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1) AMPTE/IRM Plasma Data maxmize
Resource ID:spase://VMO/NumericalData/AMPTE_IRM/Plasma/PT4.4S
Start:1984-08-22 12:58:03 Observatory:AMPTE/IRM Cadence:4.4 seconds
Stop:1986-08-11 21:32:28 Instrument:AMPTE/IRM Plasma Instrument Resource:NumericalData
AMPTE/IRM spin-averaged plasma moments at ~4.4 second resolution.

2) AMPTE/UKS Ion Plasma Data maxmize
Resource ID:spase://VMO/NumericalData/AMPTE_UKS/Plasma/FTR_PT5S
Start:1984-08-27 14:10:53 Observatory:AMPTE/UKS Cadence:5 seconds
Stop:1985-01-15 07:50:33 Instrument:AMPTE/UKS 3-D Plasma Analyzer Resource:NumericalData
AMPTE/UKS 5-second (spin) averaged ion plasma moments

3) AMPTE/UKS Ion Plasma Data, solar wind mode maxmize
Resource ID:spase://VMO/NumericalData/AMPTE_UKS/Plasma/SWI_PT5S
Start:1984-08-27 14:50:39 Observatory:AMPTE/UKS Cadence:5 seconds
Stop:1984-12-29 07:10:56 Instrument:AMPTE/UKS 3-D Plasma Analyzer Resource:NumericalData
AMPTE/UKS 5-second (spin) averaged ion plasma moments

4) Cluster II Rumba Prime Parameter Plasma Electron and Current Experiment (PEACE) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/PEACE/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2014-10-22 01:03:21 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7-10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0-180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. 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 PEACE: a Plasma Electron and Current Experiment, by A. D. Johnstone et al., from which this information was obtained.

5) Cluster II Rumba Prime Parameter Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/WHISPER/PrimeParameter/4S
Start:2000-12-10 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2014-10-22 01:03:21 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) experiment provides measurements of the electron density via active sounding of plasma resonances and records via passive wave analysis the natural wave emissions in the high-frequency range, from 4-80 KHz. 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 WHISPER, a Sounder and High-Frequency Wave Analyser Experiment, by P. M. E. Decreau et al., from which this information was obtained.

6) Cluster II Salsa Prime Parameter Plasma Electron and Current Experiment (PEACE) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/PEACE/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2014-10-22 01:02:24 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7-10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0-180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. 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 PEACE: a Plasma Electron and Current Experiment, by A. D. Johnstone et al., from which this information was obtained.

7) Cluster II Salsa Prime Parameter Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/WHISPER/PrimeParameter/4S
Start:2000-12-10 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2014-10-22 01:02:24 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) experiment provides measurements of the electron density via active sounding of plasma resonances and records via passive wave analysis the natural wave emissions in the high-frequency range, from 4-80 KHz. 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 WHISPER, a Sounder and High-Frequency Wave Analyser Experiment, by P. M. E. Decreau et al., from which this information was obtained.

8) Cluster II Samba Prime Parameter Plasma Electron and Current Experiment (PEACE) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/PEACE/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2014-10-22 01:02:57 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7-10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0-180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. 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 PEACE: a Plasma Electron and Current Experiment, by A. D. Johnstone et al., from which this information was obtained.

9) Cluster II Samba Prime Parameter Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/WHISPER/PrimeParameter/4S
Start:2000-12-10 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2014-10-22 01:02:57 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) experiment provides measurements of the electron density via active sounding of plasma resonances and records via passive wave analysis the natural wave emissions in the high-frequency range, from 4-80 KHz. 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 WHISPER, a Sounder and High-Frequency Wave Analyser Experiment, by P. M. E. Decreau et al., from which this information was obtained.

10) Cluster II Tango Prime Parameter Plasma Electron and Current Experiment (PEACE) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Tango/PEACE/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:4 seconds
Stop:2014-10-22 01:02:46 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7-10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0-180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. 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 PEACE: a Plasma Electron and Current Experiment, by A. D. Johnstone et al., from which this information was obtained.

11) Cluster II Tango Prime Parameter Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Tango/WHISPER/PrimeParameter/4S
Start:2000-12-10 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:4 seconds
Stop:2014-10-22 01:02:45 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) experiment provides measurements of the electron density via active sounding of plasma resonances and records via passive wave analysis the natural wave emissions in the high-frequency range, from 4-80 KHz. 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 WHISPER, a Sounder and High-Frequency Wave Analyser Experiment, by P. M. E. Decreau et al., from which this information was obtained.

12) Cluster II Summary Parameter Plasma Electron and Current Experiment (PEACE) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/PEACE/SummaryParameter/60S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2014-10-22 01:02:24 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7-10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0-180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. 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 PEACE: a Plasma Electron and Current Experiment, by A. D. Johnstone et al., from which this information was obtained.

13) Cluster II Summary Parameter Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/WHISPER/SummaryParameter/60S
Start:2001-01-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2014-10-22 01:02:23 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) experiment provides measurements of the electron density via active sounding of plasma resonances and records via passive wave analysis the natural wave emissions in the high-frequency range, from 4-80 KHz. 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 WHISPER, a Sounder and High-Frequency Wave Analyser Experiment, by P. M. E. Decreau et al., from which this information was obtained.

14) Dynamics Explorer 2 Ion Drift Meter (IDM) maxmize
Resource ID:spase://VMO/NumericalData/DE2/IDM/PT0.25S
Start:1981-08-15 00:00:00 Observatory:Dynamics Explorer 2 Cadence:0.25 seconds
Stop:1981-02-19 00:00:00 Instrument:Ion Drift Meter (IDM) Resource:NumericalData
Dynamics Explorer 2 Ion Drift Meter (IDM)

15) Dynamics Explorer 2 Langmuir Probe (LANG) maxmize
Resource ID:spase://VMO/NumericalData/DE2/LANG/PT0.5S
Start:1981-08-05 00:00:00 Observatory:Dynamics Explorer 2 Cadence:0.5 seconds
Stop:1981-02-19 00:00:00 Instrument:Langmuir Probe (LANG) Resource:NumericalData
Dynamics Explorer 2 Langmuir Probe (LANG)

16) Dynamics Explorer 2 Retarding Potential Analyzer (RPA) maxmize
Resource ID:spase://VMO/NumericalData/DE2/VEFI/Ni.Vi.Ti/PT2S
Start:1981-08-03 00:00:00 Observatory:Dynamics Explorer 2 Cadence:2 seconds
Stop:1981-02-19 00:00:00 Instrument:Retarding Potential Analyzer (RPA) Resource:NumericalData
Dynamics Explorer 2 Retarding Potential Analyzer (RPA)

17) Dynamics Explorer 2 Retarding Potential Analyzer (RPA) maxmize
Resource ID:spase://VMO/NumericalData/DE2/VEFI/Ni/PT0.016S
Start:1981-08-03 00:00:00 Observatory:Dynamics Explorer 2 Cadence:0.016 seconds
Stop:1981-02-19 00:00:00 Instrument:Retarding Potential Analyzer (RPA) Resource:NumericalData
Dynamics Explorer 2 Retarding Potential Analyzer (RPA)

18) Double Star 1 Spacecraft Hot Ion Analyzer (HIA) Prime Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar1/HIA/PrimeParameters/4S
Start:2004-02-04 02:40:38 Observatory:Double Star 1 Cadence:4 seconds
Stop:2007-09-29 06:38:33 Instrument:HIA (Hot Ion Analyzer) Resource:NumericalData
The Double Star 1 Hot Ion Analyzer (HIA) prime parameter data set contains various parameters at spin resolution. These parameters include universal time, the instrument status, the ion density, ion bulk velocity, and ion temperature. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.

19) Double Star 1 Spacecraft Hot Ion Analyzer (HIA) Summary Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar1/HIA/SummaryParameters/60S
Start:2004-02-04 02:40:30 Observatory:Double Star 1 Cadence:60 seconds
Stop:2007-09-29 06:38:33 Instrument:HIA (Hot Ion Analyzer) Resource:NumericalData
The Double Star 1 Hot Ion Analyzer (HIA) summary parameter data set contains various parameters at 60 s resolution. These parameters include universal time, the instrument status, the ion density, ion bulk velocity, and ion temperature. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.

20) Double Star 1 Spacecraft Data Plasma Electron and Current Experiment (PEACE) Prime Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar1/PEACE/PrimeParameters/4S
Start:2004-01-20 05:43:36 Observatory:Double Star 1 Cadence:4 seconds
Stop:2007-09-16 10:42:02 Instrument:PEACE (Plasma Electron And Current Experiment) Resource:NumericalData
The Double Star 1 Plasma Electron and Current Experiment (PEACE) prime parameter data set contains various parameters at spin resolution. These parameters include universal time, the instrument status, the electron density, electron bulk velocity, electron temperature, and electron heat flux. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.

21) Double Star 1 Spacecraft Data Plasma Electron and Current Experiment (PEACE) Summary Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar1/PEACE/SummaryParameters/60S
Start:2004-01-20 05:43:30 Observatory:Double Star 1 Cadence:60 seconds
Stop:2007-09-16 10:41:30 Instrument:PEACE (Plasma Electron And Current Experiment) Resource:NumericalData
The Double Star 1 Plasma Electron and Current Experiment (PEACE) summary parameter data set contains various parameters at 60 s resolution. These parameters include universal time, the instrument status, the electron density, electron bulk velocity, electron temperature, and electron heat flux. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.

22) Double Star 2 Spacecraft Data Low Energy Ion Detector (LEID) Prime Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar2/LEID/PrimeParameters/4S
Start:2004-08-09 09:39:12 Observatory:Double Star 2 Cadence:4 seconds
Stop:2005-10-31 17:38:00 Instrument:Low-Energy Ion Detector (LEID) Resource:NumericalData
The Double Star 2 Low Energy Ion Detector (LEID) prime parameter data set contains various parameters at spin resolution. These parameters include universal time, the instrument status, the ion density, ion bulk velocity, and ion temperature. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.

23) Double Star 2 Spacecraft Data Low Energy Ion Detector (LEID) Summary Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar2/LEID/SummaryParameters/60S
Start:2004-08-09 09:39:30 Observatory:Double Star 2 Cadence:60 seconds
Stop:2005-10-31 17:38:00 Instrument:Low-Energy Ion Detector (LEID) Resource:NumericalData
The Double Star 2 Low Energy Ion Detector (LEID) summary parameter data set contains various parameters at 60 s resolution. These parameters include universal time, the instrument status, the ion density, ion bulk velocity, and ion temperature. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.

24) Double Star 2 Spacecraft Data Plasma Electron and Current Experiment (PEACE) Prime Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar2/PEACE/PrimeParameters/4S
Start:2004-08-15 00:58:10 Observatory:Double Star 2 Cadence:4 seconds
Stop:2008-05-30 23:56:46 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The Double Star 2 Plasma Electron and Current Experiment (PEACE) prime parameter data set contains various parameters at spin resolution. These parameters include universal time, the instrument status, the electron density, electron bulk velocity, electron temperature, and electron heat flux. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.

25) Double Star 2 Spacecraft Data Plasma Electron and Current Experiment (PEACE) Summary Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar2/PEACE/SummaryParameters/60S
Start:2004-08-15 00:58:30 Observatory:Double Star 2 Cadence:60 seconds
Stop:2008-05-30 23:59:30 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The Double Star 2 Plasma Electron and Current Experiment (PEACE) summary parameter data set contains various parameters at 60 s resolution. These parameters include universal time, the instrument status, the electron density, electron bulk velocity, electron temperature, and electron heat flux. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.

26) Geotail CPI Hot Plasma Moments maxmize
Resource ID:spase://VMO/NumericalData/Geotail/CPI/HPA_PT64S
Start:1992-10-06 00:00:28 Observatory:Geotail Cadence:64 seconds
Stop:2014-10-22 01:02:45 Instrument:Geotail Hot Plasma Analyzer Resource:NumericalData
The CPI/HPA Hot Plasma Analyzer high time resolution moments of hot plasma: * Ion number density * Ion average temperature * Ion bulk flow velocity * Electron number density * Electron average temperature The CPI/HPA data are good in the magnetosphere and may be usefull in the magnetosheath.

27) 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:2014-10-22 01:02:45 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.

28) Geotail CPI Plasma Key Parameters (64s) maxmize
Resource ID:spase://VMO/NumericalData/Geotail/CPI/kp_PT64S
Start:1992-09-08 07:30:40 Observatory:Geotail Cadence:64 seconds
Stop:2014-10-22 01:02:45 Instrument:Geotail Hot Plasma Analyzer Resource:NumericalData
A combination of plasma key parameters from the Geotail CPI analyzers. The CPI-SW Solar Wind Analyzer provides * Ion number density * Average proton energy * Bulk flow velocity The CPI-HP Hot Plasma Analyzer provides * Ion number density * Average proton energy * Average electron energy * Bulk flow velocity * Plasma pressure The CPI-IC Ion Composition Analyzer provides principal Species * H+ * He++ * He+ * O+

29) Geotail Editor-A 12 second Low-Energy Particles maxmize
Resource ID:spase://VMO/NumericalData/Geotail/LEP/EDA.PT12S
Start:1993-09-14 13:45:08 Observatory:Geotail Cadence:12 seconds
Stop:2006-12-30 13:30:52 Instrument:Geotail Low Energy Particle Experiment Resource:NumericalData
12-second Editor-A low-energy particle data from the Geotail spacecraft. Editor-A data are only acquired with the real-time operation in Usuda Deep Space Center (UDSC),Japan, while the Editor-B data are 24-hours continuouslyrecorded in the onboard tape recorders and are dumpedover the NASA/JPL Deep Space Network (DSN) stations. The ion energy analyzer (LEP-EAi) has two energy scan mode: RAM-A (60 eV to 40 keV) and RAM-B (5 keV to 40 keV). RAM-B is selected to protect the very sensitive detector from intense low energy fluxes that are usually seen in the solar wind and magnetosheath. The energy scan mode is automatically selected onboard depending on incoming ion fluxes. At present, only the ion moments in the RAM-A mode are listed for the LEP-EAi data. The ion moment data of the solar wind analyzer (LEP-SW) should be used only qualitatively. The LEP-SW ion moments are listed when the energy scan mode of LEP-EAi is RAM-B.

30) Geotail Editor-B 12 second Low-Energy Particles maxmize
Resource ID:spase://VMO/NumericalData/Geotail/LEP/EDB.PT12S
Start:1993-10-05 10:09:45 Observatory:Geotail Cadence:12 seconds
Stop:2006-12-31 23:59:17 Instrument:Geotail Low Energy Particle Experiment Resource:NumericalData
12-second Editor-B low-energy particle data from the Geotail spacecraft. Editor-A data are only acquired with the real-time operation in Usuda Deep Space Center (UDSC),Japan, while the Editor-B data are 24-hours continuouslyrecorded in the onboard tape recorders and are dumpedover the NASA/JPL Deep Space Network (DSN) stations. The ion energy analyzer (LEP-EAi) has two energy scan mode: RAM-A (60 eV to 40 keV) and RAM-B (5 keV to 40 keV). RAM-B is selected to protect the very sensitive detector from intense low energy fluxes that are usually seen in the solar wind and magnetosheath. The energy scan mode is automatically selected onboard depending on incoming ion fluxes. At present, only the ion moments in the RAM-A mode are listed for the LEP-EAi data. The ion moment data of the solar wind analyzer (LEP-SW) should be used only qualitatively. The LEP-SW ion moments are listed when the energy scan mode of LEP-EAi is RAM-B.

31) Geotail MGF CPI 1-min field and plasma data at bow shock nose maxmize
Resource ID:spase://VMO/NumericalData/Geotail/Propagated/PT1M
Start:1995-01-01 00:00:00 Observatory:Geotail Cadence:1 minute
Stop:2006-12-31 23:59:59 Instrument:Geotail MGF Resource:NumericalData
Solar wind magnetic field and plasma data at 1-min resolution created from Geotail data shifted to the Earth's bow shock nose (BSN).

32) IMP 8 MIT Full Resolution Definitive Interplanetary Plasma Data maxmize
Resource ID:spase://VMO/NumericalData/IMP8/PLS/PT01M
Start:1973-10-31 20:10:26 Observatory:IMP 8 Cadence:01 minutes
Stop:2006-07-26 17:10:34 Instrument:IMP 8 Solar Plasma Faraday Cup Resource:NumericalData
The MIT Faraday cup experiment on IMP 8 measures currents from solar wind ions, and from these measurements we calculate the velocity, density, and temperature of the solar wind. The IMP 8 data files consist of fine resolution data (approximately 1 minute resolution). IMP 8 spins with a period of approximately 2.7s. The Faraday Cup (FC) instrument scans the solar wind distribution stepping through a contiguous set of energy windows, one step per spacecraft spin. The FC instrument divides the spin into thirty-two, 11.25 degree angular sectors and integrates the measured currents over different angular sectors depending upon the Mode in which the instrument is operating. The border between two of the 11.25 degree angular sectors lies on the Sun-spacecraft line. The FC sensor collector plate is divided into two, semi-circular halves; the division line is parallel to the spacecraft spin plane which is approximately parallel to the ecliptic plane. The split collector allow determination of the bulk plasma flow relative to the spin plane; North/South angles refer to flows coming from above or below the spin plane respectively (flows from the South are designated as having a positive N/S angle). The bulk flow angle in the spin plane is determined from the measurements of current vs. rotation angle. The currents telemetered to the ground are the sums of currents for the two half-collectors ("A" and "B") and, for the TMS and AQM modes, also the current for the half-collector "B". Electrons are measured except for the eight angles near the Sun. The experiment has two memories only one of which is operating perfectly. As a result, only every other TMS spectrum is usable, and the time between spectra is usually twice that that would be expected from the spacecraft spin rate. The bad half-memory also limits the energy windows that can be used in the other modes, since they require both memories to hold the data. On occasion, the data are read out rapidly enough by the spacecraft to allow repeated use of the good half-memory, and the time resolution in the TMS is approximately 32 seconds.

33) IMP 8 MAG PLS 1-min field and plasma data at bow shock nose maxmize
Resource ID:spase://VMO/NumericalData/IMP8/Propagated/PT1M
Start:1994-01-01 00:00:00 Observatory:IMP 8 Cadence:1 minute
Stop:2000-06-10 00:00:00 Instrument:IMP 8 Magnetic Field Experiment Resource:NumericalData
Solar wind magnetic field and plasma data at 1-min resolution created from IMP 8 data shifted to the Earth's bow shock nose (BSN).

34) ISEE 1 FPE plasma parameters, 6 Re to bow shock maxmize
Resource ID:spase://VMO/NumericalData/ISEE1/FPE/PT1M
Start:1977-10-29 00:00:00 Observatory:ISEE 1 Cadence:1 minute
Stop:1979-01-19 00:00:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
TBD

35) ISEE 1 Solar Wind Analyzer 24-s Plasma Parameters maxmize
Resource ID:spase://VMO/NumericalData/ISEE1/FPE/PT24S
Start:1977-10-30 00:00:00 Observatory:ISEE 1 Cadence:24 seconds
Stop:1984-01-30 00:00:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
This data set contains 24s (fast data rate) or 48s (slow rate) solar wind ion plasma parameters obtained during 1977-1983 solar wind seasons (~July - ~January) when the spacecraft's local time of apogee was on the Earth's dayside. Plasma parameters include ion density, flow speed, flow longitude and latitude angles, perpendicular (minimum) and parallel (maximum) temperatures, and alpha-to-proton density ratio. Data are available through the CDAWeb interface and, as daily files via ftp, in ASCII from nssdcftp and in CDF from CDAWeb's ftp area. The data are from LANL's Cross-Fan Solar Wind Ion Experiment, a companion to LANL's Fast Plasma Analyzer (FPE).

36) ISEE 1 VES Electron Data at 9s or 18s maxmize
Resource ID:spase://VMO/NumericalData/ISEE1/VES/PT18S
Start:1977-10-29 00:00:00 Observatory:ISEE 1 Cadence:18 seconds
Stop:1979-06-03 00:00:00 Instrument:ISEE 1 Vector Electron Spectrometer (VES) Resource:NumericalData
This data set, held in CDAWeb as ISEE1_H0_FE, contains electron moments from the Vector Electron Spectrometer (VES), and spacecraft position vectors, at 9s or 18s resolution, depending on spacecraft telemetry rate. The data set also holds 1-min averages of the measured magnetic field vector. Electron moments include density, flow velocity, temperature and its anisotropy, and heat flux vector. Also given are the pressure tensor, its diagonalizing eigenvector, and the angle between its principal axis and the ambient magnetic field vector. These parameters are based on distributions accumulated in 3 sec but telemetered over 9s or 18s. Ancillary information given includes the spacecraft spin period, the spacecraft potential, the energy channels above this potential on which the moments for this record were based, and on/off flags for the Harvey and Mozer experiments.

37) ISEE 2 FPE plasma parameters, 6 Re to bow shock maxmize
Resource ID:spase://VMO/NumericalData/ISEE2/FPE/PT1M
Start:1977-10-27 00:00:00 Observatory:ISEE 2 Cadence:1 minute
Stop:1979-01-19 00:00:00 Instrument:ISEE 2 Fast Plasma Experiment Resource:NumericalData
TBD

38) OMNI Daily Data Set maxmize
Resource ID:spase://VMO/NumericalData/OMNI/P1D
Start:1963-01-01 00:00:00 Observatory:OMNI Cadence:1 day
Stop:2014-10-22 01:03:21 Instrument:OMNI Instrument Resource:NumericalData
Daily averaged, multi-source, near-Earth solar wind magnetic field, plasma and energetic proton flux data, plus AE, AU, AL, Kp, ap, and Dst geomagnetic indices, Polar Cap (Thule) index, F10.7 index, and Rz (sunspot number). Also available at 1-hour and 27-day resolution.

39) OMNI 27-Day Data Set maxmize
Resource ID:spase://VMO/NumericalData/OMNI/P27D
Start:1963-11-02 00:00:00 Observatory:OMNI Cadence:27 days
Stop:2014-10-22 01:03:21 Instrument:OMNI Instrument Resource:NumericalData
27-day averaged, multi-source, near-Earth solar wind magnetic field, plasma and energetic proton flux data, plus AE, AU, AL, Kp, ap, and Dst geomagnetic indices, Polar Cap (Thule) index, F10.7 index, and Rz (sunspot number). Also available at 1-hour and 1-day resolution.

40) OMNI Hourly Data Set maxmize
Resource ID:spase://VMO/NumericalData/OMNI/PT1H
Start:1963-01-01 00:00:00 Observatory:OMNI Cadence:1 hour
Stop:2014-10-22 01:03:21 Instrument:OMNI Instrument Resource:NumericalData
Hourly averaged, multi-source, near-Earth solar wind magnetic field, plasma and energetic proton flux data, plus AE, AU, AL, Kp, ap, and Dst geomagnetic indices, Polar Cap (Thule) index, F10.7 index, and Rz (sunspot number). Also available at 1-day and 27-day resolution.

41) OMNI 1-min Data Set maxmize
Resource ID:spase://VMO/NumericalData/OMNI/PT1M
Start:1995-01-01 00:00:00 Observatory:OMNI Cadence:1 minute
Stop:2014-10-22 01:03:21 Instrument:OMNI Instrument Resource:NumericalData
High resolution (1-min), multi-source, near-Earth solar wind magnetic field and plasma data as shifted to Earth's bow shock nose, plus several 1-min geomagnetic activity indices.

42) OMNI 5-min Data Set maxmize
Resource ID:spase://VMO/NumericalData/OMNI/PT5M
Start:1995-01-01 00:00:00 Observatory:OMNI Cadence:5 minutes
Stop:2014-10-22 01:03:21 Instrument:OMNI Instrument Resource:NumericalData
Solar wind magnetic field and plasma data at 5-min resolution created from HRO-1 which was in turn created from ACE, Wind and IMP 8 data shifted to the Earth's bow shock nose.

43) PolarEFI_Burst_SC_Potential_PlasmaDensity maxmize
Resource ID: spase://VWO/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Burst
Start:1996-03-16 00:00:00 Observatory: Cadence:6 seconds
Stop:2008-04-13 00:00:00 Instrument: Resource:NumericalData
This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft burst resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler.

44) PolarEFI_Burst_SC_Potential_PlasmaDensity maxmize
Resource ID: spase://SMWG/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Burst
Start:1996-03-16 00:00:00 Observatory: Cadence:6 seconds
Stop:2008-04-13 00:00:00 Instrument: Resource:NumericalData
This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft burst resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler.

45) PolarEFI_Realtime_SC_Potential_PlasmaDensity maxmize
Resource ID: spase://VWO/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Realtime
Start:1996-03-16 00:00:00 Observatory: Cadence:6 seconds
Stop:2008-04-13 00:00:00 Instrument: Resource:NumericalData
This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft realtime resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler.

46) PolarEFI_Realtime_SC_Potential_PlasmaDensity maxmize
Resource ID: spase://SMWG/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Realtime
Start:1996-03-16 00:00:00 Observatory: Cadence:6 seconds
Stop:2008-04-13 00:00:00 Instrument: Resource:NumericalData
This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft realtime resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler.

47) PolarEFI_SpinResolution_SC_Potential_PlasmaDensity maxmize
Resource ID: spase://SMWG/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Spin
Start:1996-03-16 00:00:00 Observatory: Cadence:6 seconds
Stop:2008-04-13 00:00:00 Instrument: Resource:NumericalData
This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft spin resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler.

48) PolarEFI_SpinResolution_SC_Potential_PlasmaDensity maxmize
Resource ID: spase://VWO/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Spin
Start:1996-03-16 00:00:00 Observatory: Cadence:6 seconds
Stop:2008-04-13 00:00:00 Instrument: Resource:NumericalData
This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft spin resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler.

49) Polar TIDE 6-s H, He, O Data maxmize
Resource ID:spase://VMO/NumericalData/POLAR/TIDE/H0-CDF
Start:1996-03-27 00:00:00 Observatory:POLAR Cadence:6.00 seconds
Stop:1996-12-07 23:59:59 Instrument:Thermal Ion Dynamics Experiment (TIDE) Resource:NumericalData
The TIDE H0 CDF files contain H+, O+, and He+ data below 411 eV. Data are available for 1996-03-27 through 1996-09-30. Data is accumulated over the 6-second Polar spacecraft spin. For each ion, the files contain moments density, velocity (Vx, Vy, Vz), temperature (T_perp and T_para) and spectogram for differential energy flux versus energy (flux averaged over spin and polar angle), differential energy flux versus spin angle (flux averaged over energy and polar angle), and differential energy flux versus polar angle (flux averaged over energy and spin angle). Support data includes EFI spacecraft potential (adjusted by +2 volts), magnetic field location, spacecraft ram direction, plotting information, and several parameters that describe the instrument status and details about the data processing.

50) Polar TIDE Level-zero telemetry files maxmize
Resource ID:spase://VMO/NumericalData/POLAR/TIDE/Level-zero
Start:1996-03-27 00:00:00 Observatory:POLAR Cadence:9.2 seconds
Stop:2008-04-16 23:59:59 Instrument:Thermal Ion Dynamics Experiment (TIDE) Resource:NumericalData
TIDE level-zero processing software provides several analysis and display options with an extensive list of processing options. The TIDE team has provided websites that allow users to process data from the web and then download the processed datafiles and plots, see the Custom Plot and Data Dump links on one of the TIDE Home Pages. The software (C and IDL) can be downloaded and installed locally. There is a data download page that can be used to get the level-zero data and the required ancillary data (Polar orbit and attitude, extracted EFI spacecraft potential, and ion masks). NOTE: The only way to read a TIDE level-zero file is with the processing software. See the TIDE Documentation link on one of the two TIDE Home Pages for documentation of the processing software and the input file data formats. See the parameters below for more information about key elements in the level-zero processing.

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