Commit 31709966a27c666affc347d2cb4288b8f3e166b8
1 parent
85681ec4
Exists in
master
and in
12 other branches
work
Showing
13 changed files
with
26 additions
and
51 deletions
Show diff stats
Instrument/AMDA/Cluster-Rumba/EFW.xml
| ... | ... | @@ -4,8 +4,8 @@ |
| 4 | 4 | <Instrument> |
| 5 | 5 | <ResourceID>spase://CDPP/Instrument/AMDA/Cluster-Rumba/EFW</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Electric Field and Waves (EFW)</ResourceName> | |
| 8 | - <AlternateName>EFW</AlternateName> | |
| 7 | + <ResourceName>EFW</ResourceName> | |
| 8 | + <AlternateName>Electric Field and Waves (EFW)</AlternateName> | |
| 9 | 9 | <ReleaseDate>2011-02-04T15:37:46Z</ReleaseDate> |
| 10 | 10 | <Description>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 Wave Experiment for the Cluster Mission,'' by G. Gustafsson et al., from which this information was obtained.</Description> |
| 11 | 11 | <Contact> |
| ... | ... |
Instrument/AMDA/Cluster-Rumba/Ephemeris.xml
| ... | ... | @@ -4,7 +4,7 @@ |
| 4 | 4 | <Instrument> |
| 5 | 5 | <ResourceID>spase://CDPP/Instrument/AMDA/Cluster-Rumba/Ephemeris</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Cluster-Rumba Positions</ResourceName> | |
| 7 | + <ResourceName>Ephemeris</ResourceName> | |
| 8 | 8 | <AlternateName>Cluster-Rumba Ephemeris</AlternateName> |
| 9 | 9 | <ReleaseDate>2011-02-04T15:37:46Z</ReleaseDate> |
| 10 | 10 | <Description>Cluster-Rumba spacecraft positions in various coordinate systems</Description> |
| ... | ... |
Instrument/AMDA/Cluster-Rumba/FGM.xml
| ... | ... | @@ -4,8 +4,8 @@ |
| 4 | 4 | <Instrument> |
| 5 | 5 | <ResourceID>spase://CDPP/Instrument/AMDA/Cluster-Rumba/FGM</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Fluxgate Magnetometer (FGM)</ResourceName> | |
| 8 | - <AlternateName>FGM</AlternateName> | |
| 7 | + <ResourceName>FGM</ResourceName> | |
| 8 | + <AlternateName>Fluxgate Magnetometer (FGM)</AlternateName> | |
| 9 | 9 | <ReleaseDate>2011-02-04T15:37:46Z</ReleaseDate> |
| 10 | 10 | <Description>This instrument (FGM: Fluxgate Magnetometer) consists of two tri-axial fluxgate magnetometers mounted on one of the two 5 m radial booms, plus a data processing unit (DPU) on the main equipment platform. The magnetometer boom lies in the spacecraft spin plane, with the outboard sensor at the boom tip and the inboard sensor mounted 1.5 m inboard from the tip, to minimize the importance of the spacecraft background magnetic field and its variations. The sensors are mounted such that the X axes are aligned with the spacecraft spin axis, and the other axes are in the spin plane. There are five sensitivity ranges, from +/- 256 nT to +/- 65,500 nT (used only to facilitate ground testing). Range switching can be automatic or by command. Calibration is done by introducing a known current step into the feedback loop of the sensors. Telemetry allocation limits the normal output to about 20 vectors/s. For short periods at higher time resolution, data are stored at rates of up to 124.3 vectors/s in a memory block, the micro-structure analyzer (MSA). The MSA capacity is 32,000 vectors, more than 4 minutes of data at the highest sampling rate. This memory is continually over-written until a special event is detected, when its contents are frozen and held for readout interleaved with the normal lower-resolution data. The DPU has dual redundancy, including two CPUs. The CPU convolves the full bandwidth data with a Gaussian digital filter to match the rate and bandwidth of the transmitted vectors to the available telemetry rate. Unfiltered vector data are sent at 64.35 ms intervals to all but one of the other experiments. The DPU has a number of stored algorithms for recognition of events of particular interest, to trigger the MSA. The objective is to identify such events as boundary crossings or shocks when the high-rate capability of the MSA for short periods could capture the detailed signature of the event. The algorithms were defined at an early stage, but resettable thresholds for the event triggers will enable optimization in flight. There are eight different telemetry operating modes of the instrument, corresponding to both normal and burst modes, with MSA readout rates of 0, 9, 12, or 120 vectors/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 Magnetic Field Investigation: scientific objective and instrumentation,'' by A. Balogh et al., from which this information was obtained.</Description> |
| 11 | 11 | <Contact> |
| ... | ... |
Instrument/AMDA/Cluster-Rumba/PEACE.xml
| ... | ... | @@ -4,8 +4,8 @@ |
| 4 | 4 | <Instrument> |
| 5 | 5 | <ResourceID>spase://CDPP/Instrument/AMDA/Cluster-Rumba/PEACE</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Plasma Electron and Current Experiment (PEACE)</ResourceName> | |
| 8 | - <AlternateName>PEACE</AlternateName> | |
| 7 | + <ResourceName>PEACE</ResourceName> | |
| 8 | + <AlternateName>Plasma Electron and Current Experiment (PEACE)</AlternateName> | |
| 9 | 9 | <ReleaseDate>2011-02-04T15:37:46Z</ReleaseDate> |
| 10 | 10 | <Description>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.</Description> |
| 11 | 11 | <Contact> |
| ... | ... |
Instrument/AMDA/Cluster-Rumba/RAPID.xml
| ... | ... | @@ -4,8 +4,8 @@ |
| 4 | 4 | <Instrument> |
| 5 | 5 | <ResourceID>spase://CDPP/Instrument/AMDA/Cluster-Rumba/RAPID</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Research with Adaptive Particle Imaging Detectors (RAPID)</ResourceName> | |
| 8 | - <AlternateName>RAPID</AlternateName> | |
| 7 | + <ResourceName>RAPID </ResourceName> | |
| 8 | + <AlternateName>Research with Adaptive Particle Imaging Detectors (RAPID)</AlternateName> | |
| 9 | 9 | <ReleaseDate>2011-02-04T15:37:47Z</ReleaseDate> |
| 10 | 10 | <Description>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. Angular distributions are measured over a range of 180 degrees in polar angle for either species. Electrons are identified by the well-known energy-range relationship. The detection principle for ions is based on a two-dimensional analysis of a particle's velocity and energy. Moderate mass resolution of about four (for oxygen ions) permits the identification of ions and ion groups of significance. Particle species identified are electrons, protons, He and CNO group ions, and energetic neutral atoms of energies 10--100 KeV. RAPID science data are transmitted through a complex data format, using 17 Kbps in the telemetry nominal mode. Time resolution is as high as 16 samples/spin for certain elements. The nominal spin period for the spacecraft is 4 s. The RAPID field of view covers a range of 180 degrees with respect to the spin vector. The sensor systems, IIMS and IES, scan the full range of the solid angle as the spacecraft rotates. The data returned will be used to project the intensity distribution in distant particle sources on a spherical or plane image area with 192 pixels for IIMS and 144 pixels for IES. The Imaging Ion Mass Spectrometer (IIMS) sensor system is composed of three identical SCENIC (Spectroscopic Camera for Electrons, Neutral and Ion Composition) heads. The sensor systems of IIMS are identical to those in the HEP-LD instrument included in the Japanese Geotail spacecraft. The IIMS uses two-dimensional time-of-flight/energy analysis to determine particle mass. The addition of position-sensing techniques on the entrance foil, in combination with a geometrically small stop detector at the end of the flight path provides directional sensitivity. This approach divides the 180 degree polar segment into twelve contiguous angular intervals. Sectoring the spacecraft spin plane with a maximum of sixteen azimuthal intervals covers the unit sphere in velocity space completely with a total of 192 angular bins. The Imaging Electron Spectrometer (IES) achieves directional sensitivity by using novel microstrip solid-state devices in combination with a pin-hole acceptance. This technique divides the 180 degree polar range into nine angular intervals which, with sixteen sectors in the spin plane, corresponds to a total of 144 bins on the unit sphere. The RAPID spectrometer is connected to the magnetic field instrument FGM through the inter-experiment link. FGM sends 64 uncorrected magnetic field vectors per spacecraft rotation. These are used by the data processor to determine, for each of the sixteen azimuthal sectors, which look directions in the IIMS and IES fans are perpendicular to the current magnetic field vector. 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.</Description> |
| 11 | 11 | <Contact> |
| ... | ... |
Instrument/AMDA/Cluster-Rumba/STAFF.xml
| ... | ... | @@ -4,8 +4,8 @@ |
| 4 | 4 | <Instrument> |
| 5 | 5 | <ResourceID>spase://CDPP/Instrument/AMDA/Cluster-Rumba/STAFF</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF)</ResourceName> | |
| 8 | - <AlternateName>STAFF</AlternateName> | |
| 7 | + <ResourceName>STAFF</ResourceName> | |
| 8 | + <AlternateName>Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF)</AlternateName> | |
| 9 | 9 | <ReleaseDate>2011-02-04T15:37:47Z</ReleaseDate> |
| 10 | 10 | <Description>This experiment (STAFF: Spatio-Temporal Analysis of Field Fluctuations) is one of the five complementary experiments which form the Wave Experiment Consortium (WEC) on Cluster. STAFF consists of: (1) a triaxial boom-mounted search-coil magnetometer to measure the magnetic components of electromagnetic fluctuations (up to 4 KHz); and, (2) a spectrum analyzer to compute the 25 auto- and cross-correlation coefficients of the spectral matrix, using three magnetic and two electric components of the waves. The magnetic waveform (up to either 10 Hz or 180 Hz) is also transmitted. The Z-axis sensor is parallel to the spacecraft spin axis. Each sensor consists of a high-permeability core embedded inside two solenoids. The frequency response of the main winding is flattened by a secondary winding through a flux feedback effect, in the range 40--4000 Hz. Further, the secondary winding is used as a calibration loop to which an external AC signal is applied. In normal bit rate the wave-form data cover the 0.1--10 Hz frequency range, and the spectrum analyzer covers the range 8 Hz to 4 KHz. In high bit rate, the wave-form data cover 0.1--180 Hz and the spectrum analyzer covers 64 Hz to 4 KHz, using only the two highest frequency bands. 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. Other modes are also defined. The analysis will also use electric field waveform data from the EFW (part of WEC), and the hardware of the two instruments was designed to optimize correlation: low-pass filters are identical, sampling frequency is the same, and there is a synchronization signal for simultaneous sampling. The output signals of the STAFF magnetic preamplifiers are also sent to two other instruments: the WBD (part of WEC) and the EDI. Some of the magnetospheric structures to be studied are of small scale, and where the signature duration is of the order 1 s or less, the STAFF search coil data are complementary to those of the fluxgate magnetometer (FGM). 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.</Description> |
| 11 | 11 | <Contact> |
| ... | ... |
Instrument/AMDA/Cluster-Rumba/WHISPER.xml
| ... | ... | @@ -4,8 +4,8 @@ |
| 4 | 4 | <Instrument> |
| 5 | 5 | <ResourceID>spase://CDPP/Instrument/AMDA/Cluster-Rumba/WHISPER</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER)</ResourceName> | |
| 8 | - <AlternateName>WHISPER</AlternateName> | |
| 7 | + <ResourceName>WHISPER</ResourceName> | |
| 8 | + <AlternateName>Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER)</AlternateName> | |
| 9 | 9 | <ReleaseDate>2011-02-04T15:37:47Z</ReleaseDate> |
| 10 | 10 | <Description>This instrument (WHISPER: Waves of HIgh frequency and Sounder for Probing of the Electron density by Relaxation) is part of the Wave Experiment Consortium (WEC) on Cluster. Its objectives are to: (1) measure the electron density via active sounding of plasma resonances; and, (2) record via passive wave analysis the natural wave emissions in the high-frequency range, from 4--80 KHz. An active sounder can provide the total local electron density, including the cold component, which is the dominant one in many of the regions to be explored. Most of the time, this cold component cannot be obtained from particle experiments, owing to the satellite's electric potential and photoelectron sheath disturbance. The sounder consists of three main parts: (1) a sensitive double-sphere antenna, measuring the AC electric field, provided as part of the EFW experiment; (2) a transmitter, a receiver, a digital spectrum analyzer, and a controller unit, which form the WHISPER instrument itself; and, (3) command and data processing systems, which are part of the DWP experiment, which also takes care of command and telemetry for the entire WEC unit. During the active part of WHISPER operation, in each frequency step a short (1 ms in normal mode; 0.5 ms also possible) wave train at the fixed frequency is transmitted. The receiver is then activated to receive until the end of the frequency step. This is repeated for a series of frequencies, sweeping a designated range of frequencies. The frequency step duration is a multiple of 13.33 ms to allow good synchronization with the EFW instrument's sampling period, and ranges up to ~250 ms. The sweep duration is a number of steps, and ranges from 0.5 s to ~10 s. The total frequency range available for the active transmitter is from 4--80 KHz. Different signal strength levels can be selected, e.g. 50, 100, 200 V peak to peak. During passive operations, there is no short pulse transmitted. The receiver signal is measured each 13.33 ms, and after A/D conversion it is analyzed in frequency by the vector signal processor (VSP), which performs a fast Fourier transform and delivers 64 to 512 useful bins in the range 0--80 KHz. The 512-bin option is always used in sounding mode. The operational details of the instrument are managed by the microcontroller, which also handles the interface to the DWP. Extensive data compression is used, either in the DWP (normal) or within WHISPER itself as backup. There is a considerable number of WHISPER modes, with a corresponding range of frequency resolutions and final data rates. In the standard WEC modes, the telemetry rate is about 980 bps in routine and 5800 bps in high rate. Plasma densities from 0.2 to 80 cm**-3 are measured, with a time resolution of 4 s routine and 1 s at best. Natural wave electric fields are measured with a sensitivity of 0.05 microV/(m sqrt(Hz)). Time and frequency resolutions are 3 s and 640 Hz routine, and 100 ms and 320 Hz at best. In any given mode, the dynamic range is about 100 dB, but 124 dB absolute range can be reached by commanded gain change. 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.</Description> |
| 11 | 11 | <Contact> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-efw-gse.xml
| ... | ... | @@ -4,7 +4,7 @@ |
| 4 | 4 | <NumericalData> |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-efw-gse</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Cluster II Rumba Prime Parameter Electric Field and Waves (EFW) Data</ResourceName> | |
| 7 | + <ResourceName>efield gse</ResourceName> | |
| 8 | 8 | <AlternateName>Cluster 1 Prime Parameter EFW Data</AlternateName> |
| 9 | 9 | <ReleaseDate>2015-10-19T11:00:44Z</ReleaseDate> |
| 10 | 10 | <Description>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.</Description> |
| ... | ... | @@ -17,11 +17,7 @@ |
| 17 | 17 | <Name>NSSDC Master Catalog listing for Cluster II Rumba Electric Field and Waves (EFW)</Name> |
| 18 | 18 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| 19 | 19 | <Description>This site provides information concerning the Cluster II Rumba Electric Field and Waves Instrument.</Description> |
| 20 | - </InformationURL> | |
| 21 | - <Association> | |
| 22 | - <AssociationID>spase://SMWG/Observatory/Cluster-Rumba</AssociationID> | |
| 23 | - <AssociationType>ObservedBy</AssociationType> | |
| 24 | - </Association> | |
| 20 | + </InformationURL> | |
| 25 | 21 | </ResourceHeader> |
| 26 | 22 | <AccessInformation> |
| 27 | 23 | <RepositoryID>spase://SMWG/Repository/CDPP/AMDA</RepositoryID> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-efw-ppp.xml
| ... | ... | @@ -4,7 +4,7 @@ |
| 4 | 4 | <NumericalData> |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-efw-ppp</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Cluster II Rumba Prime Parameter Electric Field and Waves (EFW) Data</ResourceName> | |
| 7 | + <ResourceName>efield ppp</ResourceName> | |
| 8 | 8 | <AlternateName>Cluster 1 Prime Parameter EFW Data</AlternateName> |
| 9 | 9 | <ReleaseDate>2015-10-16T16:51:44Z</ReleaseDate> |
| 10 | 10 | <Description>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.</Description> |
| ... | ... | @@ -17,11 +17,7 @@ |
| 17 | 17 | <Name>NSSDC Master Catalog listing for Cluster II Rumba Electric Field and Waves (EFW)</Name> |
| 18 | 18 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| 19 | 19 | <Description>This site provides information concerning the Cluster II Rumba Electric Field and Waves Instrument.</Description> |
| 20 | - </InformationURL> | |
| 21 | - <Association> | |
| 22 | - <AssociationID>spase://SMWG/Observatory/Cluster-Rumba</AssociationID> | |
| 23 | - <AssociationType>ObservedBy</AssociationType> | |
| 24 | - </Association> | |
| 20 | + </InformationURL> | |
| 25 | 21 | </ResourceHeader> |
| 26 | 22 | <AccessInformation> |
| 27 | 23 | <RepositoryID>spase://SMWG/Repository/CDPP/AMDA</RepositoryID> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-efw-sr2.xml
| ... | ... | @@ -4,7 +4,7 @@ |
| 4 | 4 | <NumericalData> |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-efw-sr2</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Cluster II Rumba Prime Parameter Electric Field and Waves (EFW) Data</ResourceName> | |
| 7 | + <ResourceName>efield sr2</ResourceName> | |
| 8 | 8 | <AlternateName>Cluster 1 Prime Parameter EFW Data</AlternateName> |
| 9 | 9 | <ReleaseDate>2015-10-16T15:51:44Z</ReleaseDate> |
| 10 | 10 | <Description>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.</Description> |
| ... | ... | @@ -17,11 +17,7 @@ |
| 17 | 17 | <Name>NSSDC Master Catalog listing for Cluster II Rumba Electric Field and Waves (EFW)</Name> |
| 18 | 18 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| 19 | 19 | <Description>This site provides information concerning the Cluster II Rumba Electric Field and Waves Instrument.</Description> |
| 20 | - </InformationURL> | |
| 21 | - <Association> | |
| 22 | - <AssociationID>spase://SMWG/Observatory/Cluster-Rumba</AssociationID> | |
| 23 | - <AssociationType>ObservedBy</AssociationType> | |
| 24 | - </Association> | |
| 20 | + </InformationURL> | |
| 25 | 21 | </ResourceHeader> |
| 26 | 22 | <AccessInformation> |
| 27 | 23 | <RepositoryID>spase://SMWG/Repository/CDPP/AMDA</RepositoryID> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-pot-full.xml
| ... | ... | @@ -4,7 +4,7 @@ |
| 4 | 4 | <NumericalData> |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-pot-full</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Cluster II Rumba Prime Parameter Electric Field and Waves (EFW) Data</ResourceName> | |
| 7 | + <ResourceName>Cpot full</ResourceName> | |
| 8 | 8 | <AlternateName>Cluster 1 Prime Parameter EFW Data</AlternateName> |
| 9 | 9 | <ReleaseDate>2015-10-16T11:32:44Z</ReleaseDate> |
| 10 | 10 | <Description>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.</Description> |
| ... | ... | @@ -17,11 +17,7 @@ |
| 17 | 17 | <Name>NSSDC Master Catalog listing for Cluster II Rumba Electric Field and Waves (EFW)</Name> |
| 18 | 18 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| 19 | 19 | <Description>This site provides information concerning the Cluster II Rumba Electric Field and Waves Instrument.</Description> |
| 20 | - </InformationURL> | |
| 21 | - <Association> | |
| 22 | - <AssociationID>spase://SMWG/Observatory/Cluster-Rumba</AssociationID> | |
| 23 | - <AssociationType>ObservedBy</AssociationType> | |
| 24 | - </Association> | |
| 20 | + </InformationURL> | |
| 25 | 21 | </ResourceHeader> |
| 26 | 22 | <AccessInformation> |
| 27 | 23 | <RepositoryID>spase://SMWG/Repository/CDPP/AMDA</RepositoryID> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-pot-spin.xml
| ... | ... | @@ -4,7 +4,7 @@ |
| 4 | 4 | <NumericalData> |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-pot-spin</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Cluster II Rumba Prime Parameter Electric Field and Waves (EFW) Data</ResourceName> | |
| 7 | + <ResourceName>pot spin</ResourceName> | |
| 8 | 8 | <AlternateName>Cluster 1 Prime Parameter EFW Data</AlternateName> |
| 9 | 9 | <ReleaseDate>2015-10-16T11:41:44Z</ReleaseDate> |
| 10 | 10 | <Description>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.</Description> |
| ... | ... | @@ -17,11 +17,7 @@ |
| 17 | 17 | <Name>NSSDC Master Catalog listing for Cluster II Rumba Electric Field and Waves (EFW)</Name> |
| 18 | 18 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| 19 | 19 | <Description>This site provides information concerning the Cluster II Rumba Electric Field and Waves Instrument.</Description> |
| 20 | - </InformationURL> | |
| 21 | - <Association> | |
| 22 | - <AssociationID>spase://SMWG/Observatory/Cluster-Rumba</AssociationID> | |
| 23 | - <AssociationType>ObservedBy</AssociationType> | |
| 24 | - </Association> | |
| 20 | + </InformationURL> | |
| 25 | 21 | </ResourceHeader> |
| 26 | 22 | <AccessInformation> |
| 27 | 23 | <RepositoryID>spase://SMWG/Repository/CDPP/AMDA</RepositoryID> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster1/PEACE/clust1-pea-mom.xml
| ... | ... | @@ -4,7 +4,7 @@ |
| 4 | 4 | <NumericalData> |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster1/PEACE/clust1-pea-mom</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName>Cluster II Rumba Prime Parameter Plasma Electron and Current Experiment (PEACE) Moments</ResourceName> | |
| 7 | + <ResourceName>PEACE moments</ResourceName> | |
| 8 | 8 | <AlternateName>Cluster 1 Prime Parameter PEACE Data</AlternateName> |
| 9 | 9 | <ReleaseDate>2015-10-16T16:51:44Z</ReleaseDate> |
| 10 | 10 | <Description>The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) |
| ... | ... | @@ -44,17 +44,12 @@ |
| 44 | 44 | <Contact> |
| 45 | 45 | <PersonID>spase://SMWG/Person/Elena.Budnik</PersonID> |
| 46 | 46 | <Role>TechnicalContact</Role> |
| 47 | - </Contact> | |
| 48 | - | |
| 47 | + </Contact> | |
| 49 | 48 | <InformationURL> |
| 50 | 49 | <Name>NSSDC Master Catalog listing for Cluster II Rumba Plasma Electron and Current Experiment (PEACE)</Name> |
| 51 | 50 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-05</URL> |
| 52 | 51 | <Description>This site provides information concerning the Cluster II Rumba Plasma Electron and Current Experiment Instrument.</Description> |
| 53 | - </InformationURL> | |
| 54 | - <Association> | |
| 55 | - <AssociationID>spase://SMWG/Observatory/Cluster-Rumba</AssociationID> | |
| 56 | - <AssociationType>ObservedBy</AssociationType> | |
| 57 | - </Association> | |
| 52 | + </InformationURL> | |
| 58 | 53 | </ResourceHeader> |
| 59 | 54 | <AccessInformation> |
| 60 | 55 | <RepositoryID>spase://SMWG/Repository/CDPP/AMDA</RepositoryID> |
| ... | ... |