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1) 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.

2) 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.

3) Cluster Samba Ion Spectrometry (CIS) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/CIS/CSA/PT4s
Start:2000-01-01 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 08:00:05 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 Samba 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.

4) Cluster II Samba Prime Parameter Cluster Ion Spectrometry (CIS) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/CIS/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 07:58:22 Instrument:Cluster Ion Spectrometry (CIS) Resource:NumericalData
This instrument (CIS: Cluster Ion Spectrometry) is capable of obtaining full 3D ion distributions with high time resolution (in one spacecraft spin) and mass-per-charge resolution. The experiment consists of two different instruments, a Hot Ion Analyzer (HIA) and a time-of-flight Ion Composition and Distribution Function analyzer (CODIF). Extensive on-board processing is done, within its dual-processor Data Processing System (DPS). CODIF determines the distributions of the major ion species with energies from spacecraft potential to 40 KeV/charge with an angular resolution of 22.5 x 10.25 degrees and with two different sensitivities. The CODIF instrument uses electrostatic deflection to select by energy per charge, with subsequent time-of-flight analysis. The sensor primarily covers the energy range 0.02-40 KeV/charge, but with additional pre-acceleration for energies below 25 eV/charge, the range is extended to energies as low as the spacecraft potential. The HIA does not measure mass, but extends the dynamic range to the highest ion fluxes, and has angular resolution capability of 5.6 x 5.6 degrees for ion-beam and solar-wind measurements. The HIA is a symmetric quadrispherical analyzer of top-hat geometry, and uses microchannel-plate electron multipliers and position encoding by discrete anodes. A 2D distribution is obtained once per 62.5 ms, and a full 3D distribution of ions in the energy range ~5 eV/charge to 32 KeV/charge is obtained every 4 s. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Cluster Ion Spectrometry Experiment, by H. Reme et al., from which this information was obtained.

5) Cluster Samba Digital Wave Processor (DWP) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/DWP/CSA/PT4S
Start:2001-01-01 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 08:00:04 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.

6) Cluster Samba Digital Wave Processor (DWP) prime parameter data at about 4 sec resolution (spin averaged) in GSE Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/DWP/PrimeParameter/PT4S
Start:2000-11-01 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2009-12-30 23:59:59 Instrument:Digital Wave Processor (DWP) Resource:NumericalData
Cluster Samba Digital Wave Processor (DWP) data set contains various instrument status and data status flags as well as particle correlator information.

7) 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.

8) 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.

9) 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.

10) Cluster Samba JSOC Predicted Magnetic Positions maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/Ephemeris/JP-PMP/PT60S
Start:2000-08-14 20:35:00 Observatory:Cluster FM7 (Samba) Cadence:60 seconds
Stop:2016-06-14 08:00:05 Instrument:Cluster-Samba Positions Resource:NumericalData
This dataset contains Cluster Samba JSOC predicted magnetic positions and magnetic field magnitude.

11) Cluster Samba JSOC Predicted Scientific Events maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/Ephemeris/JP-PSE/PT60S
Start:2000-08-01 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:60 seconds
Stop:2016-06-14 08:00:05 Instrument:Cluster-Samba Positions Resource:NumericalData
This dataset contains Cluster Samba JSOC predicted scientific events, orit number, and GSE positions.

12) Cluster Samba 1-min Position Data maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/Ephemeris/PT1M
Start:2000-08-23 00:00:29 Observatory:Cluster FM7 (Samba) Cadence:1 minute
Stop:2017-01-02 04:59:30 Instrument:Cluster-Samba Positions Resource:NumericalData
Cluster-3 (FM7/Samba) satellite position and magnetic field model information.

13) Cluster Samba Fluxgate Magnetometer (FGM) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/FGM/CSA/PT0.045S
Start:2001-01-30 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:0.045 seconds
Stop:2016-09-14 08:00:05 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
The Fluxgate Magnetometer (FGM) data products from the Cluster II Samba spacecraft consist of magnetic field measurements of the Earth's magnetosphere from a few tens of nT in the outer magnetosphere to over 1,000nT at closest approach. Products are provided at three different time resolutions: full resolution, 5 vectors/second resolution and spin resolution. Each calibration file is valid for the period of one orbit defined from perigee to perigee. The full-resolution magnetic field data has no time averaging applied. If the instrument is in normal mode, the data is at approximately 22 Hz resolution. If it is in burst mode, the data is at approximately 67 Hz resolution. The second product is averaged to a time resolution of 5 vectors per second. The third product is averaged over one spacecraft spin where the spin phase for averaging is the same as that used for the Prime Parameter data. Each of the three primary data products contain the following: time, magnetic field vector, magnetic field magnitude, spacecraft position, instrument range, and telementary mode. The magnetic field components and the spacecraft position are in the GSE coordinate system. In addition to the three primary products, there are five support data products: caveats, calibration field accuracy, calibration files, data missing from processed data set, and data removed by validation process. Caveat files are produced when the calibration is known to be changing on short timescales near eclipses and for other events when visible effects have been observed in the data. Calibration accuracy files contain detailed information on the accuracy of the magnetic field data products and can be used to select periods of data. Calibration files contain the nine elements of the 3x3 calibration matrix and the three offsets for each instrument range. Each file is valid for the period of one orbit for which magnetic field data products have been submitted to the Cluster Active Archive. Data gaps are listed for times at the processing stage when no data were taken, or at the data validation stage where invalid data have been removed. 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.

14) Cluster Samba Spin Resolution Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/FGM/SpinResolution/4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 07:58:22 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains spin resolution measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster Samba spacecraft.

15) Cluster II Samba Unvalidated Prime Parameter Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/FGM/UnvalidatedParameter/4S
Start:2006-01-01 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 07:58:22 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains spin resolution unvalidated prime parameter measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster 2 Samba spacecraft. Unvalidated FGM data might sometimes contain artefacts such as spikes (duration ~ 1 spin), or short rotations (few spins). Very occasionally the data contain many spikes over several hours. Please contact Elizabeth Lucek (e.lucek@imperial.ac.uk) for more information regarding possible artefacts in specific intervals of data. The unvalidated prime parameter Data Set does not contain the spacecraft position data or additional range and telemetry mode information that the CAA parameter data set does contain.

16) Cluster Samba Plasma Electrons and Currents Experiment (PEACE) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/PEACE/CSA/PT4S
Start:2001-01-01 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 08:00:04 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The Plasma Electrons and Currents Experiment (PEACE) data products consist of prime and summary parameters (moments). Collected from two instruments, a low-energy electron analyzer (LEEA) and a high-energy electron analyzer (HEEA), the 3-D and 2-D data products contain the measured quantity in a suitable array, i.e., count rate, particle flux, particle energy flux or phase space density. The energy coverage is from 0.67 eV to 30 KeV in 92 levels. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. Each sensor covers the range 0--180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. Three categories of PEACE data are available from the Cluster Active Archive (CAA): three-dimensional distribution data, pitch angle distribution data, and electron moments data. (I) A variety of 3-D data products are produced by PEACE, but only one standard reduced resolution (compressed by a factor of 8) 3-D data (3DR) is routinely produced with a standard size that is independent of sweep mode. Other 3-D data include the flexible reduced polar resoluttion (3DXP); full resolution 3-D distributions (3DX, occasionally 3DXLAR for the "summed energy" data); and partial azimuth content data (3DXPA, 3DXPALAR). (II) Pitch angle distribution data include the standard spin rate pitch angle data (PITCH_SPIN), full time resolution pitch angle data (PITCH_FULL), and pitch angle data from various 3-D data (PITCH_3DR, PITCH_3DX, PITCH_3DXLAR, PITCH_3DXA, 3DXA_LAR). (III) For the electron moments data, the CAA provides the Prime Parameters which have some inherent limiations and the MOMENTS data which offer the highest quality moments, though not always at spin rate. The MOMENTS are Summary Parameters from 3-D data that include electron density, velocity vector, pressure tensor and heat flux vector. The vectors and tensors are provided in GSE coordinates. Velocity and temperature are also provided as components perpendicular and parallel to the magnetic field (where the magnetic field data is taken from CSDS FGM PP data, at present). Moments production software is provided by the PEACE team via the CAA to allow scientists to calculate their own moments if they wish, for example using a subset of the measured energies and polar zones. The Prime Parameters (PP) are derived from the onboard moment sums, which are converted to electron moments data (density, velocity, perpendicular and parallel temperature, parallel heat flux). The PP data are provided in the GSE coordinate system. Geometric factor updates based on in-flight calibration are used to correct for errors due to the less up-to-date onboard calibrations. It is recommended that the CAA Moments data (Summary Parameters) and not the PP data are preferred for science analysis, despite the reduced time resolution in some cases, and that use of the PP data is only made after careful consideration of their limitations. In addition to these three categories of products, there are onboard selected pitch angle data (PAD), onboard moments Sums (OMS) in both normal and burst modes, and other diagnostic data. For more details, see Chapter 8 of "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet, from which this information was obtained.

17) Cluster II Samba Prime Parameter Plasma Electron and Current Experiment (PEACE) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/PEACE/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 07:58:22 Instrument:Plasma Electron and Current Experiment (PEACE) Resource:NumericalData
The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7-10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0-180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article PEACE: a Plasma Electron and Current Experiment, by A. D. Johnstone et al., from which this information was obtained.

18) Cluster II Samba Prime Parameter Research with Adaptive Particle Imaging Detectors (RAPID) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/RAPID/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2016-09-14 07:58:22 Instrument:Research with Adaptive Particle Imaging Detectors (RAPID) Resource:NumericalData
The dual-sensor spectrometer RAPID (Research with Adaptive Particle Imaging Detectors) analyzes suprathermal plasma distributions in the energy range from 20-400 KeV for electrons and from 2 KeV/nucleon to 1.50 MeV/nucleon for ions. 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 RAPID: The Imaging Energetic Particle Spectrometer on Cluster, by B. Wilken et al., from which this information was obtained.

19) 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.

20) 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.

21) 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.

22) Cluster Samba WBD High Time Resolution Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Cluster-Samba/WBD/DS.GIF.PT30S
Start:2001-02-03 05:26:00 Observatory:Cluster FM7 (Samba) Cadence:
Stop:2016-09-14 08:00:14 Instrument:Wide Band Data (WBD) Resource:DisplayData
This dataset contains 30 s duration survey spectrogram plots from the WBD instrument on the Cluster spacecraft. The spectrograms are created by 1024 point FFTs and plotted with frequency on the vertical axis, increasing time on the horizontal, and color indicating power spectral density, in relative dB. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW 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 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 are sampled at 4.6 microseconds in the time domain, 4.7 milliseconds in the frequency domain (generally the 77 kHz bandwidth mode). The lowest time resolution data are sampled at 36.5 microseconds in the time domain, 37.3 milliseconds in the frequency domain (generally the 9.5 kHz bandwidth mode). Above the spectrogram plot are a line plot panel, followed by four status lines. The line plot panel at the top provides the gain state (0 to 75 dB, in 5 dB steps) of the instrument. The four status lines provide the following information according to the color code in the upper right corner: Data mode - whether from DSN mode (real time telemetry), or from BM2 mode (recorded onboard in Burst Mode 2) as digitally filtered or duty cycled. Antenna - the electric field (Ey or Ez) or the magnetic field (Bx or By) antenna used. Resolution - the data digitization level, which can be 1 bit, 4 bit or 8 bit. Translation - the translation from base frequency of 0 kHz. In the lower right-hand corner are the ephemeris values applicable to the start time of the plot. At the middle right-hand side are given the date and start time of the plot as well as the spacecraft number. The University of Iowa repository maintains two types of high time resolution spectrogram plots in GIF format: a ten minute (PT10M Display Cadence) and a 30 second time span (PT30S Display Cadence). Both types of files provide information on WBD gain and operational mode, the spectral data from one spacecraft, the start date and time and ephemeris data. Overview spectrograms are also available. The availability of these files depends on times of DSN and Pansak 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 (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues can be found at http://www-pw.physics.uiowa.edu/cluster/interpretation_issues/interpretation.html 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.

23) 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 ...

24) 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.

25) 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.

26) 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.

27) 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.

28) 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.

29) Cluster Samba Electric Field and Waves (EFW) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster2-Samba/EFW/CSA/PT0.0001S
Start:2001-01-01 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:0.0001 seconds
Stop:2016-09-14 08:00:04 Instrument:Electric Field and Waves (EFW) Resource:NumericalData
The Cluster Electric Field and Waves (EFW) data available from the Cluster Active Archive include: (1) The instantaneous spin-plane components of the electric field vectors with time resolution down to 0.1 millisecond, 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; and (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. Level 1 is the raw data for reference puprose only and is not accessible on CAA. Both Level 2 (at 0.2 second and full resolution of 0.04 second) and Level 3 (4-second resolution) data include spacecraft potential; 3D Electric Field in Inverted Spin Reference 2 system (ISR2); 3D Electric Field in GSE; plasma (ExB) drift velocity in ISR2; and plasma (ExB) drift velocity in GSE. In addition, Level 2 products include data in burst mode of time resolutions up to 36,000 samples/s: spacecraft potential, 2D electric field data in ISR2 and 3D magnetic field data in ISR2. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. 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.

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