6_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS fast sky-map instrument distribution - 83.9 eV (E9 using averaged even/odd steps) [mms4_dis_dist_fast9]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 83.9 eV [mms4_dis_dist_fast9_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS fast sky-map instrument distribution - 178 eV (E12) using averaged even/odd steps [mms4_dis_dist_fast12]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 178 eV [mms4_dis_dist_fast12_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS fast sky-map instrument distribution - 293 eV (E14) using averaged even/odd steps [mms4_dis_dist_fast14]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 293 eV [mms4_dis_dist_fast14_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS fast sky-map instrument distribution - 484 eV (E16) using averaged even/odd steps [mms4_dis_dist_fast16]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 484 eV [mms4_dis_dist_fast16_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS fast sky-map instrument distribution - 799 eV (E18) using averaged even/odd steps [mms4_dis_dist_fast18]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 799 eV [mms4_dis_dist_fast18_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS fast sky-map instrument distribution - 1320 eV (E20) using averaged even/odd steps [mms4_dis_dist_fast20]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 1320 eV [mms4_dis_dist_fast20_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS fast sky-map instrument distribution - 2800 eV (E23) using averaged even/odd steps [mms4_dis_dist_fast23]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 2800 eV [mms4_dis_dist_fast23_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS fast sky-map instrument distribution - 5920 eV (E26) using averaged even/odd steps [mms4_dis_dist_fast26]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 5920 eV [mms4_dis_dist_fast26_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS fast sky-map instrument distribution - 26600 eV (E32) using averaged even/odd steps [mms4_dis_dist_fast32]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

---> Movie - 26600 eV [mms4_dis_dist_fast32_movie]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

[Only List/Create in CDAWeb] MMS4 FPI/DIS fast sky-map instrument distribution 1-sigma error [mms4_dis_disterr_fast]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=31 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS vector of data-quality indicators at fast survey-start time - 32-bit error flags [mms4_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap

---> MMS4 FPI/DIS compression lossless/lossy indicator at survey-start time [mms4_dis_compressionloss_fast]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) count at fast survey-start time [mms4_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase count indicates
obs +X-axis aligned with Sun.

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at fast survey-start time [mms4_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with Sun.

MMS4 FPI/DIS fast survey average f1 count values [mms4_dis_avgf1counts_fast]

Average f1-count level as a function of energy

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MMS4_FPI_FAST_L2_DIS-MOMS (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DIS/Fast/Level2/Moments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution.  Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This moments product
contains results from integrating the standard moments of phase-space
distributions formed from the indicated data type (DES/DIS burst, FS or SS). For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotation characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DIS vector of data-quality indicators at survey-start time [mms4_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation, Bit-14 =
high MMS3 spintone due to DIS008 anomaly

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms4_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

---> MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms4_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS4 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms4_dis_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

---> MMS4 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms4_dis_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

---> MMS4 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms4_dis_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

---> MMS4 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms4_dis_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

---> MMS4 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms4_dis_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

---> MMS4 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms4_dis_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS4 FPI/DIS omni-directional ion energy spectrum during this survey [mms4_dis_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS4 FPI/DIS ion background energy during this survey [mms4_dis_spectr_bg_fast]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS4 FPI/DIS ion background number density during this survey [mms4_dis_numberdensity_bg_fast]

Background number density derived via integration of the estimated background
differential energy flux.

MMS4 FPI/DIS ion number density during this survey [mms4_dis_numberdensity_fast]

---> (no error bars displayed) MMS4 FPI/DIS ion number density during this survey [mms4_dis_numberdensity_fast_noerr]

MMS4 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms4_dis_densityextrapolation_low_fast]

MMS4 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms4_dis_densityextrapolation_high_fast]

MMS4 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms4_dis_bulkv_dbcs_fast]

---> (no error bars displayed) MMS4 FPI/DIS ion bulk-velocity DBCS vector during this survey [mms4_dis_bulkv_dbcs_fast_noerr]

MMS4 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey [mms4_dis_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS4 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms4_dis_bulkv_gse_fast]

MMS4 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey [mms4_dis_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

---> (no error bars displayed) MMS4 FPI/DIS ion bulk-velocity GSE vector during this survey [mms4_dis_bulkv_gse_fast_noerr]

MMS4 FPI/DIS ion pressure tensor in DBCS during this survey [mms4_dis_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS ion pressure tensor in GSE during this survey [mms4_dis_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS ion background pressure during this survey [mms4_dis_pres_bg_fast]

MMS4 FPI/DIS ion temperature tensor in DBCS during this survey [mms4_dis_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS ion temperature tensor in GSE during this survey [mms4_dis_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS ion heat-flux vector in DBCS during this survey [mms4_dis_heatq_dbcs_fast]

MMS4 FPI/DIS ion heat-flux vector in GSE during this survey [mms4_dis_heatq_gse_fast]

MMS4 FPI/DIS ion parallel temperature during this BP [mms4_dis_temppara_fast]

MMS4 FPI/DIS ion perpendicular temperature during this BP [mms4_dis_tempperp_fast]

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MMS4_FPI_FAST_L2_DIS-MOMSAUX

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DIS vector of data-quality indicators at survey-start time [mms4_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS4 FPI/DIS partial ion number density during this survey [mms4_dis_numberdensity_part_fast]

MMS4 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms4_dis_bulkv_part_dbcs_fast]

MMS4 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms4_dis_bulkv_part_gse_fast]

MMS4 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms4_dis_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS partial ion pressure tensor in GSE during this survey [mms4_dis_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms4_dis_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS partial ion temperature tensor in GSE during this survey [mms4_dis_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS partial ion parallel temperature during this survey [mms4_dis_temppara_part_fast]

MMS4 FPI/DIS partial ion perpendicular temperature during this survey [mms4_dis_tempperp_part_fast]

MMS4 FPI/DIS recommended energy index for partial moments during this survey [mms4_dis_part_index_fast]

Recommended energy index during this survey

MMS4 FPI/DIS compression lossless/lossy indicator at survey-start time [mms4_dis_compressionloss_fast]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS4 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms4_dis_startdelphi_count_fast]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms4_dis_startdelphi_angle_fast]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS4 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms4_dis_energyspectr_px_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS4 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms4_dis_energyspectr_mx_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS4 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms4_dis_energyspectr_py_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS4 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms4_dis_energyspectr_my_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS4 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms4_dis_energyspectr_pz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS4 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms4_dis_energyspectr_mz_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS4 FPI/DIS omni-directional ion energy spectrum during this survey [mms4_dis_energyspectr_omni_fast]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS4 FPI/DIS ion background energy during this survey [mms4_dis_spectr_bg_fast]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS4 FPI/DIS ion background number density during this survey [mms4_dis_numberdensity_bg_fast]

Background number density derived via integration of the estimated background
differential energy flux.

MMS4 FPI/DIS ion number density during this survey [mms4_dis_numberdensity_fast]

MMS4 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms4_dis_densityextrapolation_low_fast]

MMS4 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms4_dis_densityextrapolation_high_fast]

MMS4 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms4_dis_bulkv_dbcs_fast]

MMS4 FPI/DIS ion bulk-velocity estimated spintone vector in DBCS during this survey [mms4_dis_bulkv_spintone_dbcs_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS4 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms4_dis_bulkv_gse_fast]

MMS4 FPI/DIS ion bulk-velocity estimated spintone vector in GSE during this survey [mms4_dis_bulkv_spintone_gse_fast]

Estimated systematic error (positive or negative) in spin-plane bulk velocity
(km/s) due to imperfect sensor suite flat-fielding. This can be subtracted from
bulk velocity to obtain the corrected velocity vector.

MMS4 FPI/DIS ion pressure tensor in DBCS during this survey [mms4_dis_prestensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS ion pressure tensor in GSE during this survey [mms4_dis_prestensor_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS ion background pressure during this survey [mms4_dis_pres_bg_fast]

MMS4 FPI/DIS ion temperature tensor in DBCS during this survey [mms4_dis_temptensor_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS ion temperature tensor in GSE during this survey [mms4_dis_temptensor_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS ion heat-flux vector in DBCS during this survey [mms4_dis_heatq_dbcs_fast]

MMS4 FPI/DIS ion heat-flux vector in GSE during this survey [mms4_dis_heatq_gse_fast]

MMS4 FPI/DIS ion parallel temperature during this BP [mms4_dis_temppara_fast]

MMS4 FPI/DIS ion perpendicular temperature during this BP [mms4_dis_tempperp_fast]

MMS4 FPI/DIS S/C potential mean [mms4_dis_scpot_mean_fast]

Average spacecraft potential during this FP used to shift the measure energies.

MMS4 FPI/DIS S/C potential max [mms4_dis_scpot_max_fast]

Maximum spacecraft potential during this FP used to exclude energies containing
spacecraft photoelectron fluxes.

MMS4 FPI/DIS Mag data X,Y,Z,Norm DSC components [nT] at survey-start time [mms4_dis_fpibentpipe_dsc_fast]

X, Y, Z are unit vector components.

Magnetic field vector X,Y,Z, and magnitude B [mms4_dis_fpib_gse_srvy_fast]

Averaged survey magnetic field data during this FP

Magnetic field vector X,Y,Z, and magnitude B [mms4_dis_fpib_dmpa_srvy_fast]

Averaged survey magnetic field data during this FP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms4_dis_pos_gse_fast]

Position in GSM coordinates, 30 second [mms4_dis_pos_gsm_fast]

MMS4 number density integrands [mms4_dis_numberdensity_int_fast]

integrand terms used in normalized energy integration for number density

number flux [mms4_dis_numberflux_int_dbcs_fast]

integrand terms used in normalized energy integration for number flux

MMS4 pressure tensor integrands [mms4_dis_prestensor_int_dbcs_fast]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms4_dis_ugrid_int_fast]

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MMS4_FPI_FAST_L2_DIS-PARTMOMS (spase://NASA/NumericalData/MMS/4/FastPlasmaInvestigation/DIS/Fast/Level2/PartialMoments/PT4.5S)

Description

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest
(ROI) for the current Mission Phase. Data are taken at burst (30/150 ms for
DES/DIS) resolution in this mode. Data are also made available at survey (4.5 s)
resolution. Per mission design, not all burst-resolution data are downlinked,
but all survey data are downlinked. Planning around calibration activities,
avoidance of Earth radiation belts, etc, when possible, FPI usually operates in
Slow Survey (SS) Mode (60 s resolution) outside of ROI. This product contains
partial moments that come from performing the standard moment integrals over a
limited portion of velocity space. The resulting quantities are named similarly
to their corresponding standard moments, but are decorated with 'part' to
differentiate. For example, density_part is the density moment integrated from a
particular energy step to infinity. These partial moments are formed from the
indicated data type (DES/DIS burst, FS or SS). For convenience, some additional
parameters are included to augment those most commonly found in a moments
product of this sort, plus time-stamps and other annotation characterizing the
state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DIS vector of data-quality indicators at survey-start time [mms4_dis_errorflags_fast]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = bentPipe magnetic field used instead of srvy l2pre
magnetic field, Bit-10 = no internally generated photoelectron correction
applied, Bit-11 = compression pipeline error, Bit-12 = spintone calculation
error (DBCS only), Bit-13 = significant (>=20%) penetrating radiation

MMS4 FPI/DIS partial ion number density during this survey [mms4_dis_numberdensity_part_fast]

MMS4 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms4_dis_bulkv_part_dbcs_fast]

MMS4 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms4_dis_bulkv_part_gse_fast]

MMS4 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms4_dis_prestensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS partial ion pressure tensor in GSE during this survey [mms4_dis_prestensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms4_dis_temptensor_part_dbcs_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS partial ion temperature tensor in GSE during this survey [mms4_dis_temptensor_part_gse_fast]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS partial ion parallel temperature during this survey [mms4_dis_temppara_part_fast]

MMS4 FPI/DIS partial ion perpendicular temperature during this survey [mms4_dis_tempperp_part_fast]

MMS4 FPI/DIS recommended energy index during this survey [mms4_dis_part_index_fast]

Recommended energy index during this survey

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MMS4_FPI_SLOW_L2_DES-DIST

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode.  This product contains phase-space distribution maps of those
survey-resolution data from Slow Mode.  In particular, the (highest possible
quality at the time of release) corrected/converted "Slow Survey SkyMap"
distributions are reported with time-stamps and other annotation characterizing
the state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DES vector of data-quality indicators at survey-start time [mms4_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = compression pipeline error

MMS4 FPI/DES compression lossless/lossy indicator at survey-start time [mms4_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS4 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms4_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS4 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms4_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS4 FPI/DES Slow Survey sky-map instrument distribution [mms4_des_dist_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES Slow Survey sky-map instrument distribution 1-sigma error [mms4_des_disterr_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DES slow survey average f1 count values [mms4_des_avgf1counts_slow]

Average f1-count level as a function of energy

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MMS4_FPI_SLOW_L2_DES-MOMS

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DES vector of data-quality indicators at survey-start time [mms4_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only)

MMS4 FPI/DES compression lossless/lossy indicator at survey-start time [mms4_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS4 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms4_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS4 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms4_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS4 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms4_des_pitchangdist_lowen_slow]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS4 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms4_des_pitchangdist_miden_slow]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS4 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms4_des_pitchangdist_highen_slow]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS4 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms4_des_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS4 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms4_des_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS4 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms4_des_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS4 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms4_des_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS4 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms4_des_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS4 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms4_des_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS4 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms4_des_energyspectr_par_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS4 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms4_des_energyspectr_anti_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS4 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms4_des_energyspectr_perp_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS4 FPI/DES omni-directional electron energy spectrum during this survey [mms4_des_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS4 FPI/DES electron number density during this survey [mms4_des_numberdensity_slow]

MMS4 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms4_des_densityextrapolation_low_slow]

MMS4 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms4_des_densityextrapolation_high_slow]

MMS4 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms4_des_bulkv_dbcs_slow]

MMS4 FPI/DES electron bulk-velocity vector in GSE during this survey [mms4_des_bulkv_gse_slow]

MMS4 FPI/DES electron pressure tensor in DBCS during this survey [mms4_des_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES electron pressure tensor in GSE during this survey [mms4_des_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES electron temperature tensor in DBCS during this survey [mms4_des_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES electron temperature tensor in GSE during this survey [mms4_des_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES electron heat-flux vector in DBCS during this survey [mms4_des_heatq_dbcs_slow]

MMS4 FPI/DES electron heat-flux vector in GSE during this survey [mms4_des_heatq_gse_slow]

MMS4 FPI/DES electron parallel temperature during this BP [mms4_des_temppara_slow]

MMS4 FPI/DES electron perpendicular temperature during this BP [mms4_des_tempperp_slow]

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MMS4_FPI_SLOW_L2_DES-MOMSAUX

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DES vector of data-quality indicators at survey-start time [mms4_des_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DES < 0.05 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only)

MMS4 FPI/DES partial electron number density during this survey [mms4_des_numberdensity_part_slow]

MMS4 FPI/DES partial electron bulk-velocity vector in DBCS during this survey [mms4_des_bulkv_part_dbcs_slow]

MMS4 FPI/DES partial electron bulk-velocity vector in GSE during this survey [mms4_des_bulkv_part_gse_slow]

MMS4 FPI/DES partial electron pressure tensor in DBCS during this survey [mms4_des_prestensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES partial electron pressure tensor in GSE during this survey [mms4_des_prestensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES partial electron temperature tensor in DBCS during this survey [mms4_des_temptensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES partial electron temperature tensor in GSE during this survey [mms4_des_temptensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES partial electron parallel temperature during this survey [mms4_des_temppara_part_slow]

MMS4 FPI/DES partial electron perpendicular temperature during this survey [mms4_des_tempperp_part_slow]

MMS4 FPI/DES recommended energy index for partial moments during this survey [mms4_des_part_index_slow]

Recommended energy index during this survey

MMS4 FPI/DES compression lossless/lossy indicator at survey-start time [mms4_des_compressionloss_slow]

FPI/DES compression loss indicator, 0=lossless, 1=lossy

MMS4 FPI/DES Del-Phi (obs spin-phase) count at survey-start time [mms4_des_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS4 FPI/DES Del-Phi (obs spin-phase) angle at survey-start time [mms4_des_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS4 FPI/DES electron pitch-angle distribution for "low" energies during this survey [mms4_des_pitchangdist_lowen_slow]

Low energy bin: energy steps 0-10 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS4 FPI/DES electron pitch-angle distribution for "mid" energies during this survey [mms4_des_pitchangdist_miden_slow]

Mid energy bin: energy steps 11-20 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS4 FPI/DES electron pitch-angle distribution for "high" energies during this survey [mms4_des_pitchangdist_highen_slow]

High energy bin: energy steps 21-31 (of total steps 0-31). Pitch-angle bin size:
12 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not
shifted by the bulk velocity.

MMS4 FPI/DES electron energy spectrum "near" +X_DBCS during this survey [mms4_des_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS4 FPI/DES electron energy spectrum "near" -X_DBCS during this survey [mms4_des_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS4 FPI/DES electron energy spectrum "near" +Y_DBCS during this survey [mms4_des_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS4 FPI/DES electron energy spectrum "near" -Y_DBCS during this survey [mms4_des_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS4 FPI/DES electron energy spectrum "near" +Z_DBCS during this survey [mms4_des_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS4 FPI/DES electron energy spectrum "near" -Z_DBCS during this survey [mms4_des_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS4 FPI/DES electron energy parallel to the magnetic field direction during this survey [mms4_des_energyspectr_par_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within 30
degrees of the magnetic field direction.

MMS4 FPI/DES electron energy anti-parallel to the magnetic field direction during this survey [mms4_des_energyspectr_anti_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
150 degrees of the magnetic field direction.

MMS4 FPI/DES electron energy perpendicular to the magnetic field direction during this survey [mms4_des_energyspectr_perp_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction (not instrument look direction) is within
60-120 degrees of the magnetic field direction.

MMS4 FPI/DES omni-directional electron energy spectrum during this survey [mms4_des_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS4 FPI/DES electron number density during this survey [mms4_des_numberdensity_slow]

MMS4 FPI/DES estimated (via extrapolation to 0) contribution to density integral below 10eV [mms4_des_densityextrapolation_low_slow]

MMS4 FPI/DES estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms4_des_densityextrapolation_high_slow]

MMS4 FPI/DES electron bulk-velocity vector in DBCS during this survey [mms4_des_bulkv_dbcs_slow]

MMS4 FPI/DES electron bulk-velocity vector in GSE during this survey [mms4_des_bulkv_gse_slow]

MMS4 FPI/DES electron pressure tensor in DBCS during this survey [mms4_des_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES electron pressure tensor in GSE during this survey [mms4_des_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DES electron temperature tensor in DBCS during this survey [mms4_des_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES electron temperature tensor in GSE during this survey [mms4_des_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DES electron heat-flux vector in DBCS during this survey [mms4_des_heatq_dbcs_slow]

MMS4 FPI/DES electron heat-flux vector in GSE during this survey [mms4_des_heatq_gse_slow]

MMS4 FPI/DES electron parallel temperature during this BP [mms4_des_temppara_slow]

MMS4 FPI/DES electron perpendicular temperature during this BP [mms4_des_tempperp_slow]

MMS4 FPI/DES S/C potential mean [mms4_des_scpot_mean_slow]

Average spacecraft potential during this SP used to shift the measure energies.

MMS4 FPI/DES S/C potential max [mms4_des_scpot_max_slow]

Maximum spacecraft potential during this SP used to exclude energies containing
spacecraft photoelectron fluxes.

Magnetic field vector X,Y,Z, and magnitude B [mms4_des_fpib_gse_srvy_slow]

Averaged survey magnetic field data during this SP

Magnetic field vector X,Y,Z, and magnitude B [mms4_des_fpib_dmpa_srvy_slow]

Averaged survey magnetic field data during this SP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms4_des_pos_gse_slow]

Position in GSM coordinates, 30 second [mms4_des_pos_gsm_slow]

MMS4 number density integrands [mms4_des_numberdensity_int_slow]

integrand terms used in normalized energy integration for number density

number flux [mms4_des_numberflux_int_dbcs_slow]

integrand terms used in normalized energy integration for number flux

MMS4 pressure tensor integrands [mms4_des_prestensor_int_dbcs_slow]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms4_des_ugrid_int_slow]

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MMS4_FPI_SLOW_L2_DIS-DIST

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode.  This product contains phase-space distribution maps of those
survey-resolution data from Slow Mode.  In particular, the (highest possible
quality at the time of release) corrected/converted "Slow Survey SkyMap"
distributions are reported with time-stamps and other annotation characterizing
the state of the instrument system at the indicated time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DIS vector of data-quality indicators at survey-start time [mms4_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = compression pipeline error

MMS4 FPI/DIS compression lossless/lossy indicator at survey-start time [mms4_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS4 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms4_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms4_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS4 FPI/DIS Slow Survey sky-map instrument distribution [mms4_dis_dist_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS Slow Survey sky-map instrument distribution 1-sigma error [mms4_dis_disterr_slow]

Az bin: sector ind=00 looks "after" (spin-phase) Sun, ..., sector ind=15 looks
"before" Sun dir.  Head field-of-view: pixel index=00 looks to zenith, ...,
pixel index=15 looks to nadir.  FPI operations nominally bin data from 64 energy
filters into 32 pairwise energy bins, indexed 0-31.  Nominally, bins are indexed
in increasing energy order.  See FPI docs for details.

MMS4 FPI/DIS slow survey average f1 count values [mms4_dis_avgf1counts_slow]

Average f1-count level as a function of energy

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MMS4_FPI_SLOW_L2_DIS-MOMS

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DIS vector of data-quality indicators at survey-start time [mms4_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only), Bit-13 =
significant (>=20%) penetrating radiation, Bit-14 = high MMS3 spintone due to
DIS008 anomaly

MMS4 FPI/DIS compression lossless/lossy indicator at survey-start time [mms4_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS4 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms4_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms4_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS4 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms4_dis_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS4 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms4_dis_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS4 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms4_dis_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS4 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms4_dis_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS4 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms4_dis_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS4 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms4_dis_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS4 FPI/DIS omni-directional ion energy spectrum during this survey [mms4_dis_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS4 FPI/DIS ion background energy during this survey [mms4_dis_spectr_bg_slow]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS4 FPI/DIS ion background number density during this survey [mms4_dis_numberdensity_bg_slow]

Background number density derived via integration of the estimated background
differential energy flux.

MMS4 FPI/DIS ion number density during this survey [mms4_dis_numberdensity_slow]

MMS4 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms4_dis_densityextrapolation_low_slow]

MMS4 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms4_dis_densityextrapolation_high_slow]

MMS4 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms4_dis_bulkv_dbcs_slow]

MMS4 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms4_dis_bulkv_gse_slow]

MMS4 FPI/DIS ion pressure tensor in DBCS during this survey [mms4_dis_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS ion pressure tensor in GSE during this survey [mms4_dis_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS ion background pressure during this survey [mms4_dis_pres_bg_slow]

MMS4 FPI/DIS ion temperature tensor in DBCS during this survey [mms4_dis_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS ion temperature tensor in GSE during this survey [mms4_dis_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS ion heat-flux vector in DBCS during this survey [mms4_dis_heatq_dbcs_slow]

MMS4 FPI/DIS ion heat-flux vector in GSE during this survey [mms4_dis_heatq_gse_slow]

MMS4 FPI/DIS ion parallel temperature during this BP [mms4_dis_temppara_slow]

MMS4 FPI/DIS ion perpendicular temperature during this BP [mms4_dis_tempperp_slow]

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MMS4_FPI_SLOW_L2_DIS-MOMSAUX

Description

FPI usually operates in Slow Survey Mode outside of the MMS Region Of Interest
(ROI) for the current Mission Phase.  Data captured from one of the four dual
spectrometers over three spacecraft spins are reported at about 60 s resolution
in this mode. This moments product contains results from integrating the
standard moments of phase-space distributions formed during Slow Mode. For
convenience, some additional parameters are included to augment those most
commonly found in a moments product of this sort, plus time-stamps and other
annotations characterizing the state of the instrument system at the indicated
time.

Modification History

See FPI Version Release Notes
(https://lasp.colorado.edu/mms/sdc/public/datasets/fpi/) for data set 
modification history.

Data Variable Descriptions

MMS4 FPI/DIS vector of data-quality indicators at survey-start time [mms4_dis_errorflags_slow]

Value of zero signifies no quality errors. For non-zero values: Bit-0 = manually
flagged interval, Bit-1 = overcounting/saturation effects likely present in
skymap, Bit-2 = reported spacecraft potential above 20V, Bit-3 =
invalid/unavailable spacecraft potential, Bit-4 = significant (>10%) cold plasma
(<10eV) component, Bit-5 = significant (>25%) hot plasma (>30keV) component,
Bit-6 = high sonic Mach number (v/vth > 2.5), Bit-7 = low calculated density
(n_DIS <= 0.0 cm^-3), Bit-8 = invalid/unavailable magnetic field data, Bit-10 =
no internally generated photoelectron correction applied, Bit-11 = compression
pipeline error, Bit-12 = spintone calculation error (DBCS only), Bit-13 =
significant (>=20%) penetrating radiation, Bit-14 = high MMS3 spintone due to
DIS008 anomaly

MMS4 FPI/DIS partial ion number density during this survey [mms4_dis_numberdensity_part_slow]

MMS4 FPI/DIS partial ion bulk-velocity vector in DBCS during this survey [mms4_dis_bulkv_part_dbcs_slow]

MMS4 FPI/DIS partial ion bulk-velocity vector in GSE during this survey [mms4_dis_bulkv_part_gse_slow]

MMS4 FPI/DIS partial ion pressure tensor in DBCS during this survey [mms4_dis_prestensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS partial ion pressure tensor in GSE during this survey [mms4_dis_prestensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS partial ion temperature tensor in DBCS during this survey [mms4_dis_temptensor_part_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS partial ion temperature tensor in GSE during this survey [mms4_dis_temptensor_part_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS partial ion parallel temperature during this survey [mms4_dis_temppara_part_slow]

MMS4 FPI/DIS partial ion perpendicular temperature during this survey [mms4_dis_tempperp_part_slow]

MMS4 FPI/DIS recommended energy index for partial moments during this survey [mms4_dis_part_index_slow]

Recommended energy index during this survey

MMS4 FPI/DIS compression lossless/lossy indicator at survey-start time [mms4_dis_compressionloss_slow]

FPI/DIS compression loss indicator, 0=lossless, 1=lossy

MMS4 FPI/DIS Del-Phi (obs spin-phase) count at survey-start time [mms4_dis_startdelphi_count_slow]

Nominally, spin-phase counts range over [0000, 5759] cnts.  Each count
represents 1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates
obs +X-axis aligned with the sun-sensor axis.

MMS4 FPI/DIS Del-Phi (obs spin-phase) angle at survey-start time [mms4_dis_startdelphi_angle_slow]

Nominally, spin-phase angles range over [0, 360) deg.  Each count represents
1/16 deg of observatory spin-phase.  Zero spin-phase angle indicates obs +X-axis
aligned with the sun-sensor axis.

MMS4 FPI/DIS ion energy spectrum "near" +X_DBCS during this survey [mms4_dis_energyspectr_px_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +x axis (instrument look angles: 45deg <= theta < 135deg and 135deg <=
phi < 225deg).

MMS4 FPI/DIS ion energy spectrum "near" -X_DBCS during this survey [mms4_dis_energyspectr_mx_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -x axis (instrument look angles: 45deg <= theta < 135deg and phi >=
315deg or phi < 45deg).

MMS4 FPI/DIS ion energy spectrum "near" +Y_DBCS during this survey [mms4_dis_energyspectr_py_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +y axis (instrument look angles: 45deg <= theta < 135deg and 225deg <=
phi < 315deg).

MMS4 FPI/DIS ion energy spectrum "near" -Y_DBCS during this survey [mms4_dis_energyspectr_my_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -y axis (instrument look angles: 45deg <= theta < 135deg and 45deg <= phi
< 135deg).

MMS4 FPI/DIS ion energy spectrum "near" +Z_DBCS during this survey [mms4_dis_energyspectr_pz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the +z axis (instrument look angles: 135deg <= theta < 180deg and 0deg <= phi
< 360deg).

MMS4 FPI/DIS ion energy spectrum "near" -Z_DBCS during this survey [mms4_dis_energyspectr_mz_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
particles whose DBCS flow direction is within 45 degrees (polar and azimuthal)
of the -z axis (instrument look angles: 0deg <= theta < 45deg and 0deg <= phi <
360deg).

MMS4 FPI/DIS omni-directional ion energy spectrum during this survey [mms4_dis_energyspectr_omni_slow]

Differential energy flux by energy bin, averaged (weighted by solid angle) over
all directions (flow or look).

MMS4 FPI/DIS ion background energy during this survey [mms4_dis_spectr_bg_slow]

Background differential energy flux by energy bin, averaged (weighted by solid
angle) over all directions (flow or look).

MMS4 FPI/DIS ion background number density during this survey [mms4_dis_numberdensity_bg_slow]

Background number density derived via integration of the estimated background
differential energy flux.

MMS4 FPI/DIS ion number density during this survey [mms4_dis_numberdensity_slow]

MMS4 FPI/DIS estimated (via extrapolation to 0) contribution to density integral below 10eV [mms4_dis_densityextrapolation_low_slow]

MMS4 FPI/DIS estimated (via extrapolation to infinity) contribution to density integral above 30keV [mms4_dis_densityextrapolation_high_slow]

MMS4 FPI/DIS ion bulk-velocity vector in DBCS during this survey [mms4_dis_bulkv_dbcs_slow]

MMS4 FPI/DIS ion bulk-velocity vector in GSE during this survey [mms4_dis_bulkv_gse_slow]

MMS4 FPI/DIS ion pressure tensor in DBCS during this survey [mms4_dis_prestensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS ion pressure tensor in GSE during this survey [mms4_dis_prestensor_gse_slow]

The 3x3 matrix is represented as: Row1) Pxx Pxy Pxz, Row2) Pyx Pyy Pyz, Row3)
Pzx Pzy Pzz. Note that Pij=Pji.

MMS4 FPI/DIS ion background pressure during this survey [mms4_dis_pres_bg_slow]

MMS4 FPI/DIS ion temperature tensor in DBCS during this survey [mms4_dis_temptensor_dbcs_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS ion temperature tensor in GSE during this survey [mms4_dis_temptensor_gse_slow]

The 3x3 matrix is represented as: Row1) Txx Txy Txz, Row2) Tyx Tyy Tyz, Row3)
Tzx Tzy Tzz. Note that Tij=Tji.

MMS4 FPI/DIS ion heat-flux vector in DBCS during this survey [mms4_dis_heatq_dbcs_slow]

MMS4 FPI/DIS ion heat-flux vector in GSE during this survey [mms4_dis_heatq_gse_slow]

MMS4 FPI/DIS ion parallel temperature during this BP [mms4_dis_temppara_slow]

MMS4 FPI/DIS ion perpendicular temperature during this BP [mms4_dis_tempperp_slow]

MMS4 FPI/DIS S/C potential mean [mms4_dis_scpot_mean_slow]

Average spacecraft potential during this SP used to shift the measure energies.

MMS4 FPI/DIS S/C potential max [mms4_dis_scpot_max_slow]

Maximum spacecraft potential during this SP used to exclude energies containing
spacecraft photoelectron fluxes.

Magnetic field vector X,Y,Z, and magnitude B [mms4_dis_fpib_gse_srvy_slow]

Averaged survey magnetic field data during this SP

Magnetic field vector X,Y,Z, and magnitude B [mms4_dis_fpib_dmpa_srvy_slow]

Averaged survey magnetic field data during this SP. DMPA coordinates are within
3 deg from DBCS coordinates and are used for pitch-angle determination.

Position in GSE coordinates, 30 second [mms4_dis_pos_gse_slow]

Position in GSM coordinates, 30 second [mms4_dis_pos_gsm_slow]

MMS4 number density integrands [mms4_dis_numberdensity_int_slow]

integrand terms used in normalized energy integration for number density

number flux [mms4_dis_numberflux_int_dbcs_slow]

integrand terms used in normalized energy integration for number flux

MMS4 pressure tensor integrands [mms4_dis_prestensor_int_dbcs_slow]

integrand terms used in normalized energy integration for pressure tensor (L2
bulk velocity taken into account)

Normalized energies (E/(E+E0)) used in numerical integration of plasma moments [mms4_dis_ugrid_int_slow]

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MMS4_HPCA_BRST_L2_ION (spase://NASA/NumericalData/MMS/4/HotPlasmaCompositionAnalyzer/Burst/Level2/Ion/PT0.625S)

Description

References

Modification History

Initial Public Release

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MMS4_HPCA_BRST_L2_MOMENTS (spase://NASA/NumericalData/MMS/4/HotPlasmaCompositionAnalyzer/Burst/Level2/Moments/PT10S)

Description

References

Modification History

Initial Public Release

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MMS4_HPCA_SRVY_L2_ION (spase://NASA/NumericalData/MMS/4/HotPlasmaCompositionAnalyzer/Survey/Level2/Ion/PT0.625S)

Description

References

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MMS4_HPCA_SRVY_L2_MOMENTS (spase://NASA/NumericalData/MMS/4/HotPlasmaCompositionAnalyzer/Survey/Level2/Moments/PT10S)

Description

References

Modification History

Initial Public Release

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MMS4_HPCA_SRVY_L2_TOF-COUNTS (spase://NASA/NumericalData/MMS/4/HotPlasmaCompositionAnalyzer/Survey/Level2/TimeOfFlight/Counts/PT0.625S)

Description

References

Modification History

Initial Public Release

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MMS4_MEC_BRST_L2_EPHT89D (spase://NASA/NumericalData/MMS/4/Ephemeris/Burst/Level2/Tsyganenko_89_Dynamic/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS4_MEC_BRST_L2_EPHT89Q (spase://NASA/NumericalData/MMS/4/Ephemeris/Burst/Level2/Tsyganenko_89_Quiet/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS4_MEC_BRST_L2_EPHTS04D (spase://NASA/NumericalData/MMS/4/Ephemeris/Burst/Level2/Tsyganenko_04_Dynamic/PT0.030S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS4_MEC_SRVY_L2_EPHT89D (spase://NASA/NumericalData/MMS/4/Ephemeris/Survey/Level2/Tsyganenko_89_Dynamic/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS4_MEC_SRVY_L2_EPHT89Q (spase://NASA/NumericalData/MMS/4/Ephemeris/Survey/Level2/Tsyganenko_89_Quiet/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS4_MEC_SRVY_L2_EPHTS04D (spase://NASA/NumericalData/MMS/4/Ephemeris/Survey/Level2/Tsyganenko_04_Dynamic/PT30S)

Description

MMS MEC Magnetic ephemeris and coordinates, Level 2 science data. PI institution
is Los Alamos National Laboratory (LANL)

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MMS4_R0_SUMMARY

Description

Pre-generated MMS Quicklook Summary Plots
File location: https://cdaweb.gsfc.nasa.gov/pub/data/mms/ql_plots/all_mms4_summ

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MMS4_SCM_BRST_L2_SCB (spase://NASA/NumericalData/MMS/4/FIELDS/SCM/Burst/Level2/PT0.0001220703125S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
https://urldefense.proofpoint.com/v2/url?u=http-3A__link.springer.com_article_10
.1007_s11214-2D014-2D0096-2D9&d=DwIFAg&c=c6MrceVCY5m5A_KAUkrdoA&r=bjziExGTRYoZgE
2xb_dDSm9NxNIo0lG6Q-rB0Y6rHS4&m=CMzo0Vv9zPtWSdbdY1Wq9-jIkYS2cOMV9JYZsMV10y0&s=Xb
P9PiEAswHGl5lqgsDVI6zs8ivJx7yek9i2undKl10&e=

Modification History

unpack telemetry, assign sample times
2026-07-10T20:12:44.00005370378175Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-16T12:40:49.00003373622908Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-16T12:40:57.0000305771829Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms4_scm_acb_gse_scb_brst_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 8192S/s.
They are high-pass filtered above 1.00Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide.

(List/Create Only) Quality Factor (one letter per antenna, G=good) [mms4_scm_qf_scm123_scb_brst_l2]

Each letter refers to one SCM physical antenna in the SCM123 order. 'G' stands
for good data, 'Z' for data that are affected or set to zero by convolution
boundary effect, 'S' for saturated data, 'X' for out of range data, 'B' for
fillvalue/bad data.

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MMS4_SCM_BRST_L2_SCHB (spase://NASA/NumericalData/MMS/4/FIELDS/SCM/Burst/Level2/PT0.00006101515625S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
http://link.springer.com/article/10.1007/s11214-014-0096-9

Modification History

unpack telemetry, assign sample times
2026-07-10T20:13:12.00006276368782Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-16T12:41:30.00005275011067Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-16T12:41:34.00003105401998Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms4_scm_acb_gse_schb_brst_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 16384S/s.
They are high-pass filtered above 32.00Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide
(https://lasp.colorado.edu/mms/sdc/public/datasets/fields/Science_Data_Products_ 
Guide_vol2_SCM_v11_20160301.pdf).

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MMS4_SCM_SRVY_L2_SCSRVY (spase://NASA/NumericalData/MMS/4/FIELDS/SCM/Survey/Level2/PT0.03125S)

Description

The tri-axial search-coil magnetometer (SCM) with its associated preamplifier
provides the three-dimensional measurement of the magnetic field fluctuations.
The analog magnetic waveforms measured by the SCM are digitized and processed
inside the digital signal processor (DSP), collected and stored by the central
instrument data processor (CIDP) via the Fields central electronics box (CEB).
Prior to launch, all SCM Flight models were calibrated by LPP at the National
Magnetic Observatory at Chambon-la-Foret (Orleans). Once per orbit, each SCM
transfer function is checked thanks to the onboard calibration signal provided
by DSP. SCM is operated for the entire MMS orbit in survey mode. Within the ROI,
burst mode data are also acquired as well as high burst mode data. 
SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in
the GSE frame.
The instrument paper for SCM can be found at
http://link.springer.com/article/10.1007/s11214-014-0096-9

Modification History

unpack telemetry, assign sample times
2026-07-03T00:00:34.00005698204041Z - [L1A->L1B (step 1/1)] Calibration
(TMcounts->nT). See CALIBRATION_PARAMETERS for details.
2026-07-15T23:57:22.00005233287508Z - [L1B->L2 (step 1/2)] Coordinate transform
(SCM123->GSE). See COORD_TRANS_PARAMETERS for details.
2026-07-15T23:58:05.00006049871102Z - [L1B->L2 (step 2/2)] Frequency filtering.
See FREQUENCY_FILTER for details.

Data Variable Descriptions

L2 AC magnetic field in GSE frame [mms4_scm_acb_gse_scsrvy_srvy_l2]

These calibrated (nT) AC magnetic field waveform data are sampled at 32S/s. They
are high-pass filtered above 0.50Hz but not low-pass filtered. See global
attributes for details. For more information, please have a look at the SCM Data
Products Guide
(https://lasp.colorado.edu/mms/sdc/public/datasets/fields/Science_Data_Products_ 
Guide_vol2_SCM_v11_20160301.pdf).

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MOON_HELIO1HR_POSITION

Description

No TEXT global attribute value.

Data Variable Descriptions

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MSL_RAD_OBS-L1

Description

The Radiation Assessment Detector (RAD) and its data products are described in
detail in the literature (Hassler et al., 2012). Each RAD observation contains
the following: (1) Instrument counters, (2) Neutral particle count histograms in
detectors D and E, (3) LET count histograms, (4) Absorbed dose rate in detectors
B and E, (5) High-cadence dose rate in B and E (16 rates per observation).

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MSL_RAD_OBS-L2

Description

The Radiation Assessment Detector (RAD) and its data products are described in
detail in the literature (Hassler et al., 2012). Each RAD observation contains
the following: (1) Instrument counters, (2) Neutral particle count histograms in
detectors D and E, (3) LET count histograms, (4) Absorbed dose rate in detectors
B and E, (5) High-cadence dose rate in B and E (16 rates per observation).

Data Variable Descriptions

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MUNIN_M1_MDSE (spase://ESA/NumericalData/Munin/MEDUSA/Electron/PT0.25S)

Description

References:                                             
1. The Instrument Data File Set. URL http://www.idfs.org

Modification History

Initial Release

Data Variable Descriptions

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MUNIN_M1_MDSI (spase://ESA/NumericalData/Munin/MEDUSA/Ion/PT0.25S)

Description

References:                                             
1. The Instrument Data File Set. URL http://www.idfs.org

Modification History

Initial Release

Data Variable Descriptions

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MUNIN_M1_OA (spase://ESA/NumericalData/Munin/Ephemeris/PT0.25S)

Description

References:                                             
1. The Instrument Data File Set. URL http://www.idfs.org

Modification History

Initial Release

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MVN_INSITU_KP-4SEC doi:10.48322/p7yg-g215
Proper citations should include the "Accessed on date" in the form .

Description

Multi-Instrument

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MVN_MAG_L2-SUNSTATE-1SEC doi:10.48322/b9da-ph25
Proper citations should include the "Accessed on date" in the form .

Description

MAG>Mag

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MVN_SEP_L2_S1-CAL-SVY-FULL (spase://NASA/NumericalData/MAVEN/SEP/Level2/Sensor1/Survey/PT8S)

Description

MAVEN SEP electron and ion Flux

Modification History

Revision 0

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MVN_SEP_L2_S2-CAL-SVY-FULL (spase://NASA/NumericalData/MAVEN/SEP/Level2/Sensor2/Survey/PT8S)

Description

MAVEN SEP electron and ion flux

Modification History

Revision 0

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MVN_STA_L2_D8-12R1E (spase://NASA/NumericalData/MAVEN/STATIC/Level2/Distributions/APIDd8/PT4S)

Description

STATIC>Supra-Thermal And Thermal Ion Composition Particle Distributions

Modification History

Rev-1 2014-04-28

Data Variable Descriptions

Rate data for the rate channels sorted by energy step [rates]

Rate data for the rate channels sorted by energy step with dimension (NUM_DISTS,
NRATE, NENERGY) units=counts/s

Quality flag [quality_flag]

Quality flag (NUM_DISTS elements)

---> Validity flag codes valid data (bit 0), test pulser on (bit 1), diag mode (bit 2), data comp type (bit 3-4), packet compn (bit 5) [valid]

---> Validity flag codes valid data (bit 0), test pulser on (bit 1), diagnostic
mode (bit 2), data compression type (bit 3-4), packet compression (bit 5)
(NUM_DISTS elements)

---> Decoded mode number [mode]

---> Decoded mode number. (NUM_DISTS elements)

---> Index that identifies the energy and deflector sweep look up tables (LUT) for the sensor [swp_ind]

---> Index that identifies the energy and deflector sweep look up tables (LUT)
for the sensor. SWP_IND is an index that selects the following support data
arrays: ENERGY, DENERGY, THETA, DTHETA, PHI, DPHI, DOMEGA, GF and MASS_ARR.
(NUM_DISTS elements), EN_IND Le NSWP

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MVN_STA_L2_D9-12R64E (spase://NASA/NumericalData/MAVEN/STATIC/Level2/Distributions/APIDd9/PT128S)

Description

STATIC> Supra-Thermal And Thermal Ion Composition Particle Distributions

Modification History

Rev-1 2014-04-28

Data Variable Descriptions

Rate data for the rate channels sorted by energy step [rates]

Rate data for the rate channels sorted by energy step with dimension (NUM_DISTS,
NRATE, NENERGY) units=counts/s

Quality flag [quality_flag]

Quality flag (NUM_DISTS elements)

---> Validity flag codes valid data (bit 0), test pulser on (bit 1), diag mode (bit 2), data comp type (bit 3-4), packet compn (bit 5) [valid]

---> Validity flag codes valid data (bit 0), test pulser on (bit 1), diagnostic
mode (bit 2), data compression type (bit 3-4), packet compression (bit 5)
(NUM_DISTS elements)

---> Decoded mode number [mode]

---> Decoded mode number. (NUM_DISTS elements)

Decoded telemetry rate number [rate]

Decoded telemetry rate number. (NUM_DISTS elements)

---> Index that identifies the energy and deflector sweep look up tables (LUT) for the sensor [swp_ind]

---> Index that identifies the energy and deflector sweep look up tables (LUT)
for the sensor. SWP_IND is an index that selects the following support data
arrays: ENERGY, DENERGY, THETA, DTHETA, PHI, DPHI, DOMEGA, GF and MASS_ARR.
(NUM_DISTS elements), EN_IND Le NSWP

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MVN_STA_L2_DA-1R64E (spase://NASA/NumericalData/MAVEN/STATIC/Level2/Distributions/APIDda/PT4S)

Description

STATIC>Supra-Thermal And Thermal Ion Composition Particle Distributions

Modification History

Rev-1 2014-04-28

Data Variable Descriptions

Data for selected rate channel by energy step [rates]

Rate data for the rate channels sorted by energy step with dimension (NUM_DISTS,
NRATE, NENERGY) units=counts/s

Rate Channel selected (0-11) [rate_channel]

Quality flag [quality_flag]

Quality flag (NUM_DISTS elements)

---> Validity flag codes valid data (bit 0), test pulser on (bit 1), diag mode (bit 2), data comp type (bit 3-4), packet compn (bit 5) [valid]

---> Validity flag codes valid data (bit 0), test pulser on (bit 1), diagnostic
mode (bit 2), data compression type (bit 3-4), packet compression (bit 5)
(NUM_DISTS elements)

---> Decoded mode number [mode]

---> Decoded mode number. (NUM_DISTS elements)

Decoded telemetry rate number [rate]

Decoded telemetry rate number. (NUM_DISTS elements)

---> Index that identifies the energy and deflector sweep look up tables (LUT) for the sensor [swp_ind]

---> Index that identifies the energy and deflector sweep look up tables (LUT)
for the sensor. SWP_IND is an index that selects the following support data
arrays: ENERGY, DENERGY, THETA, DTHETA, PHI, DPHI, DOMEGA, GF and MASS_ARR.
(NUM_DISTS elements), EN_IND Le NSWP

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MVN_SWE_L2_ARC3D (spase://NASA/NumericalData/MAVEN/SWEA/Level2/Distributions3D/Archive/PT8S)

Description