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1) 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

2) 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

3) 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.

4) AE-E Extreme UltraViolet (EUV) Spectrometer Flux maxmize
Resource ID:spase://VSPO/NumericalData/AE-E/EUVS/PT256S
Start:1977-07-01 00:00:00 Observatory:AE-E Cadence:256 seconds
Stop:1981-06-09 23:59:59 Instrument:The Extreme Ultraviolet Spectrometer (EUVS) Resource:NumericalData
The EUV flux data came from the Extreme UltraViolet Spectrometer on the Atmosphere Explorer E. The data for 15 wavelength groups are normalized to the reference spectrum SC21REFW.DAT (located in directory REF_SPEC). GET_EUVS.FOR is a program to read the EUV data file (written by Dean Pesnell). The EUVS instrument is described in an article by Hinteregger in Radio Science, Volume 8, Number 4, 349-360, 1973. For more references please consult the file REF_LIST in the AEDOC directory. In addition to the solar EUV measurements, the EUVS also provided an opportunity to study the optical depth (absorption) of the thermosphere. Details of this analysis are described in: L.M. Chaikin and K. Fukui, Absorption Data Analysis for EUVS Experiment on the Satellites AE-C, D, and E, Air Force Geophysics Laboratory, Report AFGL-TR-79-0191, Hanscom AFB, Massachusetts, August 1979.

5) 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

6) AIM/CDE dust grain impact data maxmize
Resource ID:spase://VSPO/NumericalData/AIM/CDE/PT1D
Start:2007-06-01 00:00:00 Observatory:AIM Cadence:
Stop:2016-09-14 08:00:04 Instrument:AIM Cosmic Dust Experiment Resource:NumericalData
AIM/CDE (Cosmic Dust Experiment) data are available as Levels 1 and 2 daily netCDF files. L1 data contains, for each dust grain impact, a time tag, pulse height data, a number of electrons released by the impact, and engineering and housekeeping data. L2 data adds the mass of the impacting particle and spacecraft location at time of impact. Future L3 and L4 products will add total mass impacting per orbit and impact rates (L3) and mass correlation with CIPS total particle mass and Polar Mesospheric Cloud brightness.(

7) AIM/CIPS noctilucent cloud images and movies, etc. maxmize
Resource ID:spase://VSPO/NumericalData/AIM/CIPS/PT90M
Start:2007-06-01 00:00:00 Observatory:AIM Cadence:90 minutes
Stop:2016-09-14 08:00:04 Instrument:AIM Cloud Imaging and Particle Size experiment Resource:NumericalData
AIM/CIPS (Cloud Imaging and Particle Size) data are available in multiple processing levels: 1a (calibrated and geolocated albedo); 1b (map- projected albedo at 5km x 5km resolution); 1c (same as 1b, but with Rayleigh scattering background subtracted); 2 (imagery for 15 orbit- specific strips per day, built from 1c data); 3a (daily "daisies" built as composites over level 2 data); 3b (seasonal movies built from level 3a data); 4 (cloud properties such as ice water content and particle radius extracted from lower level data). Data files for levels 2, 3a and 4 are accessible from http://aim.hamptonu.edu/sds/cal_index_aim.php?instrument=cips, with level 2 and 4 data as gzipped netCDF's and level 3a imagery in PNG format. Brief descriptions of data levels, browse imagery, and links to fuller data documentation files at LASP are available from http://aim.hamptonu.edu/library/documentation/instruments/cips/cips_docs.html Data are available over each polar region about 4 months each year, during that region's summer.(

8) AIM/SOFIE daily plots, parameters vs.alt. & long., etc. (L3 Summary data) maxmize
Resource ID:spase://VSPO/DisplayData/AIM/SOFIE/PT90M
Start:2007-05-28 00:00:00 Observatory:AIM Cadence:90 minutes
Stop:2016-09-14 07:59:49 Instrument:AIM Solar Occultation For Ice Experiment Resource:NumericalData
This SOFIE (Solar Occultation for Ice Experiment) data set contains color-coded pairs of daily plots of several physical parameters vs altitude and longitude. Parameters include temperature, mixing ratios for H2O, O3 and CH4, and ice mass. Members of each pair are for the northern and southern hemispheres. The interface also supports plotting of lower level data.

9) AIM/SOFIE mixing ratios, extinction profiles, etc. (L2 data) maxmize
Resource ID:spase://VSPO/NumericalData/AIM/SOFIE/PT90M
Start:2007-05-28 00:00:00 Observatory:AIM Cadence:90 minutes
Stop:2016-09-14 08:00:04 Instrument:AIM Solar Occultation For Ice Experiment Resource:NumericalData
The daily netCDF files at GATS, Inc., hold level 2 SOFIE (Solar Occultation for Ice Experiment) data. These include primary absorber mixing ratios (CO2, CH4, NO,H2O, O3), 10 aerosol extinction profiles, uncertainity profiles for mixing ratios and extinctions, 83 km measurement lat./long., Temperatures, Pressures, Time, [0.150 km sampling, 150km to 3.0km, 30 profiles/day]. Vertical resolutions are 1km for gases and for polar mesospheric clouds, and .LT.3.5 km for temperatures and pressures.

10) Aeros-A Neutral Gas Densities maxmize
Resource ID:spase://VSPO/NumericalData/Aeros-A/NATE/PT256S
Start:1972-12-26 00:00:00 Observatory:Aeros-A Cadence:256 seconds
Stop:1973-08-09 23:59:59 Instrument:The Neutral Atmosphere Temperature Experiment (NATE) Resource:NumericalData
This data set contains the neutral densities measured by the Neutral Density and Temperature Probe (PI: N. Spencer) during the AEROS-A satellite mission. The data are in ASCII format and cover the time period from 12/26/1972 to 8/9/1973. The four different files provided in this data set contain the data for He, O2, N2, and Ar, respectively. Each data record provides date, time, density, density error, altitude, latitude and longitude, and local solar time.

11) 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

12) Akebono ATV auroral images maxmize
Resource ID:spase://VSPO/DisplayData/Akebono/ATV/PT3H
Start:1989-04-12 00:00:00 Observatory:Akebono Cadence:3 hours
Stop:1990-02-28 00:00:00 Instrument:Akebono Auroral TV Imagery(ATV) Resource:NumericalData
These Akebono ATV auroral images are available at somewhat irregular time intervals. There are also a few brief movies of various types of auroral forms.

13) 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.

14) 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

15) Akebono PWS NPW Data maxmize
Resource ID:spase://VWO/NumericalData/Akebono/PWS/E.NPW.PT2S
Start:1989-02-24 13:32:00 Observatory:Akebono Cadence:2 seconds
Stop:2016-09-14 08:00:15 Instrument:Plasma Wave Observation and Sounder Experiments (PWS) Resource:NumericalData
The Plasma Wave Observation and Sounder Experiment (PWS) observes both natural (NPW) and stimulated (SPW) plasma waves. The frequency range of the NPW system is 20 kHz to 5.12 MHz. These CDF data consist of Electric Field intensities measured by the PWS Recevier 1 (RX1) and Receiver 2 (RX2) units.

16) Akebono RDM electron flux annual plots maxmize
Resource ID:spase://VSPO/DisplayData/Akebono/RDM/P1Y
Start:1989-02-26 00:00:00 Observatory:Akebono Cadence:1 year
Stop:2002-12-23 00:00:00 Instrument:Radiation Dose Instrument (RDM) Resource:NumericalData
There are two families of electron flux plots. "Mapping plots" show annually averaged color-coded fluxes of 0.3-0.95, 0.95-2.5 and >2.5 MeV electrons, plotted in a radial distance vs. latitude projected into a common meridional plane. Lines of constant McIlwain-L parameter are superposed. "Flux plots" show color-coded fluxes of >2.5 MeV electrons vs. McIlwain-L and time,with each plot covering one full year.

17) Akebono RDM digital binary e, H+, He++ count rates maxmize
Resource ID:spase://VSPO/NumericalData/Akebono/RDM/PT8S
Start:1989-04-01 00:00:00 Observatory:Akebono Cadence:8 seconds
Stop:1997-12-23 00:00:00 Instrument:Radiation Dose Instrument (RDM) Resource:NumericalData
These count rate data from the High Energy Particle Monitor (HPM) of the Radiation Monitor (RDM) reside in the DARTS/Akebono binary Science DataBase (SDB). They consist of count rates at 8-sec spacecraft spin resolution for 0.3-0.95, 0.95-2.5 and >2.5 MeV electrons, 6.3-15, 15-29, 29-62 MeV protons, and 16-52 MeV alpha particles. Detailed information is found at http://darts.isas.jaxa.jp/akbn/readme/readme.rdm.txt.

18) Akebono SMS summary plots of ion count rates maxmize
Resource ID:spase://VSPO/DisplayData/Akebono/SMS/PT8S
Start:1989-04-01 00:00:00 Observatory:Akebono Cadence:8 seconds
Stop:1997-12-23 00:00:00 Instrument:Suprathermal Mass Spectrometer(SMS) Resource:NumericalData
These data consist of plots of color-coded ion count rates vs. spin phase angle and time, for thermal H+, He++, He+ and O+ ions and for suprathermal H+ and O+ ions. Each plot covers some or all of one ~3.5 hour orbit. Digital binary data and a data reading program are also accessible.

19) Akebono SMS digital binary ion count rates maxmize
Resource ID:spase://VSPO/NumericalData/Akebono/SMS/PT8S
Start:1989-02-26 00:00:00 Observatory:Akebono Cadence:8 seconds
Stop:2002-12-23 00:00:00 Instrument:Suprathermal Mass Spectrometer(SMS) Resource:NumericalData
These count rate data reside in the DARTS/Akebono binary Science DataBase (SDB). They consist of count rates at 8-sec spacecraft spin resolution, separately for thermal and suprathermal H+, He+ and O+ ions. Detailed information and a data-read program are found at http://darts.isas.jaxa.jp/akbn/readme/readme.sms.txt.

20) 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.

21) 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.

22) 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.

23) 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

24) 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).

25) Alouette-2 Topside Sounder Ionogram Data maxmize
Resource ID:spase://VWO/NumericalData/Alouette2/SFS/PT31S
Start:1965-11-29 13:42:37 Observatory:Alouette 2 Cadence:31 seconds
Stop:1968-01-01 04:11:45 Instrument:Alouette 2 Sweep-Frequency Sounder Resource:NumericalData
These ionograms were digitized from the original Alouette 2 7-track analog telemetry tapes using the facilities of the former Data Evaluation Laboratory at the NASA/GSFC. This data restoration project is headed by Dr. R.F. Benson (NASA/GSFC). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.75 km. The ionograms consist of swept-frequency operation (there is no fixed-frequency operation as in ISIS-1 and ISIS-2). The time resolution between ionograms is typically 31 seconds.

26) 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.

27) 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

28) ARCAD Magnetic Field Data maxmize
Resource ID:spase://VSPO/NumericalData/Aureol3/TRAC/PT2.50S
Start:1981-10-01 00:00:00 Observatory:Aureol 3 Cadence:2.50 seconds
Stop:1982-03-01 00:00:00 Instrument:TRAC (Fluxgate Magnetometer) Resource:NumericalData
ARCAD magnetic field data at 2.5-s resolution; altitude < 2000 km, near polar

29) BARREL Level 2 Ephemeris 4-s Data from 2013 and 2014 Launches maxmize
Resource ID:spase://VSPO/NumericalData/BARREL/EPH/L2/EPHM/PT4S
Start:2013-01-28 12:38:10 Observatory: Cadence:4 seconds
Stop:2014-02-11 17:11:55 Instrument: Resource:NumericalData
This data group contains ephemeris data (Lat, Long, Alt, and Time) from multiple balloons of the BARREL (Balloon Array for Radiation-belt Relativistic Electron Losses) investigation in 2013 and 2014. Data include geographic and magnetic coordinates. Geographic coordinates are obtained from onboard GPS unit; magnegic coordinates are derived using the IRBEM FORTRAN library for Kp=2 and Kp=6. Data products are each returned from the payload once every 4s.

30) BARREL Level 2 Fast Spectra 50-ms Data from 2013 and 2014 Launches maxmize
Resource ID:spase://VSPO/NumericalData/BARREL/XRI/L2/FSPC/PT0.05S
Start:2013-01-28 12:38:10 Observatory:BARREL Cadence:0.05 seconds
Stop:2014-02-11 17:11:55 Instrument:X-Ray Instrument Resource:NumericalData
This data group contains Bremsstrahlung X-ray measurements from the NaI spectrometers that are onboard multiple balloons of the BARREL (Balloon Array for Radiation-belt Relativistic Electron Losses) investigation in 2013 and 2014. Level 2 fast spectra data are available from four channels at 20 keV-15 MeV with a time resolution of 50 ms.

31) BARREL Level 2 Medium Spectra 4-sec Data from 2013 and 2014 Launches maxmize
Resource ID:spase://VSPO/NumericalData/BARREL/XRI/L2/MSPC/PT4S
Start:2013-01-28 12:38:10 Observatory:BARREL Cadence:4 seconds
Stop:2014-02-11 17:11:51 Instrument:X-Ray Instrument Resource:NumericalData
This data group contains Bremsstrahlung X-ray measurements from the NaI spectrometers that are onboard multiple balloons of the BARREL (Balloon Array for Radiation-belt Relativistic Electron Losses) investigation in 2013 and 2014. Level 2 medium spectra data are available from 48 channels at 100 keV- 4 MeV with a time resolution of 4 s.

32) BARREL Level 2 Rate Counters 4-s Data from 2013 and 2014 Launches maxmize
Resource ID:spase://VSPO/NumericalData/BARREL/XRI/L2/RCNT/PT4S
Start:2013-01-28 12:38:10 Observatory:BARREL Cadence:4 seconds
Stop:2014-02-12 07:21:00 Instrument:X-Ray Instrument Resource:NumericalData
This data group contains Level 2 x-ray rate counter diagnostics for the NaI spectrometers. Spectrometers (scintillators) are onboard multiple balloons of the BARREL (Balloon Array for Radiation-belt Relativistic Electron Losses) investigation in 2013 and 2014. Rate counter data records for dpu interrupt, low level, peak detect, and high level are available in 4-s accumulations.

33) BARREL Level 2 Slow Spectra 32-sec Data from 2013 and 2014 Launches maxmize
Resource ID:spase://VSPO/NumericalData/BARREL/XRI/L2/SSPC/PT32S
Start:2013-01-28 12:38:10 Observatory:BARREL Cadence:32 seconds
Stop:2014-02-11 17:11:31 Instrument:X-Ray Instrument Resource:NumericalData
This data group contains Bremsstrahlung X-ray measurements from the NaI spectrometers that are onboard multiple balloons of the BARREL (Balloon Array for Radiation-belt Relativistic Electron Losses) investigation in 2013 and 2014. Level 2 slow spectra data are available from 256 channels at 20 keV-10 MeV with a time resolution of 32 s.

34) 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

35) 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

36) 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.

37) 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.

38) 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.

39) CNOFS VEFI 1-sec Magnetic Field preliminary data maxmize
Resource ID:spase://VSPO/NumericalData/CNOFS/VEFI/BField/PT1S
Start:2008-05-09 00:00:00 Observatory:Communication/Navigation Outage Forecasting System (C/NOFS) Cadence:1 second
Stop:2009-04-30 23:59:59 Instrument:C/NOFS Vector Electric Field Instrument (VEFI) Resource:NumericalData
This data set contains magnetic field data from the fluxgate magnetometer associated with the C/NOFS Vector Electric Field Instrument (VEFI). The data include 1-sec resolution magnetic field components (North, West, Up) and spacecraft positions. As of 5/13/2010, the data were preliminary.

40) CNOFS VEFI 1-sec Electric Field preliminary data maxmize
Resource ID:spase://VSPO/NumericalData/CNOFS/VEFI/EField/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 Vector Electric Field Instrument (VEFI) Resource:NumericalData
This C/NOFS Vector Electric Field Instrument (VEFI) data set contains measurements of (magnetic) meridional and zonal components of electric fields and ExB drift velocities. Data are at 1-sec resolution.

41) CNOFS VEFI 500-msec Optical Lightning Data maxmize
Resource ID:spase://VSPO/NumericalData/CNOFS/VEFI/Lightning/PT0.5S
Start:2008-04-23 00:00:00 Observatory:Communication/Navigation Outage Forecasting System (C/NOFS) Cadence:0.5 seconds
Stop:2011-12-31 23:46:00 Instrument:C/NOFS Vector Electric Field Instrument (VEFI) Resource:NumericalData
This data set contains the low rate data from the C/NOFS Vector Electric Field Instrument (VEFI) lightning detector during nighttime passes of the satellite along its low inclination (13 degree) orbit and within the altitude domain defined by the satellite?s perigee and apogee of 401 km and 867 km, respectively. Two photodiodes measure white light irradiance at 2 Hz in 7 threshold values and in 2 look directions (north and south). Data are at 0.5-sec resolution. The lightning detector data may be used to identify a possible relationship between the occurrence of lightning and the occurrence of Spread-F caused, deep density dropouts in the ionosphere. Reference: Jacobson et al, J Atm Ocean Tech, 2011, doi:10.1175/JTECH-D-11-00047.1

42) CRRES Plasma Wave Experiment Survey Dynamic Spectrogram Plots maxmize
Resource ID:spase://VWO/DisplayData/CRRES/PWE/SFR.SA/Survey.DS.PT10H
Start:1990-08-01 17:35:00 Observatory: Cadence:8 seconds
Stop:1991-10-12 00:45:00 Instrument: Resource:DisplayData
This dataset contains one-orbit duration dynamic spectrogram GIF plots of the CRRES/Plasma Wave Experiment Sweep Frequency Receiver and Multichannel Spectrum Analyzer (electric antenna). CRRES was launched on July 25, 1990, into a geosynchronous transfer orbit with perigee altitude of 350 km and an apogee 6.3Re (Earth radii) geocentric. The inclination was 18.2 deg, the orbital period was 9 h and 52 min, and the initial magnetic local time at apogee was 0800 MLT. The plasma wave experiment measures the electromagnetic and/or electrostatic fields detected by three sensors: 1) a 100 m tip-to-tip extendable fine wire long electric dipole antenna (designated WADA for wire antenna deployment assembly), 2) a search coil magnetometer mounted at the end of a 6-m boom, and 3) a 94-m sphere-to-sphere double probe electric antenna (designated SWDA for spherical-double-probe wire deployment assembly) which is part of the EF/LP experiment. The first two sensors are the primary sensors for the plasma wave experiment whereas the third sensor is the primary sensor for EF/LP experiment. Following the antenna extensions, the spacecraft was spun down to approximately 2 rpm. The normal mode of operation for the plasma wave experiment after the antenna extensions has been to have the sweep frequency receiver locked onto the WADA antenna and the multichannel analyzer cycling through all three antennas. The basic CRRES plasma wave experiment instrumentation includes two receivers: 1) a multichannel spectrum analyzer to provide high-time-resolution spectra from 5.6 Hz to 10kHz, and 2) a sweep frequency receiver for high-frequency- resolution spectrum measurements from 100 Hz to 400 kHz. Each plot shows a plasma wave spectrogram for a one orbit (roughly 10 hour) period. The spectrograms cover the frequency range from 5.6 Hz to 400 kHz presented on a logarithmic scale. The data from 5.6-100 Hz are the measurements from the multichannel spectrum analyzer during the portions of its cycling when it is connected to the WADA antenna. Additional marks along the frequency axis indicate the boundaries between bands on the sweep frequency receiver. Band 1 extends from 100 to 800 Hz, Band 2 from 800 to 6.4 kHz, Band 3 from 6.4 to 50 kHz and Band 4 from 50 to 400 kHz. The intensity of the waves are color-coded and are in units of db(V/m/root(Hz)). The red line superimposed on each plot shows the electron cyclotron frequency calculated from the fluxgate magnetometer experiment. The time resolution above 6.4 kHz is one spectrum every 8s. The striations apparent in some emissions are a result of the beating between the spin rate and the sampling rate. Across the top of the figure is "CRRES SFR/SA" for the CRRES Plasma Wave Experiment Sweep Frequency Receiver and Multichannel Spectrum Analyzer, the units of the color scale is provided as well as the color bar with maximum and minimum values. Beneath the time axis is CRRES orbital information: Radial distance in Earth radii, Magnetic Latitude, Magnetic Local Time and L-shell. Along the left edge of the figure is the orbit number followed by the date. Along the right edge of the figure is "The University of Iowa/AFGL", the name of the software package used to create the plots and the date and time in which the plot was created.

43) Cluster Rumba Active Spacecraft POtential Control (ASPOC) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Rumba/ASPOC/CSA/PT0.033S
Start:2000-12-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:0.033 seconds
Stop:2008-07-01 00:00:00 Instrument:Active Spacecraft Potential Control (ASPOC) Resource:NumericalData
The primary objective of ASPOC (Active Spacecraft POtential Control) onboard Cluster is to insure the effective and complete measurement of the ambient plasma distribution functions down to low energy. Two main ASPOC data products are available from the Cluster Active Archive: ion bean current at 0.5 second resolution and ion current snapshot at 0.033 second resolution. Ancillary data include command history, status of the instrument at 5.15 second resolution, preliminary emitted current parameters (at 4-second resolution and 1-minute aveerges) and caveats. 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.

44) Cluster II Rumba Prime Parameter Active Spacecraft Potential Control (ASPOC) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/ASPOC/PrimeParameter/PT4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2016-09-14 07:58:16 Instrument:Active Spacecraft Potential Control (ASPOC) Resource:NumericalData
The ASPOC instrument is a single unit consisting of an electronics box and two cylindrical ion emitter modules. The emitters produce indium ions at approximately 6 KeV, in a current of less than 50 microamps. This is done by field evaporation of indium in the apex field of a needle. In the basic feedback mode of operation, a measurement of the spacecraft potential is supplied to the instrument from either the electric field experiment (EFW) or the electron analyzer (PEACE). This information is then used to adjust the emission current to reduce the spacecraft potential to some predetermined value. By default, priority is given to the EFW data, because of the higher resolution (0.034 V vs. ~1.4 V) and the more straightforward way in which the potential is derived. A calibration mode will measure the current voltage characteristics of the spacecraft, at the beginning of the mission and occasionally later to account for changes in the photoemission properties of the surface. This measurement is carried out by sweeping the ion emission current in incremental steps over some convenient range, allowing simultaneous measurements of the spacecraft potential. The length of each step is 2 to 4 spin periods. In addition to providing an improved environment for other experiments, ASPOC will permit scientific investigations of the photoelectric characteristics of the dependence of the spacecraft potential on plasma parameters, and of spacecraft charging in different plasma environments to be carried out in the so called active mode. 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 'Active Spacecraft Potential Control: an ion emitter experiment for Cluster,' by W. Riedler et al., from which this information was obtained.

45) Cluster Rumba Ion Spectrometry (CIS) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Rumba/CIS/CSA/PT4s
Start:2000-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2016-09-14 07:59:49 Instrument:Cluster Ion Spectrometry (CIS) Resource:NumericalData
The Cluster Ion Spectrometry (CIS) data products include three-dimensional ion distributions (about 0-40 keV/e) in 4-s spacecraft spin resolution and mass-per-charge composition distribution that are measured by the Hot Ion Analyzer (HIA) and Composition Distribution Function (CODIF) analyzer on board the Cluster II Rumba spacecraft. Data products consist of processed raw data (Level 1 data), moments of the distribution functions (Level 2 data), and calibrated high-resolution data in a variety of physical units (Level 3 data). Furthermore, the calibration files and high-level processing software are also available. CIS Level 1 data are decommutated, decompressed and time-tagged telemetry data in raw instrument units. CIS Level 2 data are moments of the particle functions: ion density, velocity in the GSE reference frame, and temperature in parallel and perpendicular components (obtained by diagnolizing the pressure tensor). For CODIF, which has a higher upper energy limit than HIA, the pressure is also supplied in addition. They correspond to the Prime Parameters from the Cluster Science Data System: onboard calculated moments, then reprocessed on ground (total efficiency calibration adjustments, coordinate transformations etc.). Onboard calculated moments provide 1-spin time resolution, and are calculated from the full angular and energy resolution 3-D ion distributions. In addition to the onboard calculated moments, CIS Level 2 data include also CODIF moments calculated on the ground from the 3-D ion distributions. These provide better calibration adjustments (per anode efficiency) and are thus more accurate, but have a reduced time and energy resolution. HIA on the ground calculated moments are not supplied, because the same anode calibrations would be used as for the onboard calculated ones, but with a degraded time, energy and angular resolution (no added value). A software package is available for download at the CAA web site, allowing the user to interactively calculate partial (or total) moments of the ion distributions, for selected energy and solid angle ranges: CODIF (all 4 ion species) and HIA data. CIS Level 3 data are processed high-resolution 3-D ion distributions. They are produced by correcting the Level 1 data for detector efficiencies, geometric factors and other information available from the calibration tables, and give measurements in 5 physical units in separate files: (Differential) particle flux as ions cm**?2s**?1sr**?1keV**?1, (Differential) particle energy flux in keVcm**?2s**?1sr**?1keV**?1, particle phase space density in ions s**3 km**? 6, corrected-for-efficiency particle count rate as ions s**? 1, and raw particle counts in number of ions per counter bin. These Level 3 archival files are constructed by joining files from similar telemetry data products (same ion species, different angular, energy or time resolution). They are organized as a function of the instrument (HIA or CODIF), the operational mode (magnetospheric, solar wind, or RPA), the instrument sensitivity side (High Sensity or Low Sensity), and the 4 ion species of H+, He+, He++, and O+ with energies from ~25eV/e to 40 keV/e and with medium angular resolution of 22.5 deg (for CODIF only). Two data processing software packages are available from CAA: the CIS_3D_MOM written in C to read the CIS Level 3 files, and another software written in IDL to read Level 1 data and calibrations files. The second software can read, in addition to CIS data, generic CDF and CEF data files for correlation studies. The CIS data archive at CAA also includes experiment documentation, graphical products for browsing through the data, and data caveats. 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.

46) Cluster II Rumba Prime Parameter Cluster Ion Spectrometry (CIS) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/CIS/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2016-09-14 07:58:16 Instrument:Cluster Ion Spectrometry (CIS) Resource:NumericalData
This instrument (CIS: Cluster Ion Spectrometry) is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

47) Cluster Rumba Digital Wave Processor (DWP) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Rumba/DWP/CSA/PT4S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2016-09-14 07:59:49 Instrument:Digital Wave Processor (DWP) Resource:NumericalData
As the central control and data processing unit for the Wave Experiement Consortium (WEC), the Digital Wave Processor (DWP) provided the following products in the Cluster Active Archive: (1) Time correction data (C1_CP_DWP_TCOR) with timing accuracy improved to 20 micro seconds; (2) Summary of the status of the Wave Experiment Consortium (C1_CP_DWP_ LOG) with one record for each interval that the WEC operates in the same mode for a total of 64 parameters including: instrument modes, telemetry use statistics, errors and anomalies, summary of voltage and temperature housekeeping; (3) A listing of the command sequences uplinked to the Wave Experiment Consortium (CM_CD_DWP_UT_PIOR); (4) High resolution particle correlator data for the fixed (pre-selected) energy band (C1_CP_DWP_COR_FX) and high resolution particle correlator data for the stepped energy (C1_CP_ DWP_COR_ST) which steps through the remaining 14 bands, at one step per spin; and (5) Documentation and software. Electron energy range is from 0.6 eV to 26 keV in 15 energy bands (PEACE mode dependent) and frequency range, 1.4 kHz to 41.6 kHz in 32 frequency bands and DC to 4 Hz based on successive autocorrelation function (ACF) outputs. 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.

48) Cluster Rumba Electron Drift Instrument (EDI) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Rumba/EDI/CSA/PT0.0625S
Start:2001-01-30 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:0.0625 seconds
Stop:2016-09-14 07:59:49 Instrument:Electron Drift Instrument (EDI) Resource:NumericalData
The Electron Drift Instrument (EDI) data products from the Cluster spacecraft in three main categories: (1) Electron enegergies measured between 0.5 and 1.0 keV for the Windshield Wiper mode: time series of the three components of the electron drift velocity and of the three components of the electric field in Cartesian GSE coordinate system (corrected for spacecraft motion) with different qualities and time resolution at 1-4 sec (PP, PPP, MPD); (2) Ambient electron measurements at fixed enegeris of 0.5 or 1.0 keV: time series of electron counts normally at 16 ms for the three pitch angles 0 deg, 90 deg, 180 deg, the detector look direction in the spacecraft frame and in GSE and the status for AE mode; and (3) Overview plot of the main parameters for both modes for every 3 h for one reference spacecraft (usually Cluster III). Besides the main products, there also are raw data and auxiliary data. Raw data consist of merged science files (MSF) that are obtained by merging the housekeeping and science (burst (BM) and normal (NM) mode) telemetry files. They are in binary format. Auxiliary are either data used internally by the main data production software or data dedicated to intercalibration or time-interval lists of the EDI operation modes. 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 Rumba Prime Parameter Electron Drift Instrument (EDI) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/EDI/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2016-09-14 07:58:16 Instrument:Electron Drift Instrument (EDI) Resource:NumericalData
This instrument (EDI: Electron Drift Instrument) measures the drift of a weak beam of test electrons that, when emitted in certain directions, return to the spacecraft after one gyration. This drift is related to the electric field and the gradient in the magnetic field, and these quantities can, by the use of different electron energies, be determined separately. The fundamental time step to determine the new parameters and direct the beams and the detectors is 2 ms. Inter-experiment links include: magnetic field information from FGM and STAFF, a blanking pulse received from WHISPER to warn of possible interference from that active experiment, and a similar blanking pulse sent to PEACE when the EDI electron beam could interfere with the PEACE electron measurement. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Electron Drift Instrument for Cluster, by G. Paschmann et al., from which this information was obtained.

50) Cluster II Rumba Prime Parameter Electric Field and Waves (EFW) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/EFW/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2016-09-14 07:58:16 Instrument:Electric Field and Waves (EFW) Resource:NumericalData
The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440-29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1-700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1-100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1-100/cm. There is also a frequency counter covering the range 10-200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 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 The Spherical Probe Electric Field and Waves experiment for the Cluster Mission, by G. Gustafsson et al., from which this information was obtained.

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