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1) 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.

2) 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.

3) 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

4) CRRES electric field and convection drift data maxmize
Resource ID:spase://VMO/NumericalData/CRRES/LPI/PT30S
Start:1990-10-11 00:00:00 Observatory:CRRES Cadence:30 seconds
Stop:1991-10-13 00:00:00 Instrument:Langmuir Probe Instrument Resource:NumericalData
This data set includes the electric field and convection drift information from the CRRES spacecraft. The langmuir probe instrument data is at 30 s resolution. The files include the electric field vectors, elcetric field magnitude, and the convection drift vectors from both the spherical sensors and the cylindrical antennas.

5) 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.

6) 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.

7) 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.

8) 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.

9) 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.

10) Cluster Rumba Spatio-Temporal Analysis of Field Fluctuations (STAFF) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Rumba/STAFF/CSA/PT0.125S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:0.125 seconds
Stop:2016-09-14 07:59:49 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
Magnetic field and electric field data products from the Cluster Spatio-Temporal Analysis of Field Fluctuations (STAFF) available from the Cluster Active Archive include: Level 2 calibrated data -- STAFF Waveform Analyzer (STAFF-SC) Complex Spectra of the magnetic field in GSE coordinates (normal mode, up to 12.5 Hz and burst mode up to 225 Hz) with a time resolution of 10 second and a frequency resolution of 0.1 Hz; STAFF-SC Calibrated Magnetic Field WaveForm in ISR2 coordinates (normal mode, 25 Hz sampling and burst mode, 450 Hz sampling); STAFF Spectrum Analyzer (STAFF-SA) Spectral Matrix (8 Hz to 4 KHz) which is the cross-product of the magnetic and electric fileds values computed on-board the spacecraft with time resolutions of 4 seconds and 1 second; and Power Spectral Density (8 Hz to 4 KHz) with time resolutions of 1, 0.125 and 0.25 second. Level 3 value-added products include STAFF-SA Polarization and Propagation Parameters (8 Hz to 4 KHz). In the base mode in normal bit rate the auto-spectra are averaged over 1 s, and the complete 25-component matrix is averaged over 4 s for five components. In high bit rate, only the two highest frequency bands are analyzed. In the fast modes, time resolution is 1 s for the cross-spectra, and either 0.125 s or 0.25 s for the auto-spectra. The physical units for magnetic field spectral power are nT^2 Hz^-1, and electric field spectral power, V^2 m^-2 Hz^-1. Ancillary data included preliminary spectra, uncalibrated waveform, caveats, and calibration information. 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.

11) Cluster II Rumba Prime Parameter Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/STAFF/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2016-09-14 07:58:16 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
The Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) experiment provides magnetic field power spectral density values parallel and perpendicular to the magnetic field and the electric field power spectral density values for several frequency ranges. 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 STAFF (Spatio-Temporal Analysis of Field Fluctuations) Experiment for the Cluster Mission, by N. Cornilleau-Wehrlin et al., from which this information was obtained.

12) Cluster Rumba Wide Band Data (WBD) Plasma Waves at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Rumba/WBD/CSA/PT0.000035S
Start:2001-02-04 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:0.000035 seconds
Stop:2006-12-30 03:59:59 Instrument:Wide Band Data (WBD) Resource:NumericalData
The Cluster Wide Band Data (WBD) products at the Cluster Active Archive include full time resolution calibrated waveform data obtained in one of three frequency bandwidths: 9.5 kHz, 19 kHz, or 77 kHz in the range of 0-577 KHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. Calibrated electric field data are divided by 1000 to get V m^-1. Because of the high sampling rate of the WBD data (27.4 to 219.5 kilosamples per second), the time resolution of the WBD data (~36 to 5 microseconds in the time domain) is very high. This results in a very large data volume. Because of this the WBD data are stored in CEF files (and in CDF files from which the CEF files were generated) with maximum length of 10 minutes and size of a few hundred Mbytes. The user of WBD data is thus cautioned to take this into consideration when requesting WBD data downloads from the CAA. The 10 minute CDF files can also be downloaded from NASA's CDAWeb. 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.

13) Cluster 1 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Rumba/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM5 (Rumba) Cadence:0.0000046 seconds
Stop:2016-09-14 08:00:14 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | Bandwidth | Sample Rate | |-----------|--------------| | 9.5 kHz | 27.443 kHz | | 19 kHz | 54.886 kHz | | 77 kHz | 219.544 kHz | +--------------------------+ COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...

14) Cluster II Rumba Wide Band Data (WBD) Prime Parameters maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/WBD/PrimeParameter/PT0.02S
Start:2001-02-04 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:0.02 seconds
Stop:2016-09-14 07:58:16 Instrument:Wide Band Data (WBD) Resource:NumericalData
The WBD (Wide Band Data) investigation is designed to provide high-resolution frequency/time spectra of plasma waves in the Earth's magnetosphere. These data files contain information on the band width, resolution, antenna angles, offsets, magnetic and electric field information. 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 Wideband Plasma Wave Investigation,'' by D. A. Gurnett et al., from which this information was obtained.

15) 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.

16) Cluster 1 WHISPER Natural Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Rumba/WHISPER/PT2S
Start:2000-08-16 12:39:00 Observatory:Cluster FM5 (Rumba) Cadence:2.14 seconds
Stop:2016-09-14 08:00:14 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

17) Cluster 1 WHISPER Active Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Rumba/WHISPER/PT52S
Start:2000-08-16 12:39:00 Observatory:Cluster FM5 (Rumba) Cadence:52 seconds
Stop:2016-09-14 08:00:14 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

18) 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.

19) Cluster Salsa Active Spacecraft POtential Control (ASPOC) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Salsa/ASPOC/CSA/PT0.033S
Start:2001-01-01 00:00:00 Observatory:Cluster FM6 (Salsa) 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 0.33 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.

20) Cluster II Salsa Prime Parameter Active Spacecraft Potential Control (ASPOC) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/ASPOC/PrimeParameter/PT4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2016-09-14 07:58:21 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.

21) Cluster II Salsa Electron Drift Instrument (EDI) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Salsa/EDI/CSA/PT0.016S
Start:2001-01-30 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:0.016 seconds
Stop:2016-09-14 08:00:04 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.

22) Cluster II Salsa Prime Parameter Electron Drift Instrument (EDI) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/EDI/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2016-09-14 07:58:21 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.

23) Cluster II Salsa Prime Parameter Electric Field and Waves (EFW) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/EFW/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2016-09-14 07:58:21 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.

24) Cluster Salsa Wide Band Data (WBD) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Salsa/FGM/CSA/PT0.000005S
Start:2001-02-04 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:0.000005 seconds
Stop:2006-12-04 03:59:59 Instrument:Wide Band Data (WBD) Resource:NumericalData
The Cluster Wide Band Data (WBD) products at the Cluster Active Archive include full time resolution calibrated waveform data obtained in one of three frequency bandwidths: 9.5 kHz, 19 kHz, or 77 kHz in the range of 0-577 KHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. Calibrated electric field data are divided by 1000 to get V m^-1. Because of the high sampling rate of the WBD data (27.4 to 219.5 kilosamples per second), the time resolution of the WBD data (~36 to 5 microseconds in the time domain) is very high. This results in a very large data volume. Because of this the WBD data are stored in CEF files (and in CDF files from which the CEF files were generated) with maximum length of 10 minutes and size of a few hundred Mbytes. The user of WBD data is thus cautioned to take this into consideration when requesting WBD data downloads from the CAA. The 10 minute CDF files can also be downloaded from NASA's CDAWeb. 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.

25) Cluster Salsa Spatio-Temporal Analysis of Field Fluctuations (STAFF) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Salsa/STAFF/CSA/PT0.125S
Start:2001-01-01 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:0.125 seconds
Stop:2016-09-14 08:00:04 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
Magnetic field and electric field data products from the Cluster Spatio-Temporal Analysis of Field Fluctuations (STAFF) available from the Cluster Active Archive include: Level 2 calibrated data -- STAFF Waveform Analyzer (STAFF-SC) Complex Spectra of the magnetic field in GSE coordinates (normal mode, up to 12.5 Hz and burst mode up to 225 Hz) with a time resolution of 10 second and a frequency resolution of 0.1 Hz; STAFF-SC Calibrated Magnetic Field WaveForm in ISR2 coordinates (normal mode, 25 Hz sampling and burst mode, 450 Hz sampling); STAFF Spectrum Analyzer (STAFF-SA) Spectral Matrix (8 Hz to 4 KHz) which is the cross-product of the magnetic and electric fileds values computed on-board the spacecraft with time resolutions of 4 seconds and 1 second; and Power Spectral Density (8 Hz to 4 KHz) with time resolutions of 1, 0.125 and 0.25 second. Level 3 value-added products include STAFF-SA Polarization and Propagation Parameters (8 Hz to 4 KHz). In the base mode in normal bit rate the auto-spectra are averaged over 1 s, and the complete 25-component matrix is averaged over 4 s for five components. In high bit rate, only the two highest frequency bands are analyzed. In the fast modes, time resolution is 1 s for the cross-spectra, and either 0.125 s or 0.25 s for the auto-spectra. The physical units for magnetic field spectral power are nT^2 Hz^-1, and electric field spectral power, V^2 m^-2 Hz^-1. Ancillary data included preliminary spectra, uncalibrated waveform, caveats, and calibration information. 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.

26) Cluster II Salsa Prime Parameter Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/STAFF/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2016-09-14 07:58:21 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
The Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) experiment provides magnetic field power spectral density values parallel and perpendicular to the magnetic field and the electric field power spectral density values for several frequency ranges. 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 STAFF (Spatio-Temporal Analysis of Field Fluctuations) Experiment for the Cluster Mission, by N. Cornilleau-Wehrlin et al., from which this information was obtained.

27) Cluster 2 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Salsa/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM6 (Salsa) Cadence:0.0000046 seconds
Stop:2016-09-14 08:00:15 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | Bandwidth | Sample Rate | |-----------|--------------| | 9.5 kHz | 27.443 kHz | | 19 kHz | 54.886 kHz | | 77 kHz | 219.544 kHz | +--------------------------+ COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...

28) Cluster Salsa Wide Band Data (WBD) Prime Parameters maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Salsa/WBD/PrimeParameter/PT0.02S
Start:2001-02-04 13:45:07 Observatory:Cluster FM6 (Salsa) Cadence:0.02 seconds
Stop:2002-07-29 10:15:25 Instrument:Wide Band Data (WBD) Resource:NumericalData
The WBD (Wide Band Data) investigation is designed to provide high-resolution frequency/time spectra of plasma waves in the Earth's magnetosphere. These data files contain information on the band width, resolution, antenna angles, offsets, magnetic and electric field information. 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 Wideband Plasma Wave Investigation,'' by D. A. Gurnett et al., from which this information was obtained.

29) 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.

30) Cluster 2 WHISPER Natural Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Salsa/WHISPER/PT2S
Start:2000-08-16 12:39:00 Observatory:Cluster FM6 (Salsa) Cadence:2.14 seconds
Stop:2016-09-14 08:00:15 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

31) Cluster 2 WHISPER Active Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Salsa/WHISPER/PT52S
Start:2000-08-16 12:39:00 Observatory:Cluster FM6 (Salsa) Cadence:52 seconds
Stop:2016-09-14 08:00:15 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

32) 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.

33) Cluster Samba Active Spacecraft POtential Control (ASPOC) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/ASPOC/CSA/PT0.033S
Start:2000-12-09 00:00:00 Observatory:Cluster FM7 (Samba) 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.

34) Cluster II Samba Prime Parameter Active Spacecraft Potential Control (ASPOC) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/ASPOC/PrimeParameter/PT4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 07:58:22 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.

35) Cluster Samba Electron Drift Instrument (EDI) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/EDI/CSA/PT0.0625S
Start:2001-01-30 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:0.0625 seconds
Stop:2016-09-14 08:00:04 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.

36) Cluster II Samba Prime Parameter Electron Drift Instrument (EDI) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/EDI/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 07:58:22 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.

37) Cluster II Samba Prime Parameter Electric Field and Waves (EFW) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/EFW/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 07:58:22 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.

38) Cluster Samba Spatio-Temporal Analysis of Field Fluctuations (STAFF) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/STAFF/CSA/PT0.125S
Start:2001-01-01 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:0.125 seconds
Stop:2016-09-14 08:00:05 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
Magnetic field and electric field data products from the Cluster Spatio-Temporal Analysis of Field Fluctuations (STAFF) available from the Cluster Active Archive include: Level 2 calibrated data -- STAFF Waveform Analyzer (STAFF-SC) Complex Spectra of the magnetic field in GSE coordinates (normal mode, up to 12.5 Hz and burst mode up to 225 Hz) with a time resolution of 10 second and a frequency resolution of 0.1 Hz; STAFF-SC Calibrated Magnetic Field WaveForm in ISR2 coordinates (normal mode, 25 Hz sampling and burst mode, 450 Hz sampling); STAFF Spectrum Analyzer (STAFF-SA) Spectral Matrix (8 Hz to 4 KHz) which is the cross-product of the magnetic and electric fileds values computed on-board the spacecraft with time resolutions of 4 seconds and 1 second; and Power Spectral Density (8 Hz to 4 KHz) with time resolutions of 1, 0.125 and 0.25 second. Level 3 value-added products include STAFF-SA Polarization and Propagation Parameters (8 Hz to 4 KHz). In the base mode in normal bit rate the auto-spectra are averaged over 1 s, and the complete 25-component matrix is averaged over 4 s for five components. In high bit rate, only the two highest frequency bands are analyzed. In the fast modes, time resolution is 1 s for the cross-spectra, and either 0.125 s or 0.25 s for the auto-spectra. The physical units for magnetic field spectral power are nT^2 Hz^-1, and electric field spectral power, V^2 m^-2 Hz^-1. Ancillary data included preliminary spectra, uncalibrated waveform, caveats, and calibration information. 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.

39) Cluster II Samba Prime Parameter Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/STAFF/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 07:58:22 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
The Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) experiment provides magnetic field power spectral density values parallel and perpendicular to the magnetic field and the electric field power spectral density values for several frequency ranges. 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 STAFF (Spatio-Temporal Analysis of Field Fluctuations) Experiment for the Cluster Mission, by N. Cornilleau-Wehrlin et al., from which this information was obtained.

40) Cluster Samba Wide Band Data (WBD) Plasma Waves at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/WBD/CSA/PT0.000035S
Start:2001-02-04 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:0.000035 seconds
Stop:2006-12-30 03:59:59 Instrument:Wide Band Data (WBD) Resource:NumericalData
The Cluster Wide Band Data (WBD) products at the Cluster Active Archive include full time resolution calibrated waveform data obtained in one of three frequency bandwidths: 9.5 kHz, 19 kHz, or 77 kHz in the range of 0-577 KHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. Calibrated electric field data are divided by 1000 to get V m^-1. Because of the high sampling rate of the WBD data (27.4 to 219.5 kilosamples per second), the time resolution of the WBD data (~36 to 5 microseconds in the time domain) is very high. This results in a very large data volume. Because of this the WBD data are stored in CEF files (and in CDF files from which the CEF files were generated) with maximum length of 10 minutes and size of a few hundred Mbytes. The user of WBD data is thus cautioned to take this into consideration when requesting WBD data downloads from the CAA. The 10 minute CDF files can also be downloaded from NASA's CDAWeb. 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.

41) Cluster 3 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Samba/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM7 (Samba) Cadence:0.0000046 seconds
Stop:2016-09-14 08:00:15 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | Bandwidth | Sample Rate | |-----------|--------------| | 9.5 kHz | 27.443 kHz | | 19 kHz | 54.886 kHz | | 77 kHz | 219.544 kHz | +--------------------------+ COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...

42) Cluster Samba Wide Band Data (WBD) Prime Parameters maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/WBD/PrimeParameter/PT0.02S
Start:2001-02-03 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:0.02 seconds
Stop:2002-07-29 09:00:00 Instrument:Wide Band Data (WBD) Resource:NumericalData
The WBD (Wide Band Data) investigation is designed to provide high-resolution frequency/time spectra of plasma waves in the Earth's magnetosphere. These data files contain information on the band width, resolution, antenna angles, offsets, magnetic and electric field information. 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 Wideband Plasma Wave Investigation,'' by D. A. Gurnett et al., from which this information was obtained.

43) Cluster Samba 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-Samba/WHISPER/CSA/PT0.2S
Start:2001-02-02 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:0.2 seconds
Stop:2016-09-14 08:00:05 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.

44) Cluster 3 WHISPER Natural Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Samba/WHISPER/PT2S
Start:2000-08-16 12:39:00 Observatory:Cluster FM7 (Samba) Cadence:2.14 seconds
Stop:2016-09-14 08:00:15 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

45) Cluster 3 WHISPER Active Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Samba/WHISPER/PT52S
Start:2000-08-16 12:39:00 Observatory:Cluster FM7 (Samba) Cadence:52 seconds
Stop:2016-09-14 08:00:15 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

46) Cluster II Samba Prime Parameter Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/WHISPER/PrimeParameter/4S
Start:2000-12-10 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 07:58:22 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.

47) Cluster Tango Active Spacecraft POtential Control (ASPOC) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Tango/ASPOC/CSA/PT0.033S
Start:2000-12-09 00:00:00 Observatory:Cluster FM8 (Tango) 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.

48) Cluster II Tango Prime Parameter Active Spacecraft Potential Control (ASPOC) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Tango/ASPOC/PrimeParameter/PT4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:4 seconds
Stop:2016-09-14 07:58:19 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.

49) Cluster Tango Electron Drift Instrument (EDI) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Tango/EDI/CSA/PT0.0625S
Start:2001-01-30 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:0.0625 seconds
Stop:2016-09-14 07:59:52 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.

50) Cluster II Tango Prime Parameter Electron Drift Instrument (EDI) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Tango/EDI/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:4 seconds
Stop:2016-09-14 07:58:19 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.

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