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1) Cluster II Rumba Prime Parameter Cluster Ion Spectrometry (CIS) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/CIS/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2014-10-24 01:03:08 Instrument:Cluster Ion Spectrometry (CIS) Resource:NumericalData
This instrument (CIS: Cluster Ion Spectrometry) is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

2) Cluster II Salsa Prime Parameter Cluster Ion Spectrometry (CIS) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/CIS/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2009-01-31 23:59:59 Instrument:Cluster Ion Spectrometry (CIS) Resource:NumericalData
This instrument never worked and there is no data. This instrument (CIS: Cluster Ion Spectrometry) on the other spacecraft is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

3) Cluster II Samba Prime Parameter Cluster Ion Spectrometry (CIS) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/CIS/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2014-10-24 01:02:45 Instrument:Cluster Ion Spectrometry (CIS) Resource:NumericalData
This instrument (CIS: Cluster Ion Spectrometry) is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

4) Cluster II Tango Prime Parameter Cluster Ion Spectrometry (CIS) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Tango/CIS/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:4 seconds
Stop:2014-10-24 01:02:34 Instrument:Cluster Ion Spectrometry (CIS) Resource:NumericalData
This instrument (CIS: Cluster Ion Spectrometry) is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

5) Cluster II Summary Parameter Cluster Ion Spectrometry (CIS) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/CIS/SummaryParameter/60S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2014-10-24 01:02:13 Instrument:Cluster Ion Spectrometry (CIS) Resource:NumericalData
This instrument (CIS: Cluster Ion Spectrometry) is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

6) Geotail CPI Definitive Solar Wind Moments maxmize
Resource ID:spase://VMO/NumericalData/Geotail/CPI/SWA_PT48S
Start:1992-09-28 00:00:33 Observatory:Geotail Cadence:48 seconds
Stop:2014-10-24 01:02:34 Instrument:Solar Wind Analyzer Resource:NumericalData
The CPI Solar Wind analyzer definitive plasma moments. The CPI/SW data are good in the solar wind and may be usefull in the magnetosheath.

7) ISEE 3 Elemental Abundance Ratios maxmize
Resource ID:spase://VEPO/NumericalData/ISEE3/ElemAbun
Start:1978-08-18 00:00:00 Observatory:ISEE 3 Cadence:32 months
Stop:1981-04-30 00:00:00 Instrument:High-Energy Cosmic Rays Resource:NumericalData
This ASCII file contains values and their uncertainties for 25 abundance ratios of various pairs of chemical elements. The ratios are based on 1978-1981 observations of ~50-500 MeV/n cosmic rays by the U. Chicago cosmic ray experiment on ISEE 3. Each of the ratios is linked in the ASCII file to the publication where its derivation is discussed.

8) ISEE 3 Isotopic Abundance Ratios maxmize
Resource ID:spase://VEPO/NumericalData/ISEE3/IsotAbun
Start:1978-08-18 00:00:00 Observatory:ISEE 3 Cadence:32 months
Stop:1981-04-30 00:00:00 Instrument:High-Energy Cosmic Rays Resource:NumericalData
This data product consists of a single ASCII file containing values and their uncertainties for 32 abundance ratios of various pairs of isotopes of 13 chemical elements (C, O, Ne, Mg, Al, Si, Ti, V, Cr, Mn, Fe, Co, Ni). Between this data product and a companion catalog with isotopic fractions, isotopic composition information is given for 21 chemical elements. The ratios are based on 1978-1981 observations of ~50-500 MeV/n cosmic rays by the U. Chicago cosmic ray experiment on ISEE 3. Each of the ratios is linked in the ASCII file to the publication where its derivation is discussed.

9) ISEE 3 Isotopic Fractions maxmize
Resource ID:spase://VEPO/NumericalData/ISEE3/IsotFrac
Start:1978-08-18 00:00:00 Observatory:ISEE 3 Cadence:32 months
Stop:1981-04-30 00:00:00 Instrument:High-Energy Cosmic Rays Resource:NumericalData
This data product consists of a single ASCII file containing values and their uncertainties for isotopic fractions of 56 specific isotopes relative to isotope-integrated elemental abundances, for 15 elements (Be, B, N, S, Cl, Ar, K, Ca, Ti, V, Cr, Mn, Fe, Co, Ni). Between this data product and a companion product with isotopic abundance ratios, isotopic composition information is given for 21 chemical elements. The fractions are based on 1978-1981 observations of ~50-500 MeV/n cosmic rays by the U. Chicago cosmic ray experiment on ISEE 3. Each of the ratios is linked in the ASCII file to the publication where its derivation is discussed.

10) Polar TIMAS H0 High-resolution Level 1 Data maxmize
Resource ID:spase://VMO/NumericalData/POLAR/TIMAS/H0_PT12S
Start:1996-03-17 00:03:19 Observatory:POLAR Cadence:12 seconds
Stop:2004-04-03 09:04:47 Instrument:Toroidal Imaging Mass-Angle Spectrograph (TIMAS) Resource:NumericalData
Mass resolved ion energy angle spectra covering nearly the full 4pi solid angle and the energy range 15 eV/q to 33 eV/q. H+, O+, He+ and He++ number fluxes and statistical uncertainties processed by the TIMAS science team. Data acquired with various angular and energy resolutions are combined here. Data Quality and other indicators are provided to allow selection of high resolution data (PA_status(ion)=0 and Energy_status(ion)=0 ) and High Quality data (Quality=0). See caveats for the following variables for more detailed information: Quality, PA_status, Energy_status Bcr, Fec, Even_odd, Energy_Range_ID and Spins. Reference:E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995. Version 0: December, 1997 Version 1: July, 1998 Version 2: December, 2000 Algorithm improved to more accurately subtract backgrounds arising from spill over from H+ into He++ channel and other sources. Fill data are now inserted for limited energy and pitch angle ranges for Flux_H Flux_O Flux_He_1 and Flux_He_2 variables. The meanging of values of the of Quality variable was slightly modified. Version 3: June, 2002 Algorithm for V_02 had an error that resulted in under estimation of fluxes in high count regions, i.e. the cusp/cleft and radiation belts. V_03 corrects this error and has been expanded to include calculation of fluxes obtained after December 8, 1998, when TIMAS had a damaging high voltage breakdown that resulted in reduced sensitivity.

11) Polar TIMAS H2 Level 1 Ion Upflowing Fluxes Data maxmize
Resource ID:spase://VMO/NumericalData/POLAR/TIMAS/H2_PT12S
Start:1996-03-17 00:03:25 Observatory:POLAR Cadence:12 seconds
Stop:1998-12-08 22:55:45 Instrument:Toroidal Imaging Mass-Angle Spectrograph (TIMAS) Resource:NumericalData
H+, O+, He+ and He++ upflowing fluxes and statistical uncertainties processed by the TIMAS science team.These data were used in preparing several papers, see Information URLs. Includes also non-TIMAS Data: UT, altitude, invariant latitude, L shell, magnetic local time, geomagnetic latitude (signed - n/s hemisphere), average magnetic field vector in GSM coordinates at Polar (uses KH's co-ord conversion code), spacecraft potential from EFI data base, solar zenith angles at each end of the field line, time delayed solar wind parameters from WIND (Using KH's database) interpolated across data gaps of less than 10 minutes, IMF in GSM, solar wind dynamic pressure (nPa), solar wind density (/cc), solar wind velocity (km/sec). This is a summary data base.It does not contain detailed energy step and pitch angle information for each data point. Extends over all altitudes, invariant latitudes and MLT. Below altitude of 4.0 Re 2 spin resolution (12s), above altitude of 4.0 Re 4 spin resolution (24s). Reference:E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995.

12) Polar TIMAS K1 Key Parameter data maxmize
Resource ID:spase://VMO/NumericalData/POLAR/TIMAS/K1_PT96S
Start:1999-06-07 00:09:31 Observatory:POLAR Cadence:96 seconds
Stop:2008-04-16 13:22:28 Instrument:Toroidal Imaging Mass-Angle Spectrograph (TIMAS) Resource:NumericalData
H+, O+, He+ and He++ number fluxes for survey purposes only Reference:E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995. Version 0: June, 2001

13) Polar TIMAS K2 Mass Spectral Data maxmize
Resource ID:spase://VMO/NumericalData/POLAR/TIMAS/K2_PT192S
Start:1996-03-16 12:47:36 Observatory:POLAR Cadence:192 seconds
Stop:2006-05-28 23:57:58 Instrument:Toroidal Imaging Mass-Angle Spectrograph (TIMAS) Resource:NumericalData
Mass spectra count rates for survey purposes only from the POLAR TIMAS instrument. The mass spectral data product consists of 64 mass steps covering the full detector range, for each of 6 large solid angles, for 8 selected energy steps. The data product is accumulated for 2, 4, 8, 16, or 32 spin (6 s) periods. Because of telemetry restrictions only selected data products were telemetered to the ground. The 6 angular bins cover the full instrumental range and nearly 4pi steradians. Two of the look directions are centered on the spacecraft spin axis. For the first part of the mission, the spin axis was orbit normal and the pitch angles sampled in these look directions are near 90 degrees. The other 4 look directions are in the spin plane. Data are de-spun on board based on the spin rate and time of the "sun pulse". The digital data product provides the center pitch angle of each of the 6 look directions and an estimate of the variation of the pitch angle during the accumulation time. Reference: E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995.

14) SAMPEX Polar-Cap-Averaged Fluxes, all instruments maxmize
Resource ID:spase://VEPO/NumericalData/SAMPEX/PCA/PT48M
Start:1992-07-06 00:00:00 Observatory:SAMPEX Cadence:48 minutes
Stop:2004-06-30 23:59:59 Instrument:Mass Spectrometer Telescope (MAST) Resource:NumericalData
This data set contains 17 differential fluxes of protons (mainly), helium ions, Z.GE.6 ions, and electrons, plus one integral flux of protons and electrons, as averaged over polar cap passes of the SAMPEX spacecraft. A polar cap pass covers the time poleward of geomagnetic latitude 70 deg. (Not all orbits have two polar cap passes.). For any given species, the fluxes typically come from more than one of the sensors (LICA, HILT, MAST, PET). Hence the inclusion of all instruments' data in each single record. Differential fluxes are those for (mainly) protons (Z.GE.1 channels at 5-12 and 19-27 MeV/n), helium ions (0.50-6.6, 4-9, 8-15, 9-38 MeV/n), Z.GE.6 ions (0.49-8.3, 8-42, 19.3-22.8, 22.8-31.0, 31.0-51.7, 41-220, 51.7-76.2, 76.2-113, 113-156 MeV/n), and electrons (1.5-6.0 MeV from PET only). One LICA channel measured integral fluxes of ions .GT. 0.8 MeV/n plus electrons .GT. 0.6 MeV). Data available for each polar cap pass are time tags of the begin and end points of the averaging interval, the fluxes, statistical uncertainties in the fluxes, instrument-specific flags, and a flag indicating a north or south polar cap pass. Data are organized in two different ways. Monthly ~500-KB ASCII files with records organized by instrument are available from the SAMPEX Data Center at Caltech and from nssdcftp at GSFC/SPDF, while monthly ~260 KB CDF-formatted files with records organized by species are available from the ftp area underlying CDAWeb. The parameter level information given below in this descriptor corresponds to the CDAWeb organization of data. Format information for the ASCII version is given in the Information URL of this descriptor.

15) THEMIS-A: On Board moments: ESA and SST Electron/Ion moments, density, flux, velocity, pressure and temperature. maxmize
Resource ID:spase://VMO/NumericalData/THEMIS/A/MOM/PT3S
Start:2007-08-02 00:00:30 Observatory:THEMIS-A Cadence:3 seconds
Stop:2014-10-24 01:02:34 Instrument:THEMIS-A: On Board moments: ESA and SST Electron/Ion moments density, flux, velocity, pressure and temperature. Resource:NumericalData
THEMIS-A On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations. Table 1: Coordinate Descriptions. Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system. Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system. Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis. Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system.

16) THEMIS-A: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV). maxmize
Resource ID:spase://VMO/NumericalData/THEMIS/A/SST/PT3S
Start:2007-03-14 01:00:00 Observatory:THEMIS-A Cadence:3 seconds
Stop:2014-10-24 01:02:33 Instrument:THEMIS-A: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV). Resource:NumericalData
THEMIS-A: The Solid State Telescope (SST) measures the incoming intensity (flux per solid angle) of superthermal electrons and ions. The spacecraft is fitted with two units (heads), each SST unit has two pairs of opposing ion and electron sensors. Each single sensor covers an angle of 36 degrees. The units are oriented such that one pair is always centered in the rotation plane, the other oriented at a maximum angle of 54 degrees off the plane. Each pair of units are oriented opposite each other allowing both ion and electron sensors to sweep out a maximum of 92% of the sky (45x45 degree required Elevation by Azimuth FOV, 108x22 raw) . The ion and electron sensors primarily measure particles between 30-300 keV and 30-100 keV respectively with a maximum capability of 20-6000 keV and 25-1000 keV. Full distribution data is measured over 128 angles and 16 energy bins, reduced distribution uses 6 angles and 16 energy bins, and burst mode data has 64 angles in 16 energy bins. Matched and paired electron broom magnets produce quadrapole fields reducing magnetic contamination. A mechanical attenuator is used to increase the instruments dynamical range avoiding oversaturation near the plasma sheet edge.

17) THEMIS-B: On Board moments: ESA and SST Electron/Ion moments, density, flux, velocity, pressure and temperature. maxmize
Resource ID:spase://VMO/NumericalData/THEMIS/B/MOM/PT3S
Start:2007-08-10 00:02:05 Observatory:THEMIS-B Cadence:3 seconds
Stop:2014-10-24 01:02:31 Instrument:THEMIS-B: On Board moments: ESA and SST Electron/Ion moments density, flux, velocity, pressure and temperature. Resource:NumericalData
THEMIS-B On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations. Table 1: Coordinate Descriptions. Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system. Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system. Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis. Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system.

18) THEMIS-B: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV). maxmize
Resource ID:spase://VMO/NumericalData/THEMIS/B/SST/PT3S
Start:2007-03-14 01:00:00 Observatory:THEMIS-B Cadence:3 seconds
Stop:2014-10-24 01:02:30 Instrument:THEMIS-B: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV). Resource:NumericalData
THEMIS-B: The Solid State Telescope (SST) measures the incoming intensity (flux per solid angle) of superthermal electrons and ions. The spacecraft is fitted with two units (heads), each SST unit has two pairs of opposing ion and electron sensors. Each single sensor covers an angle of 36 degrees. The units are oriented such that one pair is always centered in the rotation plane, the other oriented at a maximum angle of 54 degrees off the plane. Each pair of units are oriented opposite each other allowing both ion and electron sensors to sweep out a maximum of 92% of the sky (45x45 degree required Elevation by Azimuth FOV, 108x22 raw) . The ion and electron sensors primarily measure particles between 30-300 keV and 30-100 keV respectively with a maximum capability of 20-6000 keV and 25-1000 keV. Full distribution data is measured over 128 angles and 16 energy bins, reduced distribution uses 6 angles and 16 energy bins, and burst mode data has 64 angles in 16 energy bins. Matched and paired electron broom magnets produce quadrapole fields reducing magnetic contamination. A mechanical attenuator is used to increase the instruments dynamical range avoiding oversaturation near the plasma sheet edge.

19) THEMIS-C: On Board moments: ESA and SST Electron/Ion moments, density, flux, velocity, pressure and temperature. maxmize
Resource ID:spase://VMO/NumericalData/THEMIS/C/MOM/PT3S
Start:2007-08-10 00:00:32 Observatory:THEMIS-C Cadence:3 seconds
Stop:2014-10-24 01:02:27 Instrument:THEMIS-C: On Board moments: ESA and SST Electron/Ion moments density, flux, velocity, pressure and temperature. Resource:NumericalData
THEMIS-C On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations. Table 1: Coordinate Descriptions. Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system. Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system. Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis. Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system.

20) THEMIS-C: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV). maxmize
Resource ID:spase://VMO/NumericalData/THEMIS/C/SST/PT3S
Start:2007-03-14 01:00:00 Observatory:THEMIS-C Cadence:3 seconds
Stop:2014-10-24 01:02:27 Instrument:THEMIS-C: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV). Resource:NumericalData
THEMIS-C: The Solid State Telescope (SST) measures the incoming intensity (flux per solid angle) of superthermal electrons and ions. The spacecraft is fitted with two units (heads), each SST unit has two pairs of opposing ion and electron sensors. Each single sensor covers an angle of 36 degrees. The units are oriented such that one pair is always centered in the rotation plane, the other oriented at a maximum angle of 54 degrees off the plane. Each pair of units are oriented opposite each other allowing both ion and electron sensors to sweep out a maximum of 92% of the sky (45x45 degree required Elevation by Azimuth FOV, 108x22 raw) . The ion and electron sensors primarily measure particles between 30-300 keV and 30-100 keV respectively with a maximum capability of 20-6000 keV and 25-1000 keV. Full distribution data is measured over 128 angles and 16 energy bins, reduced distribution uses 6 angles and 16 energy bins, and burst mode data has 64 angles in 16 energy bins. Matched and paired electron broom magnets produce quadrapole fields reducing magnetic contamination. A mechanical attenuator is used to increase the instruments dynamical range avoiding oversaturation near the plasma sheet edge.

21) THEMIS-D: On Board moments: ESA and SST Electron/Ion moments, density, flux, velocity, pressure and temperature. maxmize
Resource ID:spase://VMO/NumericalData/THEMIS/D/MOM/PT3S
Start:2007-08-09 23:59:56 Observatory:THEMIS-D Cadence:3 seconds
Stop:2014-10-24 01:02:21 Instrument:THEMIS-D: On Board moments: ESA and SST Electron/Ion moments density, flux, velocity, pressure and temperature. Resource:NumericalData
THEMIS-D On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations. Table 1: Coordinate Descriptions. Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system. Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system. Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis. Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system.

22) THEMIS-D: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV). maxmize
Resource ID:spase://VMO/NumericalData/THEMIS/D/SST/PT3S
Start:2007-03-14 01:00:00 Observatory:THEMIS-D Cadence:3 seconds
Stop:2014-10-24 01:02:20 Instrument:THEMIS-D: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV). Resource:NumericalData
THEMIS-D: The Solid State Telescope (SST) measures the incoming intensity (flux per solid angle) of superthermal electrons and ions. The spacecraft is fitted with two units (heads), each SST unit has two pairs of opposing ion and electron sensors. Each single sensor covers an angle of 36 degrees. The units are oriented such that one pair is always centered in the rotation plane, the other oriented at a maximum angle of 54 degrees off the plane. Each pair of units are oriented opposite each other allowing both ion and electron sensors to sweep out a maximum of 92% of the sky (45x45 degree required Elevation by Azimuth FOV, 108x22 raw) . The ion and electron sensors primarily measure particles between 30-300 keV and 30-100 keV respectively with a maximum capability of 20-6000 keV and 25-1000 keV. Full distribution data is measured over 128 angles and 16 energy bins, reduced distribution uses 6 angles and 16 energy bins, and burst mode data has 64 angles in 16 energy bins. Matched and paired electron broom magnets produce quadrapole fields reducing magnetic contamination. A mechanical attenuator is used to increase the instruments dynamical range avoiding oversaturation near the plasma sheet edge.

23) THEMIS-E: On Board moments: ESA and SST Electron/Ion moments, density, flux, velocity, pressure and temperature. maxmize
Resource ID:spase://VMO/NumericalData/THEMIS/E/MOM/PT3S
Start:2007-08-10 00:00:16 Observatory:THEMIS-E Cadence:3 seconds
Stop:2014-10-24 01:02:18 Instrument:THEMIS-E: On Board moments: ESA and SST Electron/Ion moments density, flux, velocity, pressure and temperature. Resource:NumericalData
THEMIS-E On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations. Table 1: Coordinate Descriptions. Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system. Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system. Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis. Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system.

24) THEMIS-E: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV). maxmize
Resource ID:spase://VMO/NumericalData/THEMIS/E/SST/PT3S
Start:2007-03-14 01:00:00 Observatory:THEMIS-E Cadence:3 seconds
Stop:2014-10-24 01:02:18 Instrument:THEMIS-E: Solid State Telescope (SST): Energy flux spectrogram, electron/ion ground-calculated fluxes (30 keV - 300 keV). Resource:NumericalData
THEMIS-E: The Solid State Telescope (SST) measures the incoming intensity (flux per solid angle) of superthermal electrons and ions. The spacecraft is fitted with two units (heads), each SST unit has two pairs of opposing ion and electron sensors. Each single sensor covers an angle of 36 degrees. The units are oriented such that one pair is always centered in the rotation plane, the other oriented at a maximum angle of 54 degrees off the plane. Each pair of units are oriented opposite each other allowing both ion and electron sensors to sweep out a maximum of 92% of the sky (45x45 degree required Elevation by Azimuth FOV, 108x22 raw) . The ion and electron sensors primarily measure particles between 30-300 keV and 30-100 keV respectively with a maximum capability of 20-6000 keV and 25-1000 keV. Full distribution data is measured over 128 angles and 16 energy bins, reduced distribution uses 6 angles and 16 energy bins, and burst mode data has 64 angles in 16 energy bins. Matched and paired electron broom magnets produce quadrapole fields reducing magnetic contamination. A mechanical attenuator is used to increase the instruments dynamical range avoiding oversaturation near the plasma sheet edge.

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