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1) ACE EPAM PHA Daily-Averaged Spectra maxmize
Resource ID:spase://VEPO/NumericalData/ACE/EPAM/PHA/G122
Start:1997-08-30 00:00:00 Observatory:ACE Cadence:1 day
Stop:2016-05-19 13:22:07 Instrument:ACE Electron Proton Alpha Monitor Resource:NumericalData
Daily-averaged species-separated energy spectra derived from the Pulse Height Analyzer. Data consist of counts and fluxes of each of six species (He, C, O, Ne, Si, Fe) in each of 12 energy bins.

2) ACE Ultra Low Energy Isotope Spectrometer 1-Hour Level 2 Data maxmize
Resource ID:spase://VEPO/NumericalData/ACE/ULEIS/L2_PT1H
Start:1998-02-20 00:00:00 Observatory:ACE Cadence:1 hour
Stop:2016-05-19 13:22:09 Instrument:ACE Electron Proton Alpha Monitor Resource:NumericalData
The Ultra Low Energy Isotope Spectrometer measures ion fluxes over the charge range from H through Ni from about 20 keV/nucleon to 10 MeV/nucleon, thus covering both suprathermal and energetic particle energy ranges. Exploratory measurements of ultra-heavy species (mass range above Ni) will also be performed in a more limited energy range near 0.5 MeV/nucleon. ULEIS will be studying the elemental and isotopic composition of solar energetic particles, and the mechanisms by which these particles are energized in the solar corona. ULEIS will also investigate mechanisms by which supersonic interplanetary shock waves energize ions. To avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.

3) AMPTE/IRM Magnetic Field maxmize
Resource ID:spase://VMO/NumericalData/AMPTE_IRM/MAG/PT4.4S
Start:1984-08-21 00:48:41 Observatory:AMPTE/IRM Cadence:4.4 seconds
Stop:1986-08-11 21:45:07 Instrument:AMPTE/IRM Magnetometer Resource:NumericalData
AMPTE/IRM spin-averaged magnetic field at ~4.4 second resolution.

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

5) AMPTE/UKS Magnetic Field Data maxmize
Resource ID:spase://VMO/NumericalData/AMPTE_UKS/FGM/PT5S
Start:1984-08-21 08:24:42 Observatory:AMPTE/UKS Cadence:5 seconds
Stop:1985-01-15 08:01:02 Instrument:AMPTE/UKS Magnetometer Resource:NumericalData
AMPTE/UKS 5-second (spin) averaged magnetic field measurements

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

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

8) Cluster Rumba WBD High Time Resolution Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Cluster-Rumba/WBD/DS.GIF.PT30S
Start:2001-02-03 05:26:00 Observatory:Cluster FM5 (Rumba) Cadence:
Stop:2016-05-19 13:23:47 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.

9) 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:2016-05-19 13:22:48 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.

10) Cluster II Salsa Prime Parameter Cluster Ion Spectrometry (CIS) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/CIS/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2009-01-31 23:59:59 Instrument:Cluster Ion Spectrometry (CIS) Resource:NumericalData
This instrument never worked and there is no data. This instrument (CIS: Cluster Ion Spectrometry) on the other spacecraft 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.

11) 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:2016-05-19 13:22:48 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.

12) 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:2016-05-19 13:22:48 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.

13) Cluster Salsa Spin Resolution Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/FGM/SpinResolution/4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2016-05-19 13:22:48 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 Salsa spacecraft.

14) Cluster II Salsa Unvalidated Prime Parameter Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/FGM/UnvalidatedParameter/4S
Start:2006-01-01 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2016-05-19 13:22:48 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 Salsa 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.

15) Cluster II Salsa Prime Parameter Plasma Electron and Current Experiment (PEACE) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/PEACE/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2016-05-19 13:22:48 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.

16) Cluster II Salsa Prime Parameter Research with Adaptive Particle Imaging Detectors (RAPID) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/RAPID/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2016-05-19 13:22:48 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.

17) 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:2016-05-19 13:22:48 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.

18) Cluster Salsa WBD High Time Resolution Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Cluster-Salsa/WBD/DS.GIF.PT30S
Start:2001-02-03 05:26:00 Observatory:Cluster FM6 (Salsa) Cadence:
Stop:2016-05-19 13:23:46 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.

19) 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:2016-05-19 13:22:48 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.

20) 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:2016-05-19 13:23:47 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.

21) Cluster Tango WBD High Time Resolution Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Cluster-Tango/WBD/DS.GIF.PT30S
Start:2001-02-03 05:26:00 Observatory:Cluster FM8 (Tango) Cadence:
Stop:2016-05-19 13:23:47 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.

22) Cluster II Summary Parameter Active Spacecraft Potential Control (ASPOC) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/ASPOC/SummaryParameter/PT1M
Start:2001-01-30 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:1 minute
Stop:2016-05-19 13:22:48 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.

23) Cluster II Summary Parameter Cluster Ion Spectrometry (CIS) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/CIS/SummaryParameter/60S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2016-05-19 13:22:48 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.

24) Cluster II Summary Parameter Electron Drift Instrument (EDI) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/EDI/SummaryParameter/60S
Start:2001-02-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2016-05-19 13:22:47 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.

25) Cluster II Summary Parameter Electric Field and Waves (EFW) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/EFW/SummaryParameter/60S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2016-05-19 13:22:47 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.

26) Cluster Auxiliary Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/Ephemeris/SummaryParameter/PT1M
Start:2000-08-22 00:00:30 Observatory:Cluster FM5 (Rumba) Cadence:1 minute
Stop:2016-05-19 13:22:47 Instrument:Cluster-Rumba Positions Resource:NumericalData
Cluster Auxiliary Parameters are produced by the Cluster Hungarian Data Center in Budapest. These data are the primary orbit product supplied to users by the Cluster Active Archive. The data contain Position, Velocity and Attitude of four Cluster spacecraft. For additional details on the methodology behind these data see: Robert P., et al., "Tetrahedron Geometric Factors", p. 328, Analysis Methods of Multi-Spacecraft Data, ed. G. Paschmann and P. Daly, 1998, ESA and the International Space Institute, Bern.

27) Cluster II Summary Parameter Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/FGM/SummaryParameter/60S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2016-05-19 13:22:47 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains 1 minute resolution validated summary prime parameter measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster 2 spacecraft. The summary 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.

28) Cluster II Unvalidated Summary Parameter Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/FGM/UnvalidatedSummaryParameter/60S
Start:2006-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2016-05-19 13:22:47 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains 1 minute resolution unvalidated summary prime parameter measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster 2 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 summary 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.

29) Cluster II Summary Parameter Plasma Electron and Current Experiment (PEACE) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/PEACE/SummaryParameter/60S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2016-05-19 13:22:48 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.

30) Cluster II Summary Parameter Research with Adaptive Particle Imaging Detectors (RAPID) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/RAPID/SummaryParameter/60S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2016-05-19 13:22:47 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.

31) Cluster II Summary Parameter Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/STAFF/SummaryParameter/60S
Start:2001-01-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2016-05-19 13:22:48 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.

32) Cluster WBD Survey Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Cluster/WBD/Survey.PNG.PT2H
Start:2001-02-03 05:26:00 Observatory:Cluster FM5 (Rumba) Cadence:
Stop:2016-05-19 13:23:46 Instrument:Wide Band Data (WBD) Resource:DisplayData
This dataset contains survey spectrogram plots of varying time durations from the WBD Plasma Wave Receivers on the four Cluster spacecraft. Due to the nature of the WBD real-time operations at the DSN, data from all four spacecraft are not always available. The time span of these plots varies based on the time span of the telemetry received in real-time from the DSN and Panska Ves ground stations and can range from 30 minutes to 8 hours, 2 hours being typical. Panels are included in the overview plots for all of the spacecraft for which WBD data are available at any given time. The spectrograms are created by 1024 point FFTs and plotted with frequency in kHz on the vertical axis, increasing time on the horizontal, and color indicating the power spectral density. 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. When the data shown in the overview plot are from an electric field antenna, the power spectral density is given in units of V^2/m^2/Hz. When the data shown in the overview plot are the WBD magnetic field measurements, the power spectral density is given in relative dB. The WBD antenna used is marked on the left-hand side of each plot panel, and the spacecraft name and number are provided on the right-hand side of each panel. Below the time labels on the horizontal axis, are the ephemeris values applicable to the times marked on the horizontal axis. The ephemeris values are provided for the spacecraft whose data are shown in the bottom panel of the plot, just above the time axis labels. These ephemeris values are provided only as an indication of the general location of the Cluster quartet within the magnetosphere. Due to varying spacecraft separations, the ephemeris values for the spacecraft shown in the other plot panels may be considerably different from the values given for the spacecraft in the bottom panel. At the very bottom of the page are given the date and start time of the plots. At the top of the page, the WBD mode is noted, along with the FFT length and overlap. 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. There will typically be a separate survey spectrogram plot for each operating mode. The time resolution of the data shown in the plots is determined from the WBD instrument mode and FFT length. 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). When data from multiple spacecraft are shown in the overview plots, the time span in which WBD data are available for each spacecraft may be different. Periods when no data were available will appear white on the overview plots. On the lower right-hand corner of the page, UIowa appears next to the date on which the plot was generated in the format YYMMDD. Please note that during operations in certain magnetospheric regions, the WBD Plasma Wave Receiver may cycle between electric and magnetic field antennas or through the 125.454 kHz, 250.908 kHz, and 501.816 kHz conversion frequencies. When the instrument cycles through different modes, separate ps overview plots are generated for each antenna or conversion frequency used over the entire duration of the operation. In these plots, only data from one mode are shown on each plot, and the data are dilated across the intervals when another mode was used. The modes used and the length of the cycling intervals are provided on the left-hand side of the ps overview plot, along with a note that the plot is not intended for publication. Please contact the WBD PI if you wish to publish or present data from periods with cyclical switching between instrument modes. Higher time resolution spectrograms are also available for each spacecraft separately. These data are presented as ten minute time span and 30 second time span GIF image files. Details on Cluster WBD Interpretation Issues can be found at http://www-pw.physics.uiowa.edu/cluster/interpretation_issues/interpretation.html 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). 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.

33) Cluster II Summary Parameter Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/WHISPER/SummaryParameter/60S
Start:2001-01-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2016-05-19 13:22:47 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.

34) IBEX Background Monitor Counts maxmize
Resource ID:spase://VEPO/NumericalData/IBEX/BM/Counts/PT0.24S
Start:2008-12-25 00:00:00 Observatory: Cadence:1 second
Stop:2009-06-19 00:00:00 Instrument: Resource:NumericalData
Each record captures the counts of >~14 keV protons arriving at the IBEX Background Monitor. Also included are a time tag (seconds since 00:00 UT of January 6, 1980), an arrival direction (R.A. and Dec. in J2000 celestial coordinates), and the IBEX location. Data files are given for each 8-day orbit. The data files are in ASCII.

35) IMP 8 CPME EPE MAG PLS Merge Data Set maxmize
Resource ID:spase://VEPO/NumericalData/IMP8/CPME/EPE/PT20S
Start:1973-10-28 00:00:00 Observatory:IMP 8 Cadence:20 seconds
Stop:2000-12-31 00:00:00 Instrument:Charged Particle Measurements Experiment (CPME) Resource:NumericalData
This data set contains 20.48s IMP8 CPME and EPE energetic particle data, along with IMP8 magnetic field and plasma data to facilitate use of the particle data. CPME data consist of: spin-integrated, 20.48s resolution count rates of protons in ten energy channels (0.29-0.50 to 90-440 MeV), of alpha particles in six channels (0.59-1.14 to 28-52 MeV/n), of Z>=3 particles in five channels (0.70-1.45 to 6-105 MeV/n), of electrons in 3 channels (0.22-2.5 to 0.80-2.5 MeV), of protons and alpha particles mixed in two channels (>35, >50 MeV/n) and uncertainties in all the preceding 20-s rates; spin-integrated, 10.24s count rates of protons in three energy channels (0.29-0.50 to 0.96-2.00 MeV) and of electrons in the three energy channels given above, plus uncertainties and data quality flags for all these 10.24s rates; 10.24s count rates in 8 spin sectors for 0.29-0.50 MeV protons and for 0.22-2.50 MeV electrons and their uncertainties and dataquality flags; 20.48s count rates in 8 spin sectors for 0.59-1.14 and 1.8-4.2 MeV/n alpha particles and for 0.7-3.3 and 3.1-8.8 MeV/n Z>= 3 particles, and their uncertainties anddata quality flags. EPE data consist of 16-sectored, 20.48s counts (not rates) for Z>=1 particles in 0.05-0.22 and 0.22-0.80 MeV/n channels, for electrons in 0.03-0.10 and 0.10-0.20 MeV channels and for Z>=1, E>0.015 MeV/n particles and electrons mixed. Magnetic field data include GSE and GSM cartesian components and direction angles. Plasma data, mainly from the MIT Faraday Cup, include flow velocity, density and temperature. Better sources exist for those desiring only IMP8 magnetic field and/or plasma data. Data are available as daily gzipped ASCII files; spin- integrated, 20.48s CPME count rates are also available with display and subset capability via FTPBrowser.

36) IMP 8 CRNC hourly energetic electron fluxes maxmize
Resource ID:spase://VEPO/NumericalData/IMP8/CRNC/Electrons_PT1H
Start:1973-10-30 00:00:00 Observatory:IMP 8 Cadence:1 hour
Stop:2001-10-26 00:00:00 Instrument:Cosmic Ray Nuclear Composition Resource:NumericalData
This data set contains hourly, spin-averaged fluxes of electrons from the IMP8 Cosmic Ray Nuclear Composition experiment of U. Chicago and UNH. There are fluxes of electrons in three energy bins: 0.7-2.0, 2-12, 12-50 MeV. These fluxes were generated at GSFC/SPDF from count rates accessible from UNH.

37) IMP 8 CRNC hourly count rates of heavy nuclei maxmize
Resource ID:spase://VEPO/NumericalData/IMP8/CRNC/Heavies_PT1H
Start:1973-10-30 00:00:00 Observatory:IMP 8 Cadence:1 hour
Stop:2001-10-26 00:00:00 Instrument:Cosmic Ray Nuclear Composition Resource:NumericalData
This data set contains hourly, spin-averaged count rates of heavy nuclei, and of particles penetrating the anticoincidence sensor, from the IMP8 Cosmic Ray Nuclear Composition experiment of U. Chicago and UNH. Included are rates of CNO nuclei at E.LT.80 MeV/n and E.GT.80 MeV/n, of Z.GT.8 nuclei at "low" and "high" energies, and of penetrating particles (protons with E.GT.106 MeV, etc.)

38) IMP 8 CRNC hourly energetic alpha particle fluxes maxmize
Resource ID:spase://VEPO/NumericalData/IMP8/CRNC/Helium_PT1H
Start:1973-10-30 00:00:00 Observatory:IMP 8 Cadence:1 hour
Stop:2001-10-26 00:00:00 Instrument:Cosmic Ray Nuclear Composition Resource:NumericalData
This data set contains hourly, spin-averaged fluxes of alpha particles from the IMP8 Cosmic Ray Nuclear Composition experiment of U. Chicago and UNH. There are fluxes of alpha particles in 9 energy bins from 10.90-12.89 to 84.32-94.81 MeV/n. These fluxes were generated at GSFC/SPDF from count rates accessible from UNH.

39) IMP 8 CRNC 15-min PHA and coincidence mode counts maxmize
Resource ID:spase://VEPO/NumericalData/IMP8/CRNC/PT15M
Start:1973-10-30 00:00:00 Observatory:IMP 8 Cadence:15 minutes
Stop:2000-09-30 00:00:00 Instrument:Cosmic Ray Nuclear Composition Resource:NumericalData
This 15-min-resolution data set consists of 5 count rates from the Low Energy Telescope, 8 count rates for the main telescope (MT), 4 counts of pulse height analyzed events in each of 4 MT coincidence modes, and 27 box counts corresponding to specific species and energy ranges associated with 3 of the MT coincidence modes. Actually the 13 referenced "count rates" are given as paired counts and accumulation times. Associated documentation suggests algorithms for computation of count rates and fluxes from the MT data given, for electrons in 3 energy bands (0.7-2.0, 2.0-12, 12-50 MeV), protons in 9 bands (11.24-20.00 MeV to 74.50-94.78 MeV), helium nuclei in 10 bands (10.90-12.89 MeV per n to 84.32-94.81 MeV per n), and CNO nuclei in 1 band (25 - 250 Mev per n). There are no azimuthally sectored data in this data set. The data are accessible via ftp and, with higher functionality, via FTPBrowser.

40) IMP 8 CRNC hourly energetic proton fluxes maxmize
Resource ID:spase://VEPO/NumericalData/IMP8/CRNC/Protons_PT1H
Start:1973-10-30 00:00:00 Observatory:IMP 8 Cadence:1 hour
Stop:2001-10-26 00:00:00 Instrument:Cosmic Ray Nuclear Composition Resource:NumericalData
This data set contains hourly, spin-averaged fluxes of protons from the IMP8. Cosmic Ray Nuclear Composition experiment of U. Chicago and UNH. There are are fluxes of protons in 9 energy bins from 11.24-12.62 to 74.50-94.78 MeV. These fluxes were generated at GSFC/SPDF from count rates accessible from UNH.

41) IMP 8 UMD EECA 10.92m Rates, PHA maxmize
Resource ID:spase://VEPO/NumericalData/IMP8/EECA/PT11M
Start:1973-11-01 00:00:00 Observatory:IMP 8 Cadence:11 minutes
Stop:2001-10-26 00:00:00 Instrument:Solid-State Detectors Resource:NumericalData
This data set, from the Electrostatic Energy-Charge Analyzer (EECA) part of the U. Maryland experiment on IMP 8, contains count rate and pulse height data enabling the computation of 10.92-min resolution fluxes of: singly ionized ions in 5 energy/charge windows of lower limits between 130 and 740 keV/Q; doubly charged ions in the same 5 keV/Q windows plus another at 65 keV/Q; ions with charge states between 5 and 8 in the same 6 keV/Q windows as for doubly charged ions plus another at 37 keV/Q; ions with charge states above about 10 at 37 and 65 keV/Q windows; 600-860 keV electrons. Some of the modes are spin integrated while others are given in 90 deg quadrants about the spacecraft spin vector (which is normal to the ecliptic plane). The data set was created at NSSDC from the U.Md.-provided "summary tapes" (NSSDC IDs SPHE-00170 and 73-078A-03C) by dropping engineering data, dropping data from the ULET portion of the overall experiment (the ULET instrument failed in 1978), and converting the remaining time, spacecraft position, and EECA instrument data from binary to ASCII representation. The data are available via ftp in 1- month files of variable lengths in the 3-6 MB size range.

42) IMP 8 GME 30-min energetic particle rates and fluxes maxmize
Resource ID:spase://VEPO/NumericalData/IMP8/GME/PT30M
Start:1973-11-01 00:00:00 Observatory:IMP 8 Cadence:30 minutes
Stop:2001-10-26 00:00:00 Instrument:Solar and Cosmic-Ray Particles Resource:NumericalData
This CDAWeb-accessible data set contains 30-minute, spin-averaged count rates and fluxes, and their statistical uncertainties, of energetic particles from the IMP8 GME experiment. Included are fluxes of: protons in 30 energy bins from 0.88-1.15 to 327-485 MeV; alpha particles in 21 energy bins from 1.14-1.36 to 63.3-81.0 MeV/n; and 0.3-18 MeV electrons. Also included are count rates for each of 7 sensors and for 11 multi-sensor coincidence modes. Proton and alpha particle fluxes, for every other energy bin, are given at the FTPBrowser and MSSP interfaces identified below.

43) ISEE-2 magnetometer 1-min data at CDAWeb maxmize
Resource ID:spase://VMO/NumericalData/ISEE2/MAG/PT1M
Start:1977-10-22 21:04:19 Observatory:ISEE 2 Cadence:1 minute
Stop:1987-09-26 16:10:30 Instrument:ISEE 2 Fluxgate Magnetometer, Tri-axial Resource:NumericalData
This data set contains magnetic field component and magnitude averages every minute, with components given in spacecraft, GSE and GSM coordinates. Standard deviations in the averages are given, as are differences between the averages and model field vectors. Geocentric (GSE and GSM) spacecraft position information is given, as is ISEE1-ISEE2 separation vector information. ISEE 2 spin vector direction and ISEE 2 velocity vector information, relative to the Earth and to ISEE 1, are given. Miscellaneous other parameters are also given. Data are accessible as plots, lists and files from CDAWeb, and as CDF files from CDAWeb's ftp area.

44) ISEE-2 magnetometer 4-sec data maxmize
Resource ID:spase://VMO/NumericalData/ISEE2/MAG/PT4S
Start:1977-10-22 14:49:19 Observatory:ISEE 2 Cadence:4 seconds
Stop:1987-09-26 05:59:00 Instrument:ISEE 2 Fluxgate Magnetometer, Tri-axial Resource:NumericalData
4-sec vector magnetic field values recorded by the ESA ISEE-2 satellite, in spacecraft coordinates (close to GSE), available from UCLA and CDAWeb value-added interfaces and, via ftp, in binary from UCLA and in CDF from CDAWeb. (This descriptor updated, 6/20110, by J.King, to reflect CDAWeb accessibilityand to insert CDAWeb parameter keys.)

45) Interball-1 6-sec vector magnetic field data maxmize
Resource ID:spase://VMO/NumericalData/Interball-1/FM3I/PT6S
Start:1995-08-06 07:11:09 Observatory:Interball-1 Cadence:6 seconds
Stop:2000-10-15 21:53:26 Instrument:Interball-1 Tri-axial Fluxgate Magnetometer FGM-I Resource:NumericalData
Magnetic field measurements on-board the Interball 1 probe are carried out by the FM-3I and MFI (FGM-I) instruments. Data presented here are the combination of the data of all magnetometers. First, all FM-3I M1 data are used, if they are absent, the MFI data are used, and if data from both magnetometer are absent, FM-3I M2 data presented. The FM-3 M1 and MFI data are averaged over 6-second time intervals.

46) Hourly Cosmic Ray Intensities from the Climax Neutron Monitor maxmize
Resource ID:spase://VEPO/NumericalData/NeutronMonitor/Climax/PT1H
Start:1951-01-01 00:00:00 Observatory:Climax Cadence:1 hour
Stop:2006-11-30 23:59:59 Instrument:Climax Neutron Monitor Resource:NumericalData
Hourly averages of relativistic cosmic ray intensities from the Climax Neutron Monitor

47) Daily Average Cosmic Ray Intensities from the Climax, Huancayo, and Haleakala Neutron Monitors maxmize
Resource ID:spase://VEPO/NumericalData/NeutronMonitor/Climax_Huancayo_Haleakala/P1D
Start:1953-01-01 00:00:00 Observatory:Climax Cadence:27 days
Stop:1992-12-31 23:59:59 Instrument:Climax Neutron Monitor Resource:NumericalData
Daily averages of relativistic cosmic ray intensities from the Climax, Huancayo, and Haleakala Neutron Monitors

48) Cosmic Ray Intensities Averaged over Bartels Solar Rotations from the Climax, Huancayo, and Haleakala Neutron Monitors maxmize
Resource ID:spase://VEPO/NumericalData/NeutronMonitor/Climax_Huancayo_Haleakala/P27D
Start:1951-01-18 00:00:00 Observatory:Climax Cadence:27 days
Stop:2006-11-09 23:59:59 Instrument:Climax Neutron Monitor Resource:NumericalData
Bartels Rotation averages of relativistic cosmic ray intensities from the Climax, Huancayo, and Haleakala Neutron Monitors For Climax only, averages are given both including and excluding days with significant contributions from ground level solar particle events.

49) Hourly Cosmic Ray Intensities from Neutron Monitors at Fort Smith, Peawanuck, Nain, and Inuvik maxmize
Resource ID:spase://VEPO/NumericalData/NeutronMonitor/FtSmith_Peawanuck_Nain_Inuvik/PT1H
Start:2000-01-01 00:00:00 Observatory:Fort Smith Cadence:1 hour
Stop:2016-02-19 13:22:19 Instrument:Fort Smith Neutron Monitor Resource:NumericalData
Hourly averages of relativistic cssmic ray intensities from Bartol Research Institute Neutron Monitors at Fort Smith, Peawanuck, Nain, and Inuvik

50) Hourly Cosmic Ray Intensities from the Haleakala Neutron Monitor maxmize
Resource ID:spase://VEPO/NumericalData/NeutronMonitor/Haleakala/PT1H
Start:1953-01-01 00:00:00 Observatory:Haleakala Cadence:1 hour
Stop:1992-12-31 23:59:59 Instrument:Haleakala Neutron Monitor Resource:NumericalData
Hourly averages of relativistic cosmic ray intensities from the Haleakala Neutron Monitor

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