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1) ACE 27-day Survey Plots maxmize
Resource ID:spase://VSPO/DisplayData/ACE/MAG/27-Day
Start:1997-08-25 00:00:00 Observatory:ACE Cadence:
Stop:2016-09-14 07:59:49 Instrument:ACE Magnetic Field Instrument Resource:DisplayData
27-day gif_walk plots, selected ACE mag field and plasma data

2) ACE Daily Survey Plots maxmize
Resource ID:spase://VSPO/DisplayData/ACE/MAG/Daily
Start:1997-09-02 00:00:00 Observatory:ACE Cadence:
Stop:2016-09-14 07:59:49 Instrument:ACE Magnetic Field Instrument Resource:DisplayData
Daily gif_walk plots, ACE mag field and plasma data

3) ACE field and plasma data propagated to (17,0,0) Re maxmize
Resource ID:spase://VSPO/NumericalData/ACE/MAG_SWEPAM/PT1M
Start:1998-02-05 00:00:00 Observatory:ACE Cadence:1 minute
Stop:2016-09-14 07:52:05 Instrument:ACE Magnetic Field Instrument Resource:NumericalData
This is a family of data sets containing 1-min resolution ACE magnetic field and plasma parameters, in GSE and GSM coordinates, both at the location of the ACE spacecraft and as propagated to the location (17,0,0) Re, GSE. Magnetic field and plasma data are from the ACE MFI and SWEPAM instruments, respectively. Propagation was done by J. Weygand using software provided by D. Weimer. The software determines normal directions to assumed planar phase fronts using a modified minimum variance analysis of 1-min magnetic field data, and propagates data using these normals and the Wind-observed solar wind flow velocity. Magnetic field data consist of three Cartesian components, while plasma data consist of three Cartesian components of the flow velocity vector plus proton density and temperature. Data are current to within about 8 months. Different subdirectories hold data for unique combinations of field vs. plasma parameters, GSE vs. GSM coordinates, and unpropagated vs. propagated data. See the VMO interface for a more detailed breakout.

4) ACE MAG SWEPAM 4-min merged IMF+plasma data maxmize
Resource ID:spase://VSPO/NumericalData/ACE/MAG_SWEPAM/PT240S
Start:1998-02-05 00:00:00 Observatory:ACE Cadence:240 seconds
Stop:2016-09-14 08:00:05 Instrument:ACE Solar Wind Electron, Proton and Alpha Monitor (SWEPAM) Resource:NumericalData
ACE MAG and SWEPAM 4-min merged magnetic field and plasma parameter moments data at NSSDC

5) ACE MAG SWEPAM L2 64-s merged IMF+plasma data maxmize
Resource ID:spase://VSPO/NumericalData/ACE/MAG_SWEPAM/PT64S
Start:1998-02-05 00:00:00 Observatory:ACE Cadence:64 seconds
Stop:2016-09-14 08:00:05 Instrument:ACE Solar Wind Electron, Proton and Alpha Monitor (SWEPAM) Resource:NumericalData
ACE MAG and SWEPAM L2 64-s merged magnetic field and plasma parameter moments data at ASC

6) ACE SWEPAM STEA Electron Pitch Angle Plots maxmize
Resource ID:spase://VSPO/DisplayData/ACE/SWEPAM/PLOTS
Start:1997-10-27 00:00:00 Observatory:ACE Cadence:
Stop:2016-09-14 07:59:49 Instrument:ACE Solar Wind Electron, Proton and Alpha Monitor (SWEPAM) Resource:DisplayData
ACE SWEPAM STEA electron pitch angle plots, 12 hours per frame, 10 energy channels from 73 eV to 1.73 keV, one panel per energy channel

7) ACE SWEPAM 5-min Key Parameter (recent) data maxmize
Resource ID:spase://VSPO/NumericalData/ACE/SWEPAM/PT300S
Start:2002-07-01 00:00:00 Observatory:ACE Cadence:300 seconds
Stop:2016-09-14 08:00:05 Instrument:ACE Solar Wind Electron, Proton and Alpha Monitor (SWEPAM) Resource:NumericalData
ACE SWEPAM Solar Wind Plasma Experiment 5-Minute Key Parameters [PRELIM]

8) ACE SWEPAM L2 hourly plasma parameter data maxmize
Resource ID:spase://VSPO/NumericalData/ACE/SWEPAM/PT3600S
Start:1998-02-05 00:00:00 Observatory:ACE Cadence:3600 seconds
Stop:2016-09-14 08:00:05 Instrument:ACE Solar Wind Electron, Proton and Alpha Monitor (SWEPAM) Resource:NumericalData
ACE SWEPAM L2 1-hr, 1-day and 27-day plasma parameter moments averages at ASC

9) ACE SWEPAM/SWICS Level 3 Merged Solar Wind Proton Data maxmize
Resource ID:spase://VSPO/NumericalData/ACE/SWEPAM/SWICS/PT12M
Start:1998-01-28 00:00:12 Observatory:ACE Cadence:12 minutes
Stop:2016-09-14 08:00:05 Instrument:ACE Solar Wind Electron, Proton and Alpha Monitor (SWEPAM) Resource:NumericalData
These data files contain 12-min resolution solar wind proton flow velocity (GSE, RTN and GSM components), scalar speed, density, and (radial component of) temperature, plus the alpha particle to proton density ratio. The data are typically from the SWEPAM instrument. But because SWEPAM has reduced sensitivity at the lowest energies, and at times underestimates the proton density, especially for very slow wind, proton density is sometimes culled from low-speed (.LT. ~350 km/s) intervals in the SWEPAM Level 2 data, and proton temperature may also be culled. More rarely, the solar wind velocity may also be culled, especially during periods of both high solar energetic particle background and high wind speeds. In these cases, SWICS-determined proton density and temperature, and possibly also flow speed (not velocity vectors), are included in the data records, with a flag to indicate whether, and which, SWICS parameters are in the records. As of July, 2012, data were available to the end of 2009.

10) ACE SWICS 2.0 Solar Wind 2-Hour Data maxmize
Resource ID:spase://VSPO/NumericalData/ACE/SWICS/L2/PT2H
Start:2012-06-01 00:00:00 Observatory:ACE Cadence:2 hours
Stop:2016-09-14 08:00:05 Instrument:Solar Wind Ion Composition Spectrometer (SWICS) Resource:NumericalData
The SWICS 2.0 dataset consists of time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic distribution of heavy ions in the solar wind. This data set begins after August 23, 2011, when a radiation and age-induced hardware anomaly altered the instrument's operational state. It should not be confused with SWICS 1.1, the recalibrated data set extending from launch up to the anomaly. SWICS 2.0 continues to make heavy ion measurements which are not available from any other instrument, and new data analysis methods have been developed to address the statistical and calibration issues of the current instrument state.

11) ACE SWICS Solar Wind Data from the ACE Science Center maxmize
Resource ID:spase://VSPO/NumericalData/ACE/SWICS_SWIMS/L2/HDF
Start:1998-02-04 00:00:00 Observatory:ACE Cadence:
Stop:2016-09-14 08:00:05 Instrument:Solar Wind Ion Mass Spectrometer (SWIMS) Resource:NumericalData
The Solar Wind Ion Composition Spectrometer (SWICS) Solar Wind Data set consists of time series measurements of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind. Time resolutions: 1 hour, 2 hour, and 1 day. (Not all products are delivered at all time-resolutions.) This descriptor comprises two sets of data: (1)The SWICS 1.1 data set which covers launch up to August 23, 2011, when a radiation and age-induced hardware anomaly altered the instrument's operational state. (2)The SWICS 2.0 data set which begins after August 23, 2011, and includes a subset of the items included in the SWICS 1.1 data set, as well as the O+8/O+6 ratio.

12) ACE SWICS 1.1 Solar Wind Daily-averaged Data maxmize
Resource ID:spase://VSPO/NumericalData/ACE/SWICS_SWIMS/L2/PT24HR
Start:1998-01-01 00:00:00 Observatory:ACE Cadence:24 hours
Stop:2011-08-23 00:00:00 Instrument:Solar Wind Ion Mass Spectrometer (SWIMS) Resource:NumericalData
This ACE SWICS 1.1 data set contains Solar Wind Ion Composition Spectrometer (SWICS) level-2 daily averaged solar wind parameters, including composition (He/O, C/O, N/O, Ne/O, Mg/O, Si/O, S/O, Fe/O), bulk ion speed (He+2) and charge states (C+6/C+5, O+7/O+6 Carbon, Oxygen, Fe) at all solar wind speeds above 300 km/s (protons) and 170 km/s (Fe+16). Distribution functions of H and He isotopes are measured of both solar and interstellar sources up to energies of 100 keV/e. Please note the N/O and S/O composition data are not present in the 1-hour or 2-hour SWICS datasets. This SWICS 1.1 dataset consists of a re-release of significantly improved time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind. It is a major new version produced with completely redesigned analysis methods to account more rigorously for instrumental and statistical effects (Shearer et al. 2014). Rare elements are now identified more reliably and estimates of statistical error are provided. These release notes describe the data, the methods used to determine them, and issues of data quality and measurement uncertainty.

13) ACE SWICS 1.1 Solar Wind 2-Hour Data maxmize
Resource ID:spase://VSPO/NumericalData/ACE/SWICS_SWIMS/L2/PT2HR
Start:1998-01-01 00:00:00 Observatory:ACE Cadence:2 hours
Stop:2011-08-23 00:00:00 Instrument:Solar Wind Ion Mass Spectrometer (SWIMS) Resource:NumericalData
This ACE SWICS 1.1 data set contains Solar Wind Ion Composition Spectrometer (SWICS) level-2 2-hr averaged solar wind parameters, including density (He+2), bulk and thermal ion speeds (He+2, C+5, O+6, Fe+10), composition (He/O, C/O, Ne/O, Mg/O, Si/O, Fe/O), and charge states (C+6/C+5, O+7/O+6 Carbon, Oxygen, Fe, Ne, Mg, Si) and solar wind type indicators at all solar wind speeds above 300 km/s (protons) and 170 km/s (Fe+16). Distribution functions of H and He isotopes are measured of both solar and interstellar sources up to energies of 100 keV/e. This SWICS 1.1 dataset consists of a re-release of significantly improved time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind. It is a major new version produced with completely redesigned analysis methods to account more rigorously for instrumental and statistical effects (Shearer et al. 2014). Rare elements are now identified more reliably and estimates of statistical error are provided. These release notes describe the data, the methods used to determine them, and issues of data quality and measurement uncertainty.

14) ACE SWICS 1.1 Solar Wind 2-Hour Q-State Distribution Data maxmize
Resource ID:spase://VSPO/NumericalData/ACE/SWICS_SWIMS/L2/PT2HR_QState
Start:1998-02-04 00:00:00 Observatory:ACE Cadence:2 hours
Stop:2011-08-23 00:00:00 Instrument:Solar Wind Ion Mass Spectrometer (SWIMS) Resource:NumericalData
This ACE SWICS 1.1 data set contains Solar Wind Ion Composition Spectrometer (SWICS) level-2 2-hr data of actual Q-state distributions of carbon, oxygen, neon, magnesium, silicon and iron, as opposed to the averaged Q-states that have been available on CDAWeb for some time. This SWICS 1.1 dataset consists of a re-release of significantly improved time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind. It is a major new version produced with completely redesigned analysis methods to account more rigorously for instrumental and statistical effects (Shearer et al. 2014). Rare elements are now identified more reliably and estimates of statistical error are provided. These release notes describe the data, the methods used to determine them, and issues of data quality and measurement uncertainty.

15) ACE SWICS 1.1 Solar Wind 1-Hour Data maxmize
Resource ID:spase://VSPO/NumericalData/ACE/SWICS_SWIMS/L2/PT3600S
Start:1998-01-23 00:00:00 Observatory:ACE Cadence:3600 seconds
Stop:2011-08-23 00:00:00 Instrument:Solar Wind Ion Mass Spectrometer (SWIMS) Resource:NumericalData
ACE SWICS_SWIMS 1.1 L2 1-hr, 1-d, 27-d solar wind He, Mg, O, Fe TnV data, plus species ratios and charge states, at ASC. This SWICS 1.1 dataset consists of a re-release of significantly improved time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic properties of heavy ions in the solar wind. It is a major new version produced with completely redesigned analysis methods to account more rigorously for instrumental and statistical effects (Shearer et al. 2014). Rare elements are now identified more reliably and estimates of statistical error are provided. These release notes describe the data, the methods used to determine them, and issues of data quality and measurement uncertainty.

16) AE-C 15-s Unified Abstract data maxmize
Resource ID:spase://VSPO/NumericalData/AE-C/PT15S
Start:1973-12-16 00:00:00 Observatory:AE-C Cadence:15 seconds
Stop:1978-12-11 00:00:00 Instrument:Retarding Potential Analyser/Drift Meter (RPA) Resource:NumericalData
Atmospheric Explorer (AE)-C 15-s aeronomy data from all experiments, including electron, ion and neutral densities, temperatures, composition and winds, and airglow emissions

17) AE-D 15-s Unified Abstract data maxmize
Resource ID:spase://VSPO/NumericalData/AE-D/PT15S
Start:1975-10-06 00:00:00 Observatory:AE-D Cadence:15 seconds
Stop:1976-01-29 00:00:00 Instrument:Retarding Potential Analyzer/Drift Meter Resource:NumericalData
Atmospheric Explorer (AE)-D 15-s aeronomy data from all experiments, including electron, ion and neutral densities, temperatures, composition and winds, and airglow emissions

18) AE-E MSIS Neutral Density Data maxmize
Resource ID:spase://VSPO/NumericalData/AE-E/BIMS_OSS/PT256S
Start:1977-07-01 00:00:00 Observatory:AE-E Cadence:256 seconds
Stop:1981-06-09 23:59:59 Instrument:Bennett Ion-Mass Spectrometer (BIMS) Resource:NumericalData
This set of neutral density data was deduced from the mass spectrometer measurements on the Atmosphere Explorer E's Bennett Ion-Mass Spectrometer and Open-Source Neutral Mass Spectrometer. The density numbers (in cm-3) for hydrogen, nitrogen and molecular oxygen were provided by A. Hedin (GSFC, Code 914, now retired). They are related to A. Hedin's atmospheric modelling work (Mass Spectrometer and Incoherent Scatter atmospheric model - MSIS). In addition to density, the record includes also orbital parameters.

19) AE-E 15-s Unified Abstract data maxmize
Resource ID:spase://VSPO/NumericalData/AE-E/PT15S
Start:1975-12-11 00:00:00 Observatory:AE-E Cadence:15 seconds
Stop:1981-06-06 00:00:00 Instrument:Retarding Potential Analyzer/Drift Meter Resource:NumericalData
Atmospheric Explorer (AE)-E 15-s aeronomy data from all experiments, including electron, ion and neutral densities, temperatures, composition and winds, and airglow emissions

20) 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.

21) AEROS-A RPA ion and electron data maxmize
Resource ID:spase://VSPO/NumericalData/Aeros-A/RPA/PT5S
Start:1973-01-03 00:00:00 Observatory:Aeros-A Cadence:5 seconds
Stop:1973-08-03 00:00:00 Instrument:Energy Distribution of Ions and Electrons Resource:NumericalData
AEROS-A RPA ionospheric ion composition and temperature and electron density and temperature data; variable resolution as fine as 5-s

22) Akebono LEP ion and electron spectral plots maxmize
Resource ID:spase://VSPO/DisplayData/Akebono/LEP/PT8S
Start:1989-04-15 00:00:00 Observatory:Akebono Cadence:8 seconds
Stop:1997-12-26 00:00:00 Instrument:Low Energy Particle Instrument (LEP) Resource:NumericalData
These data consist of plots of color-coded ion and electron count rates vs. energy and time, in each of several pitch angle bins. The energy ranges are 13ev/Q to 20keV/Q (ions) and 10eV to 16keV (electrons). Each plot covers some or all of one ~3.5 hour orbit. ASCII data are also accessible.

23) Akebono LEP ion and electron count rates maxmize
Resource ID:spase://VSPO/NumericalData/Akebono/LEP/PT8S
Start:1989-04-15 00:00:00 Observatory:Akebono Cadence:8 seconds
Stop:1997-12-26 00:00:00 Instrument:Low Energy Particle Instrument (LEP) Resource:NumericalData
These data consist of ion and electron count rates taken in 18 pitch angle directions and in 29 energy channels between 10eV and 16keV (electrons) or 13ev/Q and 20keV/Q (ions). A full distribution is available each 8 seconds. Through the DARTS/LEP interface, one specifies a particular 10-deg-wide pitch angle bin and retrieves tables of ion and electron count rates with columns for the energy channels and one row for each 8-sec interval. There are companiog plots with spectrograms showing count rates vs. energy and time, one such plot for each of several ~30deg-wine pitch angle bins

24) Akebono TED thermal electron spectral plots maxmize
Resource ID:spase://VSPO/DisplayData/Akebono/TED/PT8S
Start:1989-03-01 00:00:00 Observatory:Akebono Cadence:8 seconds
Stop:1998-12-26 00:00:00 Instrument:Akebono Thermal Electron Energy Distribution (TED) Resource:NumericalData
These Akebono Thermal Electron Energy Detecftor (TED) plots display color-coded amplitudes of the second harmonic of incident flux, vs. energy (over 0-5 eV) and time. Each plot covers some or all of one ~3.5 hour orbit.

25) Akebono TED thermal electron digital spectra maxmize
Resource ID:spase://VSPO/NumericalData/Akebono/TED/PT8S
Start:1989-03-01 00:00:00 Observatory:Akebono Cadence:8 seconds
Stop:1998-12-26 00:00:00 Instrument:Akebono Thermal Electron Energy Distribution (TED) Resource:NumericalData
These Akebono Thermal Electron Energy Detecftor (TED) digital data reside at the DARTS/Akebono binary Science Database (SDB). They consist of amplitudes of the second harmonic of incident flux. Data-read software and an algorithms for converting the data to an energy distribution function in units of 1/(eV cm**3) are given in the Information URL cited below.

26) Alouette 1 Topside Electron Density Profiles Manually Scaled at CRC maxmize
Resource ID:spase://VSPO/NumericalData/Alouette1/SFS/PT32S
Start:1962-09-29 19:41:03 Observatory:Alouette 1 Cadence:32 seconds
Stop:1971-12-16 22:20:25 Instrument:Alouette 1 Sweep-Frequency Sounder Resource:NumericalData
This data set, provided by the Communications Research Centre (CRC) in Ottawa, Canada, consists of electron density profiles derived from Alouette 1 Sweep-Frequency Sounder measurements for the ionosphere above the F2 maximum (topside ionosphere). The data set is in chronological order, and includes about 27,000 profiles obtained primarily during the period 1963 to 1967. The electron density profiles were computed from digital values of frequency and virtual height, which had in turn been scaled from the ionograms. Profiles were selected because of their scientific interest. Telemetry stations are not identified, but satellite location, time of observation, solar zenith angle at the satellite, magnetic dip at the satellite, total content down to the lowest altitude of topside ionospheric reflection, and other relevant information are listed for each profile. The format gives sequences of numbers for each point scaled from the ionogram. These sequences include electron density at the successive points, and the coefficients a2, b3, b4, b5, etc. from which geometric heights can be calculated, using formulas 40 and 41 in J. E. Jackson, "The reduction of topside ionograms to electron-density profiles," Proceedings of the IEEE., p. 960, June 1969. These formulas can also be used to calculate interpolated density-height values. A CRC interpolation program (available at NSSDC) can be used with this data set. These data make up a very small portion of the recorded Alouette 1 ionograms. Latitudinal coverage is widespread, but data at longitudes near 80 deg W are more numerous than others. The data were originally provided on 9-track, 1600-bpi, odd-parity, EBCDIC tape written on a MODCOMP-4 computer. NSSDC prepared an ASCII version using the Jackson formulas to compute electron density profiles.

27) Alouette 2 electron density data maxmize
Resource ID:spase://VSPO/NumericalData/Alouette2/CEP/PT60S
Start:1966-02-21 00:00:00 Observatory:Alouette 2 Cadence:60 seconds
Stop:1967-02-16 00:00:00 Instrument:Cylindrical Electrostatic Probes Resource:NumericalData
Alouette 2 ionospheric electron density data at 1-5 min resolution

28) Alouette 2 Topside Sounder Ionogram Over Multiple Stations maxmize
Resource ID:spase://VSPO/NumericalData/Alouette2/SFS/Ionograms
Start:1965-11-29 13:42:37 Observatory:Alouette 2 Cadence:
Stop:1968-01-01 04:12:17 Instrument:Alouette 2 Sweep-Frequency Sounder Resource:NumericalData
This data set consists of ionograms derived from Alouette 2 Sweep-Frequency Sounder measurements for the ionosphere above the F2 maximum (topside ionosphere). These ionograms are reduced data plots showing as a function of fixed and swept frequency the echo time delay (virtual range) of pulsed radio signals at 355 virtual heights. They were converted from the original analog telemetry tapes covering various stations: Winkfield, U.K. (lat/lon=51/359); Quito, Ecuador (lat/lon=-1/281); Lima, Peru (Lat=-12, Long=283); Santiago, Chile (lat/lon=-33/298); and Falkland Is., U.K. (lat/lon=-52/302).

29) Alouette 2 Topside Electron Density Profiles Manually Scaled at CRC maxmize
Resource ID:spase://VSPO/NumericalData/Alouette2/SFS/PT32S
Start:1965-12-15 09:40:15 Observatory:Alouette 2 Cadence:32 seconds
Stop:1972-07-10 22:37:22 Instrument:Alouette 2 Sweep-Frequency Sounder Resource:NumericalData
This data set, provided by the Communications Research Centre (CRC) in Ottawa, Canada, consists of electron density profiles derived from Alouette 2 Sweep-Frequency Sounder for the ionosphere above the F2 maximum (topside ionosphere). The data set was originally provided on an EBCDIC magnetic tape written on an IBM 360 computer. The electron density profiles were computed from digital values of frequency and virtual height, scaled from ionograms. The data are ordered chronologically and include about 11,000 profiles. Telemetry stations are not identified, but satellite location, Greenwich mean time of observation, solar zenith angle at the satellite, dip latitude at the satellite, total electron content down to the lowest height of topside signal reflection (normally near 300 km), and other relevant information is noted with each profile. The format gives sequences of numbers for each point scaled from the ionogram. These sequences include electron density at the successive points, and the coefficients a2, b3, b4, b5, etc. from which geometric heights can be calculated, using formulas 40 and 41 in J. E. Jackson, "The reduction of topside ionograms to electron-density profiles," Proceedings of the IEEE., p. 960, June 1969. These formulas can also be used to calculate interpolated density-height values. A CRC interpolation program available at NSSDC can be used with this data set. The ionograms were selected for their scientific interest and comprise only a very small portion of reductions possible from the available ionograms. Data obtained prior to March 9, 1970, are also available on microfiche from NSSDC.

30) Apollo 12 Solar Wind Measurements at the Lunar Surface 1-HR Data maxmize
Resource ID:spase://VSPO/NumericalData/Apollo12-LM/SWS/PT1HR
Start:1969-11-19 19:30:00 Observatory:Apollo 12 Lunar Module/ALSEP Cadence:60 minutes
Stop:1976-03-25 08:30:00 Instrument:Solar Wind Spectrometer Resource:NumericalData
This data set contains hourly averaged plasma parameters from the Apollo 12 Solar Wind Spectrometer. Four sets of hourly averaged parameters are computed, using as input data -- (1) all fine-time scale parameters (FTSP), (2) all FTSP computed from spectra with small rms error on curve fitting and thermal speeds less than one-half the bulk velocity, (3) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having only one flow angle that can be directly measured, and (4) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having both flow angles directly measureable. Contained in each of the 4 sets of averages are the proton density, alpha-to-proton ratio, bulk speed, angle of flow, number of spectra, and rms deviations of each average.

31) Apollo 12 Solar Wind Measurements at the Lunar Surface 28-s Data maxmize
Resource ID:spase://VSPO/NumericalData/Apollo12-LM/SWS/PT28S
Start:1969-11-19 18:42:13 Observatory:Apollo 12 Lunar Module/ALSEP Cadence:28 seconds
Stop:1976-03-25 08:35:57 Instrument:Solar Wind Spectrometer Resource:NumericalData
This data set contains the highest time resolution plasma data available (28 sec per spectrum) from the solar wind experiment onboard Apollo 12. Contained in each record are: time, proton density, alpha-to-proton ratio, bulk speed, angle of flow, most probable thermal speed, and various housekeeping and fit parameters relating to the reliability of the calculated plasma parameters. During the local lunar night there is no solar wind signal so there are data gaps of about 15 days each lunation.

32) Apollo 15 Solar Wind Measurements at the Lunar Surface 1-HR Data maxmize
Resource ID:spase://VSPO/NumericalData/Apollo15-LM/SWS/PT1HR
Start:1971-07-31 19:30:00 Observatory:Apollo 15 Lunar Module/ALSEP Cadence:60 minutes
Stop:1972-06-30 17:30:00 Instrument:Solar Wind Spectrometer Resource:NumericalData
This data set contains hourly averaged plasma parameters from the Apollo 15 Solar Wind Spectrometer. Four sets of hourly averaged parameters are computed, using as input data -- (1) all fine-time scale parameters (FTSP), (2) all FTSP computed from spectra with small rms error on curve fitting and thermal speeds less than one-half the bulk velocity, (3) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having only one flow angle that can be directly measured, and (4) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having both flow angles directly measureable. Contained in each of the 4 sets of averages are the proton density, alpha-to-proton ratio, bulk speed, angle of flow, number of spectra, and rms deviations of each average.

33) Apollo 15 Solar Wind Measurements at the Lunar Surface 28-s Data maxmize
Resource ID:spase://VSPO/NumericalData/Apollo15-LM/SWS/PT28S
Start:1971-07-31 19:38:38 Observatory:Apollo 15 Lunar Module/ALSEP Cadence:28 seconds
Stop:1972-06-30 18:14:35 Instrument:Solar Wind Spectrometer Resource:NumericalData
This data set contains the highest time resolution plasma data available (28 sec per spectrum) from the solar wind experiment onboard Apollo 15. Contained in each record are: time, proton density, alpha-to-proton ratio, bulk speed, angle of flow, most probable thermal speed, and various housekeeping and fit parameters relating to the reliability of the calculated plasma parameters. During the local lunar night there is no solar wind signal so there are data gaps of about 15 days each lunation.

34) ARCAD Particle Flux Data maxmize
Resource ID:spase://VSPO/NumericalData/Aureol3/RIEP-2802/PT0.30S
Start:1981-10-01 00:00:00 Observatory:Aureol 3 Cadence:0.30 seconds
Stop:1982-03-01 00:00:00 Instrument:Kukushka Soft Particle Spectrometer Resource:NumericalData
ARCAD low energy electron and proton flux data at 0.3 s resolution; altitude < 2000 km, near polar

35) CCMC: Heliospheric Model Results maxmize
Resource ID:spase://VSPO/NumericalData/CCMC/Heliospheric-Model/Results
Start: Observatory: Cadence:
Stop: Instrument: Resource:NumericalData
Results of runs of heliospheric models at CCMC

36) CCMC: Ionosphere/Atmosphere Model Results maxmize
Resource ID:spase://VSPO/NumericalData/CCMC/Ionospheric-Model/Results
Start: Observatory: Cadence:
Stop: Instrument: Resource:NumericalData
Results of runs of ionosphere/atmosphere models (SAMI2, CTIP) at CCMC

37) CCMC: Magnetospheric Model Results maxmize
Resource ID:spase://VSPO/NumericalData/CCMC/Magnetospheric-Model/Results
Start: Observatory: Cadence:
Stop: Instrument: Resource:NumericalData
Results of runs of magnetopheric models (BATSRUS, UCLA-GGCM) at CCMC

38) CHAMP data (all-inclusive) via CHAMP Data Center maxmize
Resource ID:spase://VSPO/NumericalData/CHAMP/PT1M
Start:2000-07-16 00:00:00 Observatory:CHAMP Cadence:1 minute
Stop:2016-09-14 08:00:05 Instrument:CHAMP Fluxgate Magnetometer Resource:NumericalData
A wealth of CHAMP data at various time resolutions and processing levels, including vector and scalar magnetic field data, coefficients for a CHAMP-based main magnetic field model, electron density profiles, etc., are available from the CHAMP Data Center which is hosted by ISDC (Information Systems and Data Center) at GFZ (GeoForschungsZentrum, Potsdam). Registration is required for open data access.

39) CNOFS CINDI IVM 500 ms Ion Drift Data maxmize
Resource ID:spase://VSPO/NumericalData/CNOFS/CINDI/IVM/PT0.5S
Start:2008-08-01 00:00:00 Observatory:Communication/Navigation Outage Forecasting System (C/NOFS) Cadence:0.5 seconds
Stop:2016-09-14 07:59:51 Instrument:Coupled Ion-Neutral Dynamics Investigation (CINDI) Resource:NumericalData
This data set contains plasma parameters of the equatorial F-region in the ionosphere measured by the Ion Velocity Meter (IVM) of the Coupled Ion-Neutral Dynamics Investigation (CINDI) payload on board the CNOFS spacecraft. Data are available in HDF format, with an IDL program to read and plot them. Each file contains data from one day of spacecraft operation and the file contains eight primary geophysical parameters: the ion temperature (Ti) in degrees Kelvin, the ion flow in m/s in the ram (i.e.--spacecraft velocity) direction (+Vx in the direction of spacecraft velocity), the ion flows in m/s in the horizontal and vertical directions (Vy and Vz) at right angles to the ram direction (+Vz is downward, +Vy is roughly southward), the total ion density (Ni) (the sum of O+ and H+ and He+ concentrations) in ions/cc, and the individual H+, He+, and O+ concentrations in ions/cc. In addition, ion velocities also are given in the coordinate system of the local magnetic field (parallel, perpendicular, and meridional) in the plots and as ASCII data on the UT Dallas website. Based on the IGRF model, the data are transformed into magnetic coordinates only if all three ion velocities in the spacecraft coordinates are available and good.

40) CNOFS PLP 1-sec plasma preliminary data maxmize
Resource ID:spase://VSPO/NumericalData/CNOFS/PLP/PT1S
Start:2008-05-09 00:00:00 Observatory:Communication/Navigation Outage Forecasting System (C/NOFS) Cadence:1 second
Stop:2008-09-14 18:34:58 Instrument:C/NOFS Planar Langmuir Probe (PLP) Resource:NumericalData
Plasma structures at 400-850km altitudes in the equatorial ionosphere have been measured by the C/NOFS Planar Langmuir Probe (PLP). This PLP data set contains 1-sec resolution ion number density and its standard deviation, electron density, electron temperature, spacecraft potential, and spacecraft position in geodetic coordinates. As of 5/13/2010, the data were preliminary.

41) CRRES Aerospace Agency Tape data maxmize
Resource ID:spase://VSPO/NumericalData/CRRES/PT60M
Start:1990-10-11 00:00:00 Observatory:CRRES Cadence:60 minutes
Stop:1991-10-13 00:00:00 Instrument:Electron-Proton-Angle-Spectrometer Resource:NumericalData
This data set includes files from the "Aerospace Agency Tapes" compiled by the Aerospace Corporation for selected experiments from the CRRES raw telemetry data stream provided through three digital processing units (DPUs) supporting Aerospace-related sensors. These sensors are as follows: the Magnetospheric Ion Composition Spectrometer (MICS), Heavy Ion Telescope (HIT), Low Energy Magnetospheric Ion Composition Sensor (LOMICS), the Medium Electrons A spectrometer (MEA), the Electron and Proton Wide-Angle Spectrometer (EPAS), the Relativistic Proton Detector (RPD), the Proton Switches (PS1, PS2), and a 4-band photometer for chemical release measurements. These instruments were turned on during Orbit 6, off at Orbit 365, and on again at Orbit 416 through the end of mission at Orbit 1067. When another complement of instruments called LASSII were periodically turned on for 20-minute or one-hour intervals near perigee for ionospheric measurements, the RADSAT (magnetospheric) complement, including the Aerospace instruments, were turned off. Spacecraft ephemeris, attitude, and magnetic field data are also provided. For each ten-hour orbit of CRRES includes a set of five files is provided from the original Agency tapes: header, ephemeris, attitude, magnetic field, and the Aerospace instrument raw data file. The magnetic field files are not those provided on the original Agency tapes but include field vector components in magnetometer sensor coordinates as computed from software and final calibration coefficients provided by the CRRES magnetometer team. The instrument data are provided at raw telemetry level in complex form, and users are requested to contact the responsible experimenters concerning correct usage. The binary data are encoded 32-bit words for reading on IBM-compatible PC's; byte order may need to be reversed for usage of other systems (e.g., VMS). FORTRAN source codes with PC-executables are provided to extract selected parameters from the spacecraft and instrument file types. References to documentation for the Aerospace instruments are listed in the main readme file.

42) Cluster Rumba Plasma Electrons and Currents Experiment (PEACE) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Rumba/PEACE/CSA/PT4S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2016-09-14 07:59:49 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The Plasma Electrons and Currents Experiment (PEACE) data products consist of prime and summary parameters (moments). Collected from two instruments, a low-energy electron analyzer (LEEA) and a high-energy electron analyzer (HEEA), the 3-D and 2-D data products contain the measured quantity in a suitable array, i.e., count rate, particle flux, particle energy flux or phase space density. The energy coverage is from 0.67 eV to 30 KeV in 92 levels. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. 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. Three categories of PEACE data are available from the Cluster Active Archive (CAA): three-dimensional distribution data, pitch angle distribution data, and electron moments data. (I) A variety of 3-D data products are produced by PEACE, but only one standard reduced resolution (compressed by a factor of 8) 3-D data (3DR) is routinely produced with a standard size that is independent of sweep mode. Other 3-D data include the flexible reduced polar resoluttion (3DXP); full resolution 3-D distributions (3DX, occasionally 3DXLAR for the "summed energy" data); and partial azimuth content data (3DXPA, 3DXPALAR). (II) Pitch angle distribution data include the standard spin rate pitch angle data (PITCH_SPIN), full time resolution pitch angle data (PITCH_FULL), and pitch angle data from various 3-D data (PITCH_3DR, PITCH_3DX, PITCH_3DXLAR, PITCH_3DXA, 3DXA_LAR). (III) For the electron moments data, the CAA provides the Prime Parameters which have some inherent limiations and the MOMENTS data which offer the highest quality moments, though not always at spin rate. The MOMENTS are Summary Parameters from 3-D data that include electron density, velocity vector, pressure tensor and heat flux vector. The vectors and tensors are provided in GSE coordinates. Velocity and temperature are also provided as components perpendicular and parallel to the magnetic field (where the magnetic field data is taken from CSDS FGM PP data, at present). Moments production software is provided by the PEACE team via the CAA to allow scientists to calculate their own moments if they wish, for example using a subset of the measured energies and polar zones. The Prime Parameters (PP) are derived from the onboard moment sums, which are converted to electron moments data (density, velocity, perpendicular and parallel temperature, parallel heat flux). The PP data are provided in the GSE coordinate system. Geometric factor updates based on in-flight calibration are used to correct for errors due to the less up-to-date onboard calibrations. It is recommended that the CAA Moments data (Summary Parameters) and not the PP data are preferred for science analysis, despite the reduced time resolution in some cases, and that use of the PP data is only made after careful consideration of their limitations. In addition to these three categories of products, there are onboard selected pitch angle data (PAD), onboard moments Sums (OMS) in both normal and burst modes, and other diagnostic data. For more details, see Chapter 8 of "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.

43) 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:2016-09-14 07:58:16 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.

44) Cluster Rumba Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Rumba/WHISPER/CSA/PT0.2S
Start:2001-02-02 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:0.2 seconds
Stop:2016-09-14 07:59:49 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
Two main types of data resulted from WHISPER (Waves of HF and Sounder for Probing Electron Density by Relaxation) onboard Cluster: the total electron density at standard time resolutions of either 2.15 or 52 s, and electric field spectra in the frequency range 2?82 KHz with time resolutions of 1.7 or 3.4 seconds. Data products available from the Cluster Active Archive include: electron number density, electric spectral power density (natural waves), electric spectral power density from active and passive emission during sounding, and electric waveform power density (energy) in 0.2 second resolution. Ancillary data include density comparisons with PEACE and CIS measurements onboard Cluster; sounding times; housekeeping data; electron density in spin-resolution (4 seconds) and 1 minute averages; electron gyrofrequency in plasmasphere; instrument parameters during natural mode and active mode; active to passive spectral power density coded ratio; and caveats. Please note that WHISPER densities are used for calibrations of CLUSTER instruments, in particular particle instruments, which have difficulties to measure the colder part of the population, and EFW instrument, because spacecraft potential variations, currently used as a proxy of density variations, depend not only on the density but also on the energy of electrons. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.

45) 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:2016-09-14 07:58:16 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.

46) Cluster II Salsa Plasma Electrons and Currents Experiment (PEACE) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Salsa/PEACE/CSA/PT4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2016-09-14 08:00:04 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The Plasma Electrons and Currents Experiment (PEACE) data products consist of prime and summary parameters (moments). Collected from two instruments, a low-energy electron analyzer (LEEA) and a high-energy electron analyzer (HEEA), the 3-D and 2-D data products contain the measured quantity in a suitable array, i.e., count rate, particle flux, particle energy flux or phase space density. The energy coverage is from 0.67 eV to 30 KeV in 92 levels. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. 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. Three categories of PEACE data are available from the Cluster Active Archive (CAA): three-dimensional distribution data, pitch angle distribution data, and electron moments data. (I) A variety of 3-D data products are produced by PEACE, but only one standard reduced resolution (compressed by a factor of 8) 3-D data (3DR) is routinely produced with a standard size that is independent of sweep mode. Other 3-D data include the flexible reduced polar resoluttion (3DXP); full resolution 3-D distributions (3DX, occasionally 3DXLAR for the "summed energy" data); and partial azimuth content data (3DXPA, 3DXPALAR). (II) Pitch angle distribution data include the standard spin rate pitch angle data (PITCH_SPIN), full time resolution pitch angle data (PITCH_FULL), and pitch angle data from various 3-D data (PITCH_3DR, PITCH_3DX, PITCH_3DXLAR, PITCH_3DXA, 3DXA_LAR). (III) For the electron moments data, the CAA provides the Prime Parameters which have some inherent limiations and the MOMENTS data which offer the highest quality moments, though not always at spin rate. The MOMENTS are Summary Parameters from 3-D data that include electron density, velocity vector, pressure tensor and heat flux vector. The vectors and tensors are provided in GSE coordinates. Velocity and temperature are also provided as components perpendicular and parallel to the magnetic field (where the magnetic field data is taken from CSDS FGM PP data, at present). Moments production software is provided by the PEACE team via the CAA to allow scientists to calculate their own moments if they wish, for example using a subset of the measured energies and polar zones. The Prime Parameters (PP) are derived from the onboard moment sums, which are converted to electron moments data (density, velocity, perpendicular and parallel temperature, parallel heat flux). The PP data are provided in the GSE coordinate system. Geometric factor updates based on in-flight calibration are used to correct for errors due to the less up-to-date onboard calibrations. It is recommended that the CAA Moments data (Summary Parameters) and not the PP data are preferred for science analysis, despite the reduced time resolution in some cases, and that use of the PP data is only made after careful consideration of their limitations. In addition to these three categories of products, there are onboard selected pitch angle data (PAD), onboard moments Sums (OMS) in both normal and burst modes, and other diagnostic data. For more details, see Chapter 8 of "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.

47) 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:2016-09-14 07:58:21 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.

48) Cluster Salsa Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Salsa/WHISPER/CSA/PT1S
Start:2001-02-02 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:1 second
Stop:2016-09-14 08:00:04 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
Two main types of data resulted from WHISPER (Waves of HF and Sounder for Probing Electron Density by Relaxation) onboard Cluster: the total electron density at standard time resolutions of either 2.15 or 52 s, and electric field spectra in the frequency range 2?82 KHz with time resolutions of 1.7 or 3.4 seconds. Data products available from the Cluster Active Archive include: electron number density, electric spectral power density (natural waves), electric spectral power density from active and passive emission during sounding, and electric waveform power density (energy). Ancillary data include density comparisons with PEACE and CIS measurements onboard Cluster; sounding times; housekeeping data; electron density in spin-resolution (4 seconds) and 1 minute averages; electron gyrofrequency in plasmasphere; instrument parameters during natural mode and active mode; active to passive spectral power density coded ratio; and caveats. Please note that WHISPER densities are used for calibrations of CLUSTER instruments, in particular particle instruments, which have difficulties to measure the colder part of the population, and EFW instrument, because spacecraft potential variations, currently used as a proxy of density variations, depend not only on the density but also on the energy of electrons. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.

49) 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:2016-09-14 07:58:21 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.

50) Cluster Samba Plasma Electrons and Currents Experiment (PEACE) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/PEACE/CSA/PT4S
Start:2001-01-01 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 08:00:04 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The Plasma Electrons and Currents Experiment (PEACE) data products consist of prime and summary parameters (moments). Collected from two instruments, a low-energy electron analyzer (LEEA) and a high-energy electron analyzer (HEEA), the 3-D and 2-D data products contain the measured quantity in a suitable array, i.e., count rate, particle flux, particle energy flux or phase space density. The energy coverage is from 0.67 eV to 30 KeV in 92 levels. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. 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. Three categories of PEACE data are available from the Cluster Active Archive (CAA): three-dimensional distribution data, pitch angle distribution data, and electron moments data. (I) A variety of 3-D data products are produced by PEACE, but only one standard reduced resolution (compressed by a factor of 8) 3-D data (3DR) is routinely produced with a standard size that is independent of sweep mode. Other 3-D data include the flexible reduced polar resoluttion (3DXP); full resolution 3-D distributions (3DX, occasionally 3DXLAR for the "summed energy" data); and partial azimuth content data (3DXPA, 3DXPALAR). (II) Pitch angle distribution data include the standard spin rate pitch angle data (PITCH_SPIN), full time resolution pitch angle data (PITCH_FULL), and pitch angle data from various 3-D data (PITCH_3DR, PITCH_3DX, PITCH_3DXLAR, PITCH_3DXA, 3DXA_LAR). (III) For the electron moments data, the CAA provides the Prime Parameters which have some inherent limiations and the MOMENTS data which offer the highest quality moments, though not always at spin rate. The MOMENTS are Summary Parameters from 3-D data that include electron density, velocity vector, pressure tensor and heat flux vector. The vectors and tensors are provided in GSE coordinates. Velocity and temperature are also provided as components perpendicular and parallel to the magnetic field (where the magnetic field data is taken from CSDS FGM PP data, at present). Moments production software is provided by the PEACE team via the CAA to allow scientists to calculate their own moments if they wish, for example using a subset of the measured energies and polar zones. The Prime Parameters (PP) are derived from the onboard moment sums, which are converted to electron moments data (density, velocity, perpendicular and parallel temperature, parallel heat flux). The PP data are provided in the GSE coordinate system. Geometric factor updates based on in-flight calibration are used to correct for errors due to the less up-to-date onboard calibrations. It is recommended that the CAA Moments data (Summary Parameters) and not the PP data are preferred for science analysis, despite the reduced time resolution in some cases, and that use of the PP data is only made after careful consideration of their limitations. In addition to these three categories of products, there are onboard selected pitch angle data (PAD), onboard moments Sums (OMS) in both normal and burst modes, and other diagnostic data. For more details, see Chapter 8 of "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.

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