2.4.1 spase://CNES/NumericalData/CDPP-AMDA/MMS/MMS3/FPI/mms3-fpi-desmoms DES : electrons Dual Electron Spectrometers : fast mode 2024-10-04T05:34:35Z 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 sur vey 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 in dicated time. spase://SMWG/Person/James.L.Burch PrincipalInvestigator spase://CNES/Person/CDPP-AMDA/B.Giles PrincipalInvestigator MMS home page at GSFC http://mms.gsfc.nasa.gov FPI overview http://www.nasa.gov/mission_pages/mms/spacecraft/instruments.html#fpi mms3-fpi-fast PartOf fast mode spase://SMWG/Repository/CDPP/AMDA Online Open CDPP/AMDA HAPI Server https://amda.irap.omp.eu/service/hapi mms3-fpi-desmoms Web Service to this product using the HAPI interface. CSV Thank you for acknowledging the use of AMDA in publications with wording like "Data analysis was performed with the AMDA science analysis system provided by the Centre de Données de la Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de Paris and Université Paul Sabatier, Toulouse". See the Rules of the road at https://amda.cdpp.eu/help/policy.html . Please acknowledge the Data Providers. spase://SMWG/Repository/CDPP/AMDA Online Open CDPP/AMDA Web application https://amda.cdpp.eu Access to Data via CDPP/AMDA Web application. CSV VOTable CDF PNG Thank you for acknowledging the use of AMDA in publications with wording like "Data analysis was performed with the AMDA science analysis system provided by the Centre de Données de la Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de Paris and Université Paul Sabatier, Toulouse". See the Rules of the road at https://amda.cdpp.eu/help/policy.html . Please acknowledge the Data Providers. LASP spase://CNES/Instrument/CDPP-AMDA/MMS3/FPI MagneticField 2015-05-06T00:00:01Z 2024-08-14T00:57:17Z PT4.5S density mms3_des_ne cm^-3 TimeSeries Electron Scalar NumberDensity density : err mms3_des_ne_err cm^-3 TimeSeries Electron Scalar NumberDensity v_gse mms3_des_vgse km/s Cartesian GSE TimeSeries 3 vx Component.I 1 mms3_des_vgse(0) vy Component.J 2 mms3_des_vgse(1) vz Component.K 3 mms3_des_vgse(2) Electron Scalar NumberDensity v_gse : err mms3_des_v_err km/s TimeSeries 3 vx Component.I 1 mms3_des_v_err(0) vy Component.J 2 mms3_des_v_err(1) vz Component.K 3 mms3_des_v_err(2) Electron Scalar NumberDensity t_para mms3_des_tpara eV TimeSeries Electron Scalar Temperature t_perp mms3_des_tperp eV TimeSeries Electron Scalar Temperature heatq_gse mms3_des_heatq phys.pressure mW/m^2 Cartesian GSE TimeSeries 3 x 1 mms3_des_heatq(0) y 2 mms3_des_heatq(1) z 3 mms3_des_heatq(2) Electron Vector HeatFlux pressure_gse mms3_des_press phys.pressure nPa Cartesian GSE TimeSeries 9 xx 1 mms3_des_press(0) xy 2 mms3_des_press(1) xz 3 mms3_des_press(2) yx 4 mms3_des_press(3) yy 5 mms3_des_press(4) yz 6 mms3_des_press(5) zx 7 mms3_des_press(6) zy 8 mms3_des_press(7) zz 9 mms3_des_press(8) Electron Tensor Pressure elec eflux : omni mms3_des_omni keV/(cm^2-s-sr-keV) Spectrogram Electron EnergyFlux elec eflux : para mms3_des_para keV/(cm^2-s-sr-keV) Spectrogram Electron EnergyFlux elec eflux : anti mms3_des_anti keV/(cm^2-s-sr-keV) Spectrogram Electron EnergyFlux elec eflux : perp mms3_des_perp keV/(cm^2-s-sr-keV) Spectrogram Electron EnergyFlux pa dist : lowen mms3_des_palow Low energy bin: 0 eV - 200 eV. Pitch-angle bin size: 6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not shifted by the bulk velocity keV/(cm^2-s-sr-keV) Spectrogram Electron EnergyFlux pa dist : miden mms3_des_pamid Mid energy bin: 200 eV - 2 keV. Pitch-angle bin size: 6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not shifted by the bulk velocity keV/(cm^2-s-sr-keV) Spectrogram Electron EnergyFlux pa dist : highen mms3_des_pahigh High energy bin: 2 keV - 30 keV. Pitch-angle bin size: 6 deg. Note that pitch angles are calculated in the spacecraft frame; i.e., not shifted by the bulk velocity keV/(cm^2-s-sr-keV) Spectrogram Electron EnergyFlux