|
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C1_CQ_CIS-HIA_CAVEATS
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Mixed time resolution: 1/16 s for normal and 1/128 s for burst mode The AEC (*.edi_ae_cor) files were used to correct for angular (theta-phi) dependence of the efficieny The correction is applied to the original CDF files delivered by the EDI team
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Non-regularly spaced time-series! It contains quarter-spin, half-spin and spin resolution data with all qualities: GOOD/CAUTION/BAD. The values 2/1/0 for GOOD/CAUTION/BAD are written to Status[0]. Data from spin, half spin and quarter spin IFF files are merged by an algorithm that can be thought of as a 'use more if not lower quality' algorithm. The analysis is performed on each spin's worth of data starting with spin resolution. If there is more data of half spin resolution with equal or better quality, it replaces the spin resolution data. Likewise, if there is more data of quarter spin resolution with equal or better quality, it replaces the half spin resolution data. The electric field and drift velocity measurements are given in the inertial frame (a correction has been applied for the spacecraft velocity). DATASET VERSION HISTORY VERSION 01: The first version of this dataset was converted by the CAA from source CDF files provided by the EDI team. This conversion involved insertion of a half interval parameter that was not included in the source files and correction of missing or bad metadata. The half interval determination was based on comparison with the spin time-tags provided in the EDI CSDS Prime Parameter data file. In some cases a consistent determination could not be found with the PP data and the half-interval was set to the minimum, quarter spin, 1 second, value. CDF to CEF Conversion was done using revision 1.1 (2006/11/06) of edi_mp_convert.pro Metadata correction was done using revision 1.1 (2006/11/06) of edi_fix_fatal.sh FILE VERSION HISTORY For this initial conversion the CAA CEF files have retained the same file version number as the source CDF files. In most cases file versions are V13 or V14. VERSION 02: Minor changes
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Mixed time resolution: 1/8 s for normal and 1/64 s for burst mode MIN_TIME_RESOLUTION is set to fill_value MAX_TIME_RESOLUTION is given for BM Not regularly spaced timeline The background electron counts at fixed energy and pitch angle may be contaminated with beam electrons Status parameter has two bits for electron energy and acquisition time for the electron counts bit0=0: acquisition time=1/512 s; bit0=1: acq_time=1/1024 s bit1 is the energy flag=0/1 for 1/0.5 keV electron energy
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Spin resolution data with GOOD/CAUTION qualities. The values 2/1 for GOOD/CAUTION are in Status[0]. The electric field and drift velocity measurements are given in the inertial frame (a correction has been applied for the spacecraft velocity).
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
This dataset has been calculated using the following products: - C1_CP_FGM_5VPS - CL_SP_AUX - C1_CP_AUX_POSGSE_1M
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
Level 3 quantity P is the negative of the spacecraft potential, calculated by averaging the Level 2 quantity P over 4 seconds. For more information on data quality and how the CAA data are processed, please consult the EFW CAA Users Guide and the EFW CAA Interface Control Document (ICD). Detailed quality information is provided as a 16 bit set of flags in the parameter P_bitmask__C1_CP_EFW_L3_P. The meaning of the bits is as follows (LSB numbering starting at 0): Bit 0: Reset. Bit 1: Bad bias. Bit 2: Probe latchup. Bit 3: Low density saturation (-68V). Bits 4-12: N/A Bit 13: Whisper operating. Bit 14: Saturation due to high bias current. Bit 15: N/A
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
This dataset has been calculated using the following products: - C1_CP_FGM_5VPS - CL_SP_AUX - C1_CP_AUX_POSGSE_1M
Each Cluster spacecraft carries an identical FGM instrument (Fluxgate Magnetometer) to measure the DC magnetic field vector. Each instrument, in turn, consists of two triaxial fluxgate magnetometers and an onboard data processing unit. The instrument samples the magnetic field at a cadence of 22 Hz (67 Hz in Burst mode). In order to minimise the magnetic background of the spacecraft, one of the magnetometer sensors (the outboard, or OB sensor) is located at the end of one of the two 5 m radial booms of the spacecraft, the other (the inboard, or IB sensor) at 1.5 m inboard from the end of the boom. Since the start of the scientific operations on February 1, 2001, only the outboard sensor on each satellite has been used.
*C1_CQ_FGM_CAVF
No TEXT global attribute value.
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C1_CQ_RAP_CAVEATS *C1_CP_RAP_DSETTINGS
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C1_CQ_STA_CALIB_YTR_CAVEATS *C1_CQ_STA_NOTSRP_MTR_CAVEATS DATASET VERSION HISTORY Version 01: First version of dataset. Version 02: Few corrected re-deliveries. Version 03: Removal of on-board calibration records is now based on the calibration bit (instead of the step-in-cal character).
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C1_CQ_STA_SA_UNDEF_MFA_TR_CAVEATS *C1_CQ_STA_NOTSRP_MTR_CAVEATS *C1_CQ_STA_CALIB_YTR_CAVEATS DATASET VERSION HISTORY: Version 09 : Reprocessed due to FGM and/or SPD-AUX files re-deliveries. Version 08 : FGM induced gaps revised and completed. Version 07 : New calibration tables plus addition of the half-interval duration and status. Removal of onboard calibration data. Now with FGM induced gaps. FGM file used described in the FILE_CAVEATS metadata section. Warning to the users of versions lower than 07: Delta_plus of Time__C1_CP_STA_PPP variables was set to a fixed value instead of a value varying with the mode. This chosen fixed value is the minimum time resolution (4s) which is correct in most of the cases (Normal Bit Rate). Note that the data themselves are correct. The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Version 05: used the new calibration tables (feb 2013). Version 03: AUX files in CDF format used are 26 hours. Same data than version02 but less missing values. Version 02: Data format corrected. Version 01: Obsolete. Should not be used !
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C1_CQ_STA_SA_PSD_NEG_CAVEATS *C1_CQ_STA_NOTSRP_MTR_CAVEATS *C1_CQ_STA_CALIB_YTR_CAVEATS Version 07 : New calibration tables plus addition of the interval duration and status. Removal of onboard calibration data. Warning to the users of versions lower than 07: Delta_plus of Time__C1_CP_STA_PSD variables is set to a fixed value instead of a value varying with the mode. This chosen fixed value is the usual minimum time resolution (1s) which is correct in most of the time (Normal Bit Rate). The time resolution is better in High Bit Rate. Note that the data themselves are correct. Version 04 : All the headers have been updated (laboratory name and email). Introduction of a new header file (Dataset). The PSD negative values in the version 03 have been replaced by the fillvalue (-1.00E+31). Version 03: The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Phase rotation corrected + exhaustive data. Older versions are obsolete and should not be used ! The negative values must not be taken into account by the users. Version 02 : Obsolete. This version may be used if Version 03 is not available, as long as only total B and total E power are used ! Version 01 : Obsolete. Should not be used !
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C1_CQ_STA_NOTSRP_MTR_CAVEATS *C1_CQ_STA_CALIB_YTR_CAVEATS Version 07 : New calibration tables plus addition of the interval duration and status. Removal of onboard calibration data. Warning to the users of versions lower than 07: Delta_plus of Time__C1_CP_STA_SM variables is set to a fixed value instead of a value varying with the mode. This chosen fixed value is the minimum time resolution (4s) which is correct in most of the cases (Normal Bit Rate) Note that the data themselves are correct. Version 04 : All the headers have been updated (laboratory name and email). Introduction of a new header file (Dataset). Units and Si Conversion of the variables BB and BE have been corrected. Version 03 : Phase rotation corrected + exhaustive data. The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Older versions are obsolete and should not be used ! Version 02 : Obsolete. Should not be used ! Version 01 : Obsolete. Should not be used !
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: dataset headers update, QUALITY changed to CONTRAST, addition of a new QUALITY variable VERSION 03: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 04: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: dataset headers update VERSION 03: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 04: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation used to calculate magnetic field and L value in PMP files produced after 23 Feb 2020.
JSOC predicted magnetic positions.
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997) AP _ Apogee CY 1 Start of visibility window at Canberra (5 deg elevation) CY 2 Start of visibility window at Canberra (5 deg elevation) CY 3 Start of visibility window at Canberra (5 deg elevation) CZ 1 End of visibility window at Canberra (5 deg elevation) CZ 2 End of visibility window at Canberra (5 deg elevation) CZ 3 End of visibility window at Canberra (5 deg elevation) CZ 4 End of visibility window at Canberra (5 deg elevation) DY 1 Start of visibility window at Vilspa (5 deg elevation) DY 2 Start of visibility window at Vilspa (5 deg elevation) DY 3 Start of visibility window at Vilspa (5 deg elevation) DY 4 Start of visibility window at Vilspa (5 deg elevation) DY 5 Start of visibility window at Vilspa (5 deg elevation) DZ 1 End of visibility window at Vilspa (5 deg elevation) DZ 2 End of visibility window at Vilspa (5 deg elevation) DZ 3 End of visibility window at Vilspa (5 deg elevation) DZ 4 End of visibility window at Vilspa (5 deg elevation) GY 1 Start of visibility window at Goldstone (5 deg elevation) GY 2 Start of visibility window at Goldstone (5 deg elevation) GY 3 Start of visibility window at Goldstone (5 deg elevation) GY 4 Start of visibility window at Goldstone (5 deg elevation) GZ 1 End of visibility window at Goldstone (5 deg elevation) GZ 2 End of visibility window at Goldstone (5 deg elevation) GZ 3 End of visibility window at Goldstone (5 deg elevation) JY 1 Start of visibility window at Maspalomas (5 deg elevation) JY 2 Start of visibility window at Maspalomas (5 deg elevation) JY 3 Start of visibility window at Maspalomas (5 deg elevation) JY 4 Start of visibility window at Maspalomas (5 deg elevation) JZ 1 End of visibility window at Maspalomas (5 deg elevation) JZ 2 End of visibility window at Maspalomas (5 deg elevation) JZ 3 End of visibility window at Maspalomas (5 deg elevation) KA 1 Start of visibility window at Kourou (5 deg elevation) KA 2 Start of visibility window at Kourou (5 deg elevation) KA 3 Start of visibility window at Kourou (5 deg elevation) KA 4 Start of visibility window at Kourou (5 deg elevation) KL 1 End of visibility window at Kourou (5 deg elevation) KL 2 End of visibility window at Kourou (5 deg elevation) KL 3 End of visibility window at Kourou (5 deg elevation) KL 4 End of visibility window at Kourou (5 deg elevation) MY 1 Start of visibility window at Madrid (5 deg elevation) MY 2 Start of visibility window at Madrid (5 deg elevation) MY 3 Start of visibility window at Madrid (5 deg elevation) MY 4 Start of visibility window at Madrid (5 deg elevation) MZ 1 End of visibility window at Madrid (5 deg elevation) MZ 2 End of visibility window at Madrid (5 deg elevation) MZ 3 End of visibility window at Madrid (5 deg elevation) NS S Southbound neutral sheet NT I Enter north tail lobe from inner magnetosphere PA 1 Start of visibility window at Perth (5 deg elevation) PA 2 Start of visibility window at Perth (5 deg elevation) PA 3 Start of visibility window at Perth (5 deg elevation) PA 4 Start of visibility window at Perth (5 deg elevation) PE _ Perigee PL 1 End of visibility window at Perth (5 deg elevation) PL 2 End of visibility window at Perth (5 deg elevation) PL 3 End of visibility window at Perth (5 deg elevation) PL 4 End of visibility window at Perth (5 deg elevation) PL 5 End of visibility window at Perth (5 deg elevation) QL I Inbound critical L value for auroral zone QL O Outbound critical L value for auroral zone RA 1 Start of visibility window at Redu (5 deg elevation) RA 2 Start of visibility window at Redu (5 deg elevation) RA 3 Start of visibility window at Redu (5 deg elevation) RA 4 Start of visibility window at Redu (5 deg elevation) RL 1 End of visibility window at Redu (5 deg elevation) RL 2 End of visibility window at Redu (5 deg elevation) RL 3 End of visibility window at Redu (5 deg elevation) RL 4 End of visibility window at Redu (5 deg elevation) RL 5 End of visibility window at Redu (5 deg elevation) ST O Leave south tail lobe for inner magnetosphere TL I Inbound radiation belt entry for WEC TL O Outbound radiation belt exit for WEC VL I Inbound critical L value for EDI VL O Outbound critical L value for EDI XL I Inbound critical L value for PEACE XL O Outbound critical L value for PEACE YL I Inbound critical L value for RAPID YL O Outbound critical L value for RAPID ZL I Inbound critical L value for CIS ZL O Outbound critical L value for CIS
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation pole used to calculate GSM latitude and MLT in PSE files produced after 23 Feb 2020. PSE files updated to support orbits >999 and six decimal figures on orbit phase from 25 March 2006.
JSOC predicted scientific events.
K. Torkar et al, Active spacecraft potential control for Cluster - implementation and first results Ann. Geophys., 19, pp 1289 - 1302, 2001)
none Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
H. Reme et al, First multispacecraft ion measurements in and near the Earth's magnetosphere with the identical Cluster Ion Spectrometry (CIS) experiment Annales Geophysicae, 19, pp 1303 - 1354, 2001
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C1_PP_CIS_20220930 pre-validated by CIS team and supplied to UKCDC for inges The user of the CIS data needs to be cautious. Please refer to the CIS Home Page: http://cluster.irap.omp.eu/index.php?page=caveats , link [Caveats for specific data intervals], for caveats concerning these data.
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster Space Sci. Rev., 79, pp 209 - 231, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C1_PP_DWP_20220702 HAS NOT BEEN VALIDATED - USE WITH CAUTION *** This CSDS DWP product has not been validated prior to release.
G. Paschmann et al, The Electron Drift Instrument for Cluster Space Sci. Rev., 79, pp 233 - 269, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats 1) EDI's automated analysis algorithm has a known susceptibility to producing occasional incorrect values of the drift velocities (and electric fields). The code attempts to prevent these bad values to be output to the cdf file. No further removal is done in the validation process. 2) When drift velocities become sufficiently large, there can be a 180-degree ambiguity in drift direction that is usually flagged in bit 7 (counting from 0) of Status Byte 3. 3) There are two methods to analyze a spin's worth of EDI data. If bits 5 & 6 in Status Byte 3 are NOT set, the employed method was triangulation. If either bit 5 or 6 are set, then the results are from time-of-flight analysis. 4) The reported drift velocities and electric field refer to inertial coordinates, i.e., have been corrected for spacecraft velocity. However, the magnitude errors (in %) and the angle errors (in degrees), reported in Status Bytes 5 & 6, respectively, refer to the spacecraft frame and have NOT yet been converted to inertial coordinates. 5) The reduced chi-square reported as a data word is a measure of the goodness-of-fit of the triangulation analysis.
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster Space Sci. Rev., 79, pp 137 - 156, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data calibration may be unreliable at this early stage of the mission
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CSDS data are not for publication *** Be aware that data may be reprocessed as necessary to improve quality For questions on data validity please contact sdc-adm@plasma.kth.se Fill value inserted for E_dusk__C1_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z Fill value inserted for E_pow_f1__C1_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z Fill value inserted for E_sigma__C1_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z Fill value inserted for U_probe_sc__C1_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment Space Sci. Rev., 79, pp 351 - 398, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 PP & SP data is generated at MSSL, then provided to UK-CDHF
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats This is PEACE PP/SP data version 3.1, produced at MSSL Based on onboard moments but using corrected geometric factors which account for uplinked changes of the values used in onboard calibration as well as estimated changes due to variable MCP gain performance Onboard moments are calculated for up to three energy ranges. Photoelectron contamination may affect 0, 1 or 2 of these ranges EFW PP probe-spacecraft potential was used to select the energy ranges to be excluded to remove misleading photoelectron contributions. Note that the density may be underestimated if there are both plasma electrons and photoelectrons in the lowest energy range When 88h58 is used for the HEEA sensor, sometimes the entire plasma electron population and photoelectrons are in just the lowest of the 3 energy ranges. This data has been deleted in this release of the PEACE PPs Data is deleted if the spacecraft electric potential is too large for the simple correction procedure to work or there is no EFW PP data available Measured electron energies have not been corrected for their acceleration by the spacecraft electric potential Onboard moments use onboard energy tables, efficiencies and response surfaces. Any errors in these parameters cannot be corrected in ground data processing Before 2001-09-11 the onboard energy efficiencies were not accurate, which caused the density in the solar wind to be overestimated. This data has been removed in this release of the PEACE PPs The calculation of T_par, T_perp and Q_par used PP FGM data The data is for context and information only. It is not suitable for detailed analysis, but may be used for event selection The next iteration of PP/SP moments will be of a higher quality Please see links under http://www.mssl.ucl.ac.uk/www_plasma/missions/cluster/clusterII.html for more information Please contact the PEACE PI to request science quality data Automatically validated by UKCDC Product delivered pre-validated by the PI institute
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster Space Sci. Rev., 79, pp 399 - 473, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data processed on 2024-10-18T10:59:07Z Caveats file: RAP_CAV_C1_V245.DAT; Release Sep 16, 2024
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats 2023-09-19T00:00:00.000Z/9999-12-31T23:59:59.000Z: RAPID permanently turned off as of Sep 19, 2023. Corrected time stamps for ions and electrons. Energy threshold shifts have been applied.
N. Cornilleau et al, The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment Space Sci. Rev., 79, pp 107 - 136, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats PI Software Version 4.2, 25 September 2006
P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser: Performances and Perspectives for the Cluster Mission Space Sci. Rev., 79, pp 157 - 193, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Two types of parameters are provided by WHISPER: 1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding operations. The N_e_res value is calculated from an algorithm for resonance recognition, which cannot take account of all level of information available to the experimenter. The reliability of N_e_res parameters derived at the CSDS level is thus limited in an unknown manner. The N_e_res_q parameter (one value for each N_e_res data point) provides a crude idea of the probability that the N_e_res value is actually correct. A value of 0 means that the value is probably wrong, a value above 80 that it is probably correct. Anything in between reflects a crude evaluation of the chances. Refer to PI for details. 2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are related to recording of natural wave emissions. Those parameters, not affected by variations in instrument's transfer functions, are globally OK. However, two factors can affect the precision of the measurements: a) the occasional presence of spurious emissions created by operations of the EDI instrument increases the wave power values measured on SC1, SC2 and SC3, from an unknown amount, b) the limited dynamical range of the instrument leads to an underestimation of the E_pow parameters values when the voltage difference measured by the double sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp (depending of the gain chosen). As a consequence, high values have to be taken with special caution.
A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C1_UP_FGM_20230830 HAS NOT BEEN VALIDATED - USE WITH CAUTION *** For the extended mission (starting 1/1/2006) CSDS FGM products are not validated prior to release to the science community. Spikes and other artefacts that were previously removed during validation of the FGM PP/SP data may occur in these files.
High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'cluster_wbd_calibration.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data by 1000 to get V m^-1; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. ... Bandwidth Sample Rate --------- ------------ 9.5 kHz 27.443 kHz 19 kHz 54.886 kHz 77 kHz 219.544 kHz ... COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. ...
Created Mar 2008.Revised Dec 2008, Jan 2010
WARNING: 19 and 77 kHz Bandwidth modes with 8-bit resolution, and 77 kHz Bandwidth mode with 4-bit resolution (see Resolution variable) are not continuous data modes. Always check for periodic time jumps for these modes.
Also known as Conversion Frequency.
Steps of 5 dB from 0 to 75.
Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between the Xgse axis and the antenna direction. Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between Ygse axis and the projection of the antenna direction in the Ygse-Zgse plane, measured counter-clockwise from +Ygse (angle=0 deg) to +Zgse (angle=90 deg), -Ygse (angle=180 deg) and -Zgse (angle=270 deg). Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
DC Offset values may be used to reverse calibrate the data to the original raw counts and to determine the boundaries of the original transport packets. A description of the procedure may be found in the 'cluster_wbd_calibration.pdf' document (see Global attributes section of this file). In addition, sample code for reverse calibration may be found in the above mentioned document.
WARNING: If Translation is not equal to 0, this variable represents the electric field amplitude associated with the down-converted waveform. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.
Clipped data: Measurement was equal to raw data value maximum (255) or minimum (0). This does not necessarily mean the receiver was in saturation, which would be accompanied by non-linear effects.
High time resolution calibrated waveform data sampled in one of 3 frequency bandwidths in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'CAA_EST_CR_WBD_v20.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, see 'CAA_EST_CR_WBD_v20.pdf'. The steps for converting are briefly outlined below: 1) If Electric Field, first divide calibrated data by 1000 to get V m^-1; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth VAR_NOTES for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table in VAR_NOTES of the 'BM_Mode' variable for the appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any;7) if Translation is not equal to 0, add the appropriate translation frequency to each frequency component (see Translation CATDESC for the exact values). ... COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. ...
Created Nov 2014.
WARNING: Burst Modes 0 through 5 are not continuous data modes (see 'BM_Mode' variable). Always check for periodic time jumps for these modes.Values for Bandwidth are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Also known as Conversion Frequency.WARNING: If this variable is not equal to 0, the electric field waveform (WBD_Elec vs. Epoch variables) is the product of a down-conversion to 0.0 kHz which took place onboard within the WBD instrument. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.Values for Translation are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Values for ANTENNA are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Steps of 5 dB from 0 to 75.Values for Gain are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between the Xgse axis and the antenna direction. Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between Ygse axis and the projection of the antenna direction in the Ygse-Zgse plane, measured counter-clockwise from +Ygse (angle=0 deg) to +Zgse (angle=90 deg), -Ygse (angle=180 deg) and -Zgse (angle=270 deg). Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
DC Offset values may be used to reverse calibrate the data to the original raw counts and to determine the boundaries of the original transport packets. A description of the procedure may be found in the WBD calibration report 'CAA_EST_CR_WBD_v20.pdf' (see Global attributes section of this file). In addition, sample code for reverse calibration may be found in the above mentioned document.
WARNING: If Translation is not equal to 0, this variable represents the electric field amplitude associated with the down-converted waveform. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.
Clipped data: Measurement was equal to raw data value maximum (255) or minimum (0). This does not necessarily mean the receiver was in saturation, which would be accompanied by non-linear effects.
The following are the sampling rates for each of the 10 defined modes: Bandwidth Burst Mode Sample Rate --------- ---------- ------------ 9.5 kHz 0, 1 27.443 kHz19.0 kHz 2, 3 54.886 kHz77.0 kHz 4, 5 219.544 kHz 9.5 kHz 6, 7 9.148 kHz 9.5 kHz 8, 9 6.861 kHz
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Mixed time resolution: 1/16 s for normal and 1/128 s for burst mode The AEC (*.edi_ae_cor) files were used to correct for angular (theta-phi) dependence of the efficieny The correction is applied to the original CDF files delivered by the EDI team
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Non-regularly spaced time-series! It contains quarter-spin, half-spin and spin resolution data with all qualities: GOOD/CAUTION/BAD. The values 2/1/0 for GOOD/CAUTION/BAD are written to Status[0]. Data from spin, half spin and quarter spin IFF files are merged by an algorithm that can be thought of as a 'use more if not lower quality' algorithm. The analysis is performed on each spin's worth of data starting with spin resolution. If there is more data of half spin resolution with equal or better quality, it replaces the spin resolution data. Likewise, if there is more data of quarter spin resolution with equal or better quality, it replaces the half spin resolution data. The electric field and drift velocity measurements are given in the inertial frame (a correction has been applied for the spacecraft velocity). DATASET VERSION HISTORY VERSION 01: The first version of this dataset was converted by the CAA from source CDF files provided by the EDI team. This conversion involved insertion of a half interval parameter that was not included in the source files and correction of missing or bad metadata. The half interval determination was based on comparison with the spin time-tags provided in the EDI CSDS Prime Parameter data file. In some cases a consistent determination could not be found with the PP data and the half-interval was set to the minimum, quarter spin, 1 second, value. CDF to CEF Conversion was done using revision 1.1 (2006/11/06) of edi_mp_convert.pro Metadata correction was done using revision 1.1 (2006/11/06) of edi_fix_fatal.sh FILE VERSION HISTORY For this initial conversion the CAA CEF files have retained the same file version number as the source CDF files. In most cases file versions are V13 or V14. VERSION 02: Minor changes
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Mixed time resolution: 1/8 s for normal and 1/64 s for burst mode MIN_TIME_RESOLUTION is set to fill_value MAX_TIME_RESOLUTION is given for BM Not regularly spaced timeline The background electron counts at fixed energy and pitch angle may be contaminated with beam electrons Status parameter has two bits for electron energy and acquisition time for the electron counts bit0=0: acquisition time=1/512 s; bit0=1: acq_time=1/1024 s bit1 is the energy flag=0/1 for 1/0.5 keV electron energy
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Spin resolution data with GOOD/CAUTION qualities. The values 2/1 for GOOD/CAUTION are in Status[0]. The electric field and drift velocity measurements are given in the inertial frame (a correction has been applied for the spacecraft velocity).
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
This dataset has been calculated using the following products: - C2_CP_FGM_5VPS - CL_SP_AUX - C2_CP_AUX_POSGSE_1M
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
Level 3 quantity P is the negative of the spacecraft potential, calculated by averaging the Level 2 quantity P over 4 seconds. For more information on data quality and how the CAA data are processed, please consult the EFW CAA Users Guide and the EFW CAA Interface Control Document (ICD). Detailed quality information is provided as a 16 bit set of flags in the parameter P_bitmask__C2_CP_EFW_L3_P. The meaning of the bits is as follows (LSB numbering starting at 0): Bit 0: Reset. Bit 1: Bad bias. Bit 2: Probe latchup. Bit 3: Low density saturation (-68V). Bits 4-12: N/A Bit 13: Whisper operating. Bit 14: Saturation due to high bias current. Bit 15: N/A
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
This dataset has been calculated using the following products: - C2_CP_FGM_5VPS - CL_SP_AUX - C2_CP_AUX_POSGSE_1M
Each Cluster spacecraft carries an identical FGM instrument (Fluxgate Magnetometer) to measure the DC magnetic field vector. Each instrument, in turn, consists of two triaxial fluxgate magnetometers and an onboard data processing unit. The instrument samples the magnetic field at a cadence of 22 Hz (67 Hz in Burst mode). In order to minimise the magnetic background of the spacecraft, one of the magnetometer sensors (the outboard, or OB sensor) is located at the end of one of the two 5 m radial booms of the spacecraft, the other (the inboard, or IB sensor) at 1.5 m inboard from the end of the boom. Since the start of the scientific operations on February 1, 2001, only the outboard sensor on each satellite has been used.
*C2_CQ_FGM_CAVF
No TEXT global attribute value.
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C2_CQ_RAP_CAVEATS *C2_CP_RAP_DSETTINGS
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C2_CQ_STA_CALIB_YTR_CAVEATS *C2_CQ_STA_NOTSRP_MTR_CAVEATS DATASET VERSION HISTORY Version 01: First version of dataset. Version 02: Few corrected re-deliveries. Version 03: Removal of on-board calibration records is now based on the calibration bit (instead of the step-in-cal character).
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C2_CQ_STA_SA_UNDEF_MFA_TR_CAVEATS *C2_CQ_STA_NOTSRP_MTR_CAVEATS *C2_CQ_STA_CALIB_YTR_CAVEATS DATASET VERSION HISTORY: Version 09 : Reprocessed due to FGM and/or SPD-AUX files re-deliveries. Version 08 : FGM induced gaps revised and completed. Version 07 : New calibration tables plus addition of the half-interval duration and status. Removal of onboard calibration data. Now with FGM induced gaps. FGM file used described in the FILE_CAVEATS metadata section. Warning to the users of versions lower than 07: Delta_plus of Time__C2_CP_STA_PPP variables was set to a fixed value instead of a value varying with the mode. This chosen fixed value is the minimum time resolution (4s) which is correct in most of the cases (Normal Bit Rate). Note that the data themselves are correct. The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Version 05: used the new calibration tables (feb 2013). Version 03: AUX files in CDF format used are 26 hours. Same data than version02 but less missing values. Version 02: Data format corrected. Version 01: Obsolete. Should not be used !
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C2_CQ_STA_SA_PSD_NEG_CAVEATS *C2_CQ_STA_NOTSRP_MTR_CAVEATS *C2_CQ_STA_CALIB_YTR_CAVEATS Version 07 : New calibration tables plus addition of the interval duration and status. Removal of onboard calibration data. Warning to the users of versions lower than 07: Delta_plus of Time__C2_CP_STA_PSD variables is set to a fixed value instead of a value varying with the mode. This chosen fixed value is the usual minimum time resolution (1s) which is correct in most of the time (Normal Bit Rate). The time resolution is better in High Bit Rate. Note that the data themselves are correct. Version 04 : All the headers have been updated (laboratory name and email). Introduction of a new header file (Dataset). The PSD negative values in the version 03 have been replaced by the fillvalue (-1.00E+31). Version 03: The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Phase rotation corrected + exhaustive data. Older versions are obsolete and should not be used ! The negative values must not be taken into account by the users. Version 02 : Obsolete. This version may be used if Version 03 is not available, as long as only total B and total E power are used ! Version 01 : Obsolete. Should not be used !
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C2_CQ_STA_NOTSRP_MTR_CAVEATS *C2_CQ_STA_CALIB_YTR_CAVEATS Version 07 : New calibration tables plus addition of the interval duration and status. Removal of onboard calibration data. Warning to the users of versions lower than 07: Delta_plus of Time__C2_CP_STA_SM variables is set to a fixed value instead of a value varying with the mode. This chosen fixed value is the minimum time resolution (4s) which is correct in most of the cases (Normal Bit Rate) Note that the data themselves are correct. Version 04 : All the headers have been updated (laboratory name and email). Introduction of a new header file (Dataset). Units and Si Conversion of the variables BB and BE have been corrected. Version 03 : Phase rotation corrected + exhaustive data. The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Older versions are obsolete and should not be used ! Version 02 : Obsolete. Should not be used ! Version 01 : Obsolete. Should not be used !
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: dataset headers update, QUALITY changed to CONTRAST, addition of a new QUALITY variable VERSION 03: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 04: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: dataset headers update VERSION 03: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 04: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation used to calculate magnetic field and L value in PMP files produced after 23 Feb 2020.
JSOC predicted magnetic positions.
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997) AP _ Apogee CY 1 Start of visibility window at Canberra (5 deg elevation) CY 2 Start of visibility window at Canberra (5 deg elevation) CY 3 Start of visibility window at Canberra (5 deg elevation) CZ 1 End of visibility window at Canberra (5 deg elevation) CZ 2 End of visibility window at Canberra (5 deg elevation) CZ 3 End of visibility window at Canberra (5 deg elevation) CZ 4 End of visibility window at Canberra (5 deg elevation) DY 1 Start of visibility window at Vilspa (5 deg elevation) DY 2 Start of visibility window at Vilspa (5 deg elevation) DY 3 Start of visibility window at Vilspa (5 deg elevation) DY 4 Start of visibility window at Vilspa (5 deg elevation) DZ 1 End of visibility window at Vilspa (5 deg elevation) DZ 2 End of visibility window at Vilspa (5 deg elevation) DZ 3 End of visibility window at Vilspa (5 deg elevation) GY 1 Start of visibility window at Goldstone (5 deg elevation) GY 2 Start of visibility window at Goldstone (5 deg elevation) GY 3 Start of visibility window at Goldstone (5 deg elevation) GY 4 Start of visibility window at Goldstone (5 deg elevation) GZ 1 End of visibility window at Goldstone (5 deg elevation) GZ 2 End of visibility window at Goldstone (5 deg elevation) GZ 3 End of visibility window at Goldstone (5 deg elevation) JY 1 Start of visibility window at Maspalomas (5 deg elevation) JY 2 Start of visibility window at Maspalomas (5 deg elevation) JY 3 Start of visibility window at Maspalomas (5 deg elevation) JY 4 Start of visibility window at Maspalomas (5 deg elevation) JZ 1 End of visibility window at Maspalomas (5 deg elevation) JZ 2 End of visibility window at Maspalomas (5 deg elevation) JZ 3 End of visibility window at Maspalomas (5 deg elevation) KA 1 Start of visibility window at Kourou (5 deg elevation) KA 2 Start of visibility window at Kourou (5 deg elevation) KA 3 Start of visibility window at Kourou (5 deg elevation) KA 4 Start of visibility window at Kourou (5 deg elevation) KL 1 End of visibility window at Kourou (5 deg elevation) KL 2 End of visibility window at Kourou (5 deg elevation) KL 3 End of visibility window at Kourou (5 deg elevation) KL 4 End of visibility window at Kourou (5 deg elevation) MY 1 Start of visibility window at Madrid (5 deg elevation) MY 2 Start of visibility window at Madrid (5 deg elevation) MY 3 Start of visibility window at Madrid (5 deg elevation) MY 4 Start of visibility window at Madrid (5 deg elevation) MZ 1 End of visibility window at Madrid (5 deg elevation) MZ 2 End of visibility window at Madrid (5 deg elevation) MZ 3 End of visibility window at Madrid (5 deg elevation) NS S Southbound neutral sheet NT I Enter north tail lobe from inner magnetosphere PA 1 Start of visibility window at Perth (5 deg elevation) PA 2 Start of visibility window at Perth (5 deg elevation) PA 3 Start of visibility window at Perth (5 deg elevation) PE _ Perigee PL 1 End of visibility window at Perth (5 deg elevation) PL 2 End of visibility window at Perth (5 deg elevation) PL 3 End of visibility window at Perth (5 deg elevation) PL 4 End of visibility window at Perth (5 deg elevation) QL I Inbound critical L value for auroral zone QL O Outbound critical L value for auroral zone RA 1 Start of visibility window at Redu (5 deg elevation) RA 2 Start of visibility window at Redu (5 deg elevation) RA 3 Start of visibility window at Redu (5 deg elevation) RA 4 Start of visibility window at Redu (5 deg elevation) RL 1 End of visibility window at Redu (5 deg elevation) RL 2 End of visibility window at Redu (5 deg elevation) RL 3 End of visibility window at Redu (5 deg elevation) RL 4 End of visibility window at Redu (5 deg elevation) ST O Leave south tail lobe for inner magnetosphere TL I Inbound radiation belt entry for WEC TL O Outbound radiation belt exit for WEC VL I Inbound critical L value for EDI VL O Outbound critical L value for EDI WL I Inbound critical L value for ASPOC WL O Outbound critical L value for ASPOC XL I Inbound critical L value for PEACE XL O Outbound critical L value for PEACE YL I Inbound critical L value for RAPID YL O Outbound critical L value for RAPID ZL I Inbound critical L value for CIS ZL O Outbound critical L value for CIS
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation pole used to calculate GSM latitude and MLT in PSE files produced after 23 Feb 2020. PSE files updated to support orbits >999 and six decimal figures on orbit phase from 25 March 2006.
JSOC predicted scientific events.
K. Torkar et al, Active spacecraft potential control for Cluster - implementation and first results Ann. Geophys., 19, pp 1289 - 1302, 2001)
none Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats One raw data format (5.1.5 secs) of bad data may occur when the instrument is powered on.
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster Space Sci. Rev., 79, pp 209 - 231, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C2_PP_DWP_20220702 HAS NOT BEEN VALIDATED - USE WITH CAUTION *** This CSDS DWP product has not been validated prior to release.
G. Paschmann et al, The Electron Drift Instrument for Cluster Space Sci. Rev., 79, pp 233 - 269, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats The guns are switched off since 2004/04/10 because of strong interferences with WHISPER. Only Ambient Electron data have been measured
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster Space Sci. Rev., 79, pp 137 - 156, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data calibration may be unreliable at this early stage of the mission
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CSDS data are not for publication *** Be aware that data may be reprocessed as necessary to improve quality For questions on data validity please contact sdc-adm@plasma.kth.se Fill value inserted for E_dusk__C2_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z Fill value inserted for E_pow_f1__C2_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z Fill value inserted for E_sigma__C2_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z Fill value inserted for U_probe_sc__C2_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment Space Sci. Rev., 79, pp 351 - 398, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 PP & SP data is generated at MSSL, then provided to UK-CDHF
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats This is PEACE PP/SP data version 3.1, produced at MSSL Based on onboard moments but using corrected geometric factors which account for uplinked changes of the values used in onboard calibration as well as estimated changes due to variable MCP gain performance Onboard moments are calculated for up to three energy ranges. Photoelectron contamination may affect 0, 1 or 2 of these ranges EFW PP probe-spacecraft potential was used to select the energy ranges to be excluded to remove misleading photoelectron contributions. Note that the density may be underestimated if there are both plasma electrons and photoelectrons in the lowest energy range When 88h58 is used for the HEEA sensor, sometimes the entire plasma electron population and photoelectrons are in just the lowest of the 3 energy ranges. This data has been deleted in this release of the PEACE PPs Data is deleted if the spacecraft electric potential is too large for the simple correction procedure to work or there is no EFW PP data available Measured electron energies have not been corrected for their acceleration by the spacecraft electric potential Onboard moments use onboard energy tables, efficiencies and response surfaces. Any errors in these parameters cannot be corrected in ground data processing Before 2001-09-11 the onboard energy efficiencies were not accurate, which caused the density in the solar wind to be overestimated. This data has been removed in this release of the PEACE PPs The calculation of T_par, T_perp and Q_par used PP FGM data The data is for context and information only. It is not suitable for detailed analysis, but may be used for event selection The next iteration of PP/SP moments will be of a higher quality Please see links under http://www.mssl.ucl.ac.uk/www_plasma/missions/cluster/clusterII.html for more information Please contact the PEACE PI to request science quality data Automatically validated by UKCDC Product delivered pre-validated by the PI institute
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster Space Sci. Rev., 79, pp 399 - 473, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data processed on 2024-10-18T10:59:07Z Caveats file: RAP_CAV_C2_V245.DAT; Release Sep 16, 2024
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats 2024-02-01T03:57:00.000Z/9999-12-31T23:59:59.000Z: RAPID permanently turned off as of Feb 1, 2024 Corrected time stamps for ions and electrons. Energy threshold shifts have been applied.
N. Cornilleau et al, The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment Space Sci. Rev., 79, pp 107 - 136, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats PI Software Version 4.2, 25 September 2006
P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser: Performances and Perspectives for the Cluster Mission Space Sci. Rev., 79, pp 157 - 193, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Two types of parameters are provided by WHISPER: 1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding operations. The N_e_res value is calculated from an algorithm for resonance recognition, which cannot take account of all level of information available to the experimenter. The reliability of N_e_res parameters derived at the CSDS level is thus limited in an unknown manner. The N_e_res_q parameter (one value for each N_e_res data point) provides a crude idea of the probability that the N_e_res value is actually correct. A value of 0 means that the value is probably wrong, a value above 80 that it is probably correct. Anything in between reflects a crude evaluation of the chances. Refer to PI for details. 2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are related to recording of natural wave emissions. Those parameters, not affected by variations in instrument's transfer functions, are globally OK. However, two factors can affect the precision of the measurements: a) the occasional presence of spurious emissions created by operations of the EDI instrument increases the wave power values measured on SC1, SC2 and SC3, from an unknown amount, b) the limited dynamical range of the instrument leads to an underestimation of the E_pow parameters values when the voltage difference measured by the double sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp (depending of the gain chosen). As a consequence, high values have to be taken with special caution.
A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C2_UP_FGM_20230830 HAS NOT BEEN VALIDATED - USE WITH CAUTION *** For the extended mission (starting 1/1/2006) CSDS FGM products are not validated prior to release to the science community. Spikes and other artefacts that were previously removed during validation of the FGM PP/SP data may occur in these files.
High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'cluster_wbd_calibration.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data by 1000 to get V m^-1; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. ... Bandwidth Sample Rate --------- ------------ 9.5 kHz 27.443 kHz 19 kHz 54.886 kHz 77 kHz 219.544 kHz ... COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. ...
Created Mar 2008.Revised Dec 2008, Jan 2010
WARNING: 19 and 77 kHz Bandwidth modes with 8-bit resolution, and 77 kHz Bandwidth mode with 4-bit resolution (see Resolution variable) are not continuous data modes. Always check for periodic time jumps for these modes.
Also known as Conversion Frequency.
Steps of 5 dB from 0 to 75.
Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between the Xgse axis and the antenna direction. Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between Ygse axis and the projection of the antenna direction in the Ygse-Zgse plane, measured counter-clockwise from +Ygse (angle=0 deg) to +Zgse (angle=90 deg), -Ygse (angle=180 deg) and -Zgse (angle=270 deg). Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
DC Offset values may be used to reverse calibrate the data to the original raw counts and to determine the boundaries of the original transport packets. A description of the procedure may be found in the 'cluster_wbd_calibration.pdf' document (see Global attributes section of this file). In addition, sample code for reverse calibration may be found in the above mentioned document.
WARNING: If Translation is not equal to 0, this variable represents the electric field amplitude associated with the down-converted waveform. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.
Clipped data: Measurement was equal to raw data value maximum (255) or minimum (0). This does not necessarily mean the receiver was in saturation, which would be accompanied by non-linear effects.
High time resolution calibrated waveform data sampled in one of 3 frequency bandwidths in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'CAA_EST_CR_WBD_v20.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, see 'CAA_EST_CR_WBD_v20.pdf'. The steps for converting are briefly outlined below: 1) If Electric Field, first divide calibrated data by 1000 to get V m^-1; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth VAR_NOTES for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table in VAR_NOTES of the 'BM_Mode' variable for the appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any;7) if Translation is not equal to 0, add the appropriate translation frequency to each frequency component (see Translation CATDESC for the exact values). ... COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. ...
Created Nov 2014.
WARNING: Burst Modes 0 through 5 are not continuous data modes (see 'BM_Mode' variable). Always check for periodic time jumps for these modes.Values for Bandwidth are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Also known as Conversion Frequency.WARNING: If this variable is not equal to 0, the electric field waveform (WBD_Elec vs. Epoch variables) is the product of a down-conversion to 0.0 kHz which took place onboard within the WBD instrument. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.Values for Translation are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Values for ANTENNA are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Steps of 5 dB from 0 to 75.Values for Gain are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between the Xgse axis and the antenna direction. Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between Ygse axis and the projection of the antenna direction in the Ygse-Zgse plane, measured counter-clockwise from +Ygse (angle=0 deg) to +Zgse (angle=90 deg), -Ygse (angle=180 deg) and -Zgse (angle=270 deg). Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
DC Offset values may be used to reverse calibrate the data to the original raw counts and to determine the boundaries of the original transport packets. A description of the procedure may be found in the WBD calibration report 'CAA_EST_CR_WBD_v20.pdf' (see Global attributes section of this file). In addition, sample code for reverse calibration may be found in the above mentioned document.
WARNING: If Translation is not equal to 0, this variable represents the electric field amplitude associated with the down-converted waveform. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.
Clipped data: Measurement was equal to raw data value maximum (255) or minimum (0). This does not necessarily mean the receiver was in saturation, which would be accompanied by non-linear effects.
The following are the sampling rates for each of the 10 defined modes: Bandwidth Burst Mode Sample Rate --------- ---------- ------------ 9.5 kHz 0, 1 27.443 kHz19.0 kHz 2, 3 54.886 kHz77.0 kHz 4, 5 219.544 kHz 9.5 kHz 6, 7 9.148 kHz 9.5 kHz 8, 9 6.861 kHz
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C3_CQ_CIS-HIA_CAVEATS
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Mixed time resolution: 1/16 s for normal and 1/128 s for burst mode The AEC (*.edi_ae_cor) files were used to correct for angular (theta-phi) dependence of the efficieny The correction is applied to the original CDF files delivered by the EDI team
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Non-regularly spaced time-series! It contains quarter-spin, half-spin and spin resolution data with all qualities: GOOD/CAUTION/BAD. The values 2/1/0 for GOOD/CAUTION/BAD are written to Status[0]. Data from spin, half spin and quarter spin IFF files are merged by an algorithm that can be thought of as a 'use more if not lower quality' algorithm. The analysis is performed on each spin's worth of data starting with spin resolution. If there is more data of half spin resolution with equal or better quality, it replaces the spin resolution data. Likewise, if there is more data of quarter spin resolution with equal or better quality, it replaces the half spin resolution data. The electric field and drift velocity measurements are given in the inertial frame (a correction has been applied for the spacecraft velocity). DATASET VERSION HISTORY VERSION 01: The first version of this dataset was converted by the CAA from source CDF files provided by the EDI team. This conversion involved insertion of a half interval parameter that was not included in the source files and correction of missing or bad metadata. The half interval determination was based on comparison with the spin time-tags provided in the EDI CSDS Prime Parameter data file. In some cases a consistent determination could not be found with the PP data and the half-interval was set to the minimum, quarter spin, 1 second, value. CDF to CEF Conversion was done using revision 1.1 (2006/11/06) of edi_mp_convert.pro Metadata correction was done using revision 1.1 (2006/11/06) of edi_fix_fatal.sh FILE VERSION HISTORY For this initial conversion the CAA CEF files have retained the same file version number as the source CDF files. In most cases file versions are V13 or V14. VERSION 02: Minor changes
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Mixed time resolution: 1/8 s for normal and 1/64 s for burst mode MIN_TIME_RESOLUTION is set to fill_value MAX_TIME_RESOLUTION is given for BM Not regularly spaced timeline The background electron counts at fixed energy and pitch angle may be contaminated with beam electrons Status parameter has two bits for electron energy and acquisition time for the electron counts bit0=0: acquisition time=1/512 s; bit0=1: acq_time=1/1024 s bit1 is the energy flag=0/1 for 1/0.5 keV electron energy
Electron Drift Instrument Electric field measured by the drift velocity of monoenergetic artificial electron beams injected perpendicularly to the ambient magnetic field
Spin resolution data with GOOD/CAUTION qualities. The values 2/1 for GOOD/CAUTION are in Status[0]. The electric field and drift velocity measurements are given in the inertial frame (a correction has been applied for the spacecraft velocity).
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
The quality of the data is in status byte 0. Other options to filter are in bytes 3,5,6. More information can be found in UG(p.8) and ICD documents.
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
This dataset has been calculated using the following products: - C3_CP_FGM_5VPS - CL_SP_AUX - C3_CP_AUX_POSGSE_1M
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
Level 3 quantity P is the negative of the spacecraft potential, calculated by averaging the Level 2 quantity P over 4 seconds. For more information on data quality and how the CAA data are processed, please consult the EFW CAA Users Guide and the EFW CAA Interface Control Document (ICD). Detailed quality information is provided as a 16 bit set of flags in the parameter P_bitmask__C3_CP_EFW_L3_P. The meaning of the bits is as follows (LSB numbering starting at 0): Bit 0: Reset. Bit 1: Bad bias. Bit 2: Probe latchup. Bit 3: Low density saturation (-68V). Bits 4-12: N/A Bit 13: Whisper operating. Bit 14: Saturation due to high bias current. Bit 15: N/A
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
This dataset has been calculated using the following products: - C3_CP_FGM_5VPS - CL_SP_AUX - C3_CP_AUX_POSGSE_1M
Each Cluster spacecraft carries an identical FGM instrument (Fluxgate Magnetometer) to measure the DC magnetic field vector. Each instrument, in turn, consists of two triaxial fluxgate magnetometers and an onboard data processing unit. The instrument samples the magnetic field at a cadence of 22 Hz (67 Hz in Burst mode). In order to minimise the magnetic background of the spacecraft, one of the magnetometer sensors (the outboard, or OB sensor) is located at the end of one of the two 5 m radial booms of the spacecraft, the other (the inboard, or IB sensor) at 1.5 m inboard from the end of the boom. Since the start of the scientific operations on February 1, 2001, only the outboard sensor on each satellite has been used.
*C3_CQ_FGM_CAVF
No TEXT global attribute value.
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C3_CQ_RAP_CAVEATS *C3_CP_RAP_DSETTINGS
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C3_CQ_STA_CALIB_YTR_CAVEATS *C3_CQ_STA_NOTSRP_MTR_CAVEATS DATASET VERSION HISTORY Version 01: First version of dataset. Version 02: Few corrected re-deliveries. Version 03: Removal of on-board calibration records is now based on the calibration bit (instead of the step-in-cal character).
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C3_CQ_STA_SA_UNDEF_MFA_TR_CAVEATS *C3_CQ_STA_NOTSRP_MTR_CAVEATS *C3_CQ_STA_CALIB_YTR_CAVEATS DATASET VERSION HISTORY: Version 09 : Reprocessed due to FGM and/or SPD-AUX files re-deliveries. Version 08 : FGM induced gaps revised and completed. Version 07 : New calibration tables plus addition of the half-interval duration and status. Removal of onboard calibration data. Now with FGM induced gaps. FGM file used described in the FILE_CAVEATS metadata section. Warning to the users of versions lower than 07: Delta_plus of Time__C3_CP_STA_PPP variables was set to a fixed value instead of a value varying with the mode. This chosen fixed value is the minimum time resolution (4s) which is correct in most of the cases (Normal Bit Rate). Note that the data themselves are correct. The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Version 05: used the new calibration tables (feb 2013). Version 03: AUX files in CDF format used are 26 hours. Same data than version02 but less missing values. Version 02: Data format corrected. Version 01: Obsolete. Should not be used !
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C3_CQ_STA_SA_PSD_NEG_CAVEATS *C3_CQ_STA_NOTSRP_MTR_CAVEATS *C3_CQ_STA_CALIB_YTR_CAVEATS Version 07 : New calibration tables plus addition of the interval duration and status. Removal of onboard calibration data. Warning to the users of versions lower than 07: Delta_plus of Time__C3_CP_STA_PSD variables is set to a fixed value instead of a value varying with the mode. This chosen fixed value is the usual minimum time resolution (1s) which is correct in most of the time (Normal Bit Rate). The time resolution is better in High Bit Rate. Note that the data themselves are correct. Version 04 : All the headers have been updated (laboratory name and email). Introduction of a new header file (Dataset). The PSD negative values in the version 03 have been replaced by the fillvalue (-1.00E+31). Version 03: The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Phase rotation corrected + exhaustive data. Older versions are obsolete and should not be used ! The negative values must not be taken into account by the users. Version 02 : Obsolete. This version may be used if Version 03 is not available, as long as only total B and total E power are used ! Version 01 : Obsolete. Should not be used !
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C3_CQ_STA_NOTSRP_MTR_CAVEATS *C3_CQ_STA_CALIB_YTR_CAVEATS Version 07 : New calibration tables plus addition of the interval duration and status. Removal of onboard calibration data. Warning to the users of versions lower than 07: Delta_plus of Time__C3_CP_STA_SM variables is set to a fixed value instead of a value varying with the mode. This chosen fixed value is the minimum time resolution (4s) which is correct in most of the cases (Normal Bit Rate) Note that the data themselves are correct. Version 04 : All the headers have been updated (laboratory name and email). Introduction of a new header file (Dataset). Units and Si Conversion of the variables BB and BE have been corrected. Version 03 : Phase rotation corrected + exhaustive data. The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Older versions are obsolete and should not be used ! Version 02 : Obsolete. Should not be used ! Version 01 : Obsolete. Should not be used !
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: dataset headers update, QUALITY changed to CONTRAST, addition of a new QUALITY variable VERSION 03: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 04: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: dataset headers update VERSION 03: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 04: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation used to calculate magnetic field and L value in PMP files produced after 23 Feb 2020.
JSOC predicted magnetic positions.
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997) AP _ Apogee CY 1 Start of visibility window at Canberra (5 deg elevation) CY 2 Start of visibility window at Canberra (5 deg elevation) CY 3 Start of visibility window at Canberra (5 deg elevation) CZ 1 End of visibility window at Canberra (5 deg elevation) CZ 2 End of visibility window at Canberra (5 deg elevation) CZ 3 End of visibility window at Canberra (5 deg elevation) CZ 4 End of visibility window at Canberra (5 deg elevation) DY 1 Start of visibility window at Vilspa (5 deg elevation) DY 2 Start of visibility window at Vilspa (5 deg elevation) DY 3 Start of visibility window at Vilspa (5 deg elevation) DZ 1 End of visibility window at Vilspa (5 deg elevation) DZ 2 End of visibility window at Vilspa (5 deg elevation) DZ 3 End of visibility window at Vilspa (5 deg elevation) GY 1 Start of visibility window at Goldstone (5 deg elevation) GY 2 Start of visibility window at Goldstone (5 deg elevation) GY 3 Start of visibility window at Goldstone (5 deg elevation) GY 4 Start of visibility window at Goldstone (5 deg elevation) GZ 1 End of visibility window at Goldstone (5 deg elevation) GZ 2 End of visibility window at Goldstone (5 deg elevation) GZ 3 End of visibility window at Goldstone (5 deg elevation) JY 1 Start of visibility window at Maspalomas (5 deg elevation) JY 2 Start of visibility window at Maspalomas (5 deg elevation) JY 3 Start of visibility window at Maspalomas (5 deg elevation) JY 4 Start of visibility window at Maspalomas (5 deg elevation) JZ 1 End of visibility window at Maspalomas (5 deg elevation) JZ 2 End of visibility window at Maspalomas (5 deg elevation) JZ 3 End of visibility window at Maspalomas (5 deg elevation) KA 1 Start of visibility window at Kourou (5 deg elevation) KA 2 Start of visibility window at Kourou (5 deg elevation) KA 3 Start of visibility window at Kourou (5 deg elevation) KA 4 Start of visibility window at Kourou (5 deg elevation) KL 1 End of visibility window at Kourou (5 deg elevation) KL 2 End of visibility window at Kourou (5 deg elevation) KL 3 End of visibility window at Kourou (5 deg elevation) KL 4 End of visibility window at Kourou (5 deg elevation) MY 1 Start of visibility window at Madrid (5 deg elevation) MY 2 Start of visibility window at Madrid (5 deg elevation) MY 3 Start of visibility window at Madrid (5 deg elevation) MY 4 Start of visibility window at Madrid (5 deg elevation) MZ 1 End of visibility window at Madrid (5 deg elevation) MZ 2 End of visibility window at Madrid (5 deg elevation) MZ 3 End of visibility window at Madrid (5 deg elevation) NS S Southbound neutral sheet NT I Enter north tail lobe from inner magnetosphere PA 1 Start of visibility window at Perth (5 deg elevation) PA 2 Start of visibility window at Perth (5 deg elevation) PA 3 Start of visibility window at Perth (5 deg elevation) PE _ Perigee PL 1 End of visibility window at Perth (5 deg elevation) PL 2 End of visibility window at Perth (5 deg elevation) PL 3 End of visibility window at Perth (5 deg elevation) PL 4 End of visibility window at Perth (5 deg elevation) QL I Inbound critical L value for auroral zone QL O Outbound critical L value for auroral zone RA 1 Start of visibility window at Redu (5 deg elevation) RA 2 Start of visibility window at Redu (5 deg elevation) RA 3 Start of visibility window at Redu (5 deg elevation) RA 4 Start of visibility window at Redu (5 deg elevation) RL 1 End of visibility window at Redu (5 deg elevation) RL 2 End of visibility window at Redu (5 deg elevation) RL 3 End of visibility window at Redu (5 deg elevation) ST O Leave south tail lobe for inner magnetosphere TL I Inbound radiation belt entry for WEC TL O Outbound radiation belt exit for WEC VL I Inbound critical L value for EDI VL O Outbound critical L value for EDI WL I Inbound critical L value for ASPOC WL O Outbound critical L value for ASPOC XL I Inbound critical L value for PEACE XL O Outbound critical L value for PEACE YL I Inbound critical L value for RAPID YL O Outbound critical L value for RAPID ZL I Inbound critical L value for CIS ZL O Outbound critical L value for CIS
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation pole used to calculate GSM latitude and MLT in PSE files produced after 23 Feb 2020. PSE files updated to support orbits >999 and six decimal figures on orbit phase from 25 March 2006.
JSOC predicted scientific events.
K. Torkar et al, Active spacecraft potential control for Cluster - implementation and first results Ann. Geophys., 19, pp 1289 - 1302, 2001)
none Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats One raw data format (5.1.5 secs) of bad data may occur when the instrument is powered on.
H. Reme et al, First multispacecraft ion measurements in and near the Earth's magnetosphere with the identical Cluster Ion Spectrometry (CIS) experiment Annales Geophysicae, 19, pp 1303 - 1354, 2001
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C3_PP_CIS_20211231 pre-validated by CIS team and supplied to UKCDC for inges The user of the CIS data needs to be cautious. Please refer to the CIS Home Page: http://cluster.irap.omp.eu/index.php?page=caveats , link [Caveats for specific data intervals], for caveats concerning these data.
G. Paschmann et al, The Electron Drift Instrument for Cluster Space Sci. Rev., 79, pp 233 - 269, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats 1) EDI's automated analysis algorithm has a known susceptibility to producing occasional incorrect values of the drift velocities (and electric fields). The code attempts to prevent these bad values to be output to the cdf file. No further removal is done in the validation process. 2) When drift velocities become sufficiently large, there can be a 180-degree ambiguity in drift direction that is usually flagged in bit 7 (counting from 0) of Status Byte 3. 3) There are two methods to analyze a spin's worth of EDI data. If bits 5 & 6 in Status Byte 3 are NOT set, the employed method was triangulation. If either bit 5 or 6 are set, then the results are from time-of-flight analysis. 4) The reported drift velocities and electric field refer to inertial coordinates, i.e., have been corrected for spacecraft velocity. However, the magnitude errors (in %) and the angle errors (in degrees), reported in Status Bytes 5 & 6, respectively, refer to the spacecraft frame and have NOT yet been converted to inertial coordinates. 5) The reduced chi-square reported as a data word is a measure of the goodness-of-fit of the triangulation analysis.
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster Space Sci. Rev., 79, pp 137 - 156, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data calibration may be unreliable at this early stage of the mission
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CSDS data are not for publication *** Be aware that data may be reprocessed as necessary to improve quality For questions on data validity please contact sdc-adm@plasma.kth.se
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment Space Sci. Rev., 79, pp 351 - 398, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 PP & SP data is generated at MSSL, then provided to UK-CDHF
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats This is PEACE PP/SP data version 3.1, produced at MSSL Based on onboard moments but using corrected geometric factors which account for uplinked changes of the values used in onboard calibration as well as estimated changes due to variable MCP gain performance Onboard moments are calculated for up to three energy ranges. Photoelectron contamination may affect 0, 1 or 2 of these ranges EFW PP probe-spacecraft potential was used to select the energy ranges to be excluded to remove misleading photoelectron contributions. Note that the density may be underestimated if there are both plasma electrons and photoelectrons in the lowest energy range When 88h58 is used for the HEEA sensor, sometimes the entire plasma electron population and photoelectrons are in just the lowest of the 3 energy ranges. This data has been deleted in this release of the PEACE PPs Data is deleted if the spacecraft electric potential is too large for the simple correction procedure to work or there is no EFW PP data available Measured electron energies have not been corrected for their acceleration by the spacecraft electric potential Onboard moments use onboard energy tables, efficiencies and response surfaces. Any errors in these parameters cannot be corrected in ground data processing Before 2001-09-11 the onboard energy efficiencies were not accurate, which caused the density in the solar wind to be overestimated. This data has been removed in this release of the PEACE PPs The calculation of T_par, T_perp and Q_par used PP FGM data The data is for context and information only. It is not suitable for detailed analysis, but may be used for event selection The next iteration of PP/SP moments will be of a higher quality Please see links under http://www.mssl.ucl.ac.uk/www_plasma/missions/cluster/clusterII.html for more information Please contact the PEACE PI to request science quality data Automatically validated by UKCDC Product delivered pre-validated by the PI institute
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster Space Sci. Rev., 79, pp 399 - 473, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data processed on 2024-10-18T10:59:07Z Caveats file: RAP_CAV_C3_V245.DAT; Release Sep 16, 2024
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Corrected time stamps for ions and electrons. Energy threshold shifts have been applied. Solar noise removed from electrons. Changed EDB format, on-board anisotropies not possible in NM
N. Cornilleau et al, The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment Space Sci. Rev., 79, pp 107 - 136, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats PI Software Version 4.2, 25 September 2006
P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser: Performances and Perspectives for the Cluster Mission Space Sci. Rev., 79, pp 157 - 193, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Two types of parameters are provided by WHISPER: 1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding operations. The N_e_res value is calculated from an algorithm for resonance recognition, which cannot take account of all level of information available to the experimenter. The reliability of N_e_res parameters derived at the CSDS level is thus limited in an unknown manner. The N_e_res_q parameter (one value for each N_e_res data point) provides a crude idea of the probability that the N_e_res value is actually correct. A value of 0 means that the value is probably wrong, a value above 80 that it is probably correct. Anything in between reflects a crude evaluation of the chances. Refer to PI for details. 2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are related to recording of natural wave emissions. Those parameters, not affected by variations in instrument's transfer functions, are globally OK. However, two factors can affect the precision of the measurements: a) the occasional presence of spurious emissions created by operations of the EDI instrument increases the wave power values measured on SC1, SC2 and SC3, from an unknown amount, b) the limited dynamical range of the instrument leads to an underestimation of the E_pow parameters values when the voltage difference measured by the double sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp (depending of the gain chosen). As a consequence, high values have to be taken with special caution.
A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C3_UP_FGM_20230830 HAS NOT BEEN VALIDATED - USE WITH CAUTION *** For the extended mission (starting 1/1/2006) CSDS FGM products are not validated prior to release to the science community. Spikes and other artefacts that were previously removed during validation of the FGM PP/SP data may occur in these files.
High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'cluster_wbd_calibration.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. ... Bandwidth Sample Rate --------- ------------ 9.5 kHz 27.443 kHz 19 kHz 54.886 kHz 77 kHz 219.544 kHz ... COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. ...
Created Mar 2008.Revised Dec 2008, Jan 2010
WARNING: 19 and 77 kHz Bandwidth modes with 8-bit resolution, and 77 kHz Bandwidth mode with 4-bit resolution (see Resolution variable) are not continuous data modes. Always check for periodic time jumps for these modes.
Also known as Conversion Frequency.
Steps of 5 dB from 0 to 75.
Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between the Xgse axis and the antenna direction. Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between Ygse axis and the projection of the antenna direction in the Ygse-Zgse plane, measured counter-clockwise from +Ygse (angle=0 deg) to +Zgse (angle=90 deg), -Ygse (angle=180 deg) and -Zgse (angle=270 deg). Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
DC Offset values may be used to reverse calibrate the data to the original raw counts and to determine the boundaries of the original transport packets. A description of the procedure may be found in the 'cluster_wbd_calibration.pdf' document (see Global attributes section of this file). In addition, sample code for reverse calibration may be found in the above mentioned document.
WARNING: If Translation is not equal to 0, this variable represents the electric field amplitude associated with the down-converted waveform. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.
Clipped data: Measurement was equal to raw data value maximum (255) or minimum (0). This does not necessarily mean the receiver was in saturation, which would be accompanied by non-linear effects.
High time resolution calibrated waveform data sampled in one of 3 frequency bandwidths in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'CAA_EST_CR_WBD_v20.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, see 'CAA_EST_CR_WBD_v20.pdf'. The steps for converting are briefly outlined below: 1) If Electric Field, first divide calibrated data by 1000 to get V m^-1; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth VAR_NOTES for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table in VAR_NOTES of the 'BM_Mode' variable for the appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any;7) if Translation is not equal to 0, add the appropriate translation frequency to each frequency component (see Translation CATDESC for the exact values). ... COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. ...
Created Nov 2014.
WARNING: Burst Modes 0 through 5 are not continuous data modes (see 'BM_Mode' variable). Always check for periodic time jumps for these modes.Values for Bandwidth are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Also known as Conversion Frequency.WARNING: If this variable is not equal to 0, the electric field waveform (WBD_Elec vs. Epoch variables) is the product of a down-conversion to 0.0 kHz which took place onboard within the WBD instrument. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.Values for Translation are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Values for ANTENNA are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Steps of 5 dB from 0 to 75.Values for Gain are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between the Xgse axis and the antenna direction. Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between Ygse axis and the projection of the antenna direction in the Ygse-Zgse plane, measured counter-clockwise from +Ygse (angle=0 deg) to +Zgse (angle=90 deg), -Ygse (angle=180 deg) and -Zgse (angle=270 deg). Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
DC Offset values may be used to reverse calibrate the data to the original raw counts and to determine the boundaries of the original transport packets. A description of the procedure may be found in the WBD calibration report 'CAA_EST_CR_WBD_v20.pdf' (see Global attributes section of this file). In addition, sample code for reverse calibration may be found in the above mentioned document.
WARNING: If Translation is not equal to 0, this variable represents the electric field amplitude associated with the down-converted waveform. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.
Clipped data: Measurement was equal to raw data value maximum (255) or minimum (0). This does not necessarily mean the receiver was in saturation, which would be accompanied by non-linear effects.
The following are the sampling rates for each of the 10 defined modes: Bandwidth Burst Mode Sample Rate --------- ---------- ------------ 9.5 kHz 0, 1 27.443 kHz19.0 kHz 2, 3 54.886 kHz77.0 kHz 4, 5 219.544 kHz 9.5 kHz 6, 7 9.148 kHz 9.5 kHz 8, 9 6.861 kHz
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
Cluster Ion Spectrometry. The CIS (Cluster Ion Spectrometry) experiment is a comprehensive ionic plasma spectrometry package onboard the Cluster spacecraft, capable of obtaining full three-dimentional ion distributions (about 0 to 40 keV/e) with a time resolution of one spacecraft spin (4 sec) and with mass-per-charge composition determination. The CIS package consists of two different instruments, a time-of-flight ion Composition and Distribution Function analyser (CODIF, or CIS-1) and a Hot Ion Analyser (HIA, or CIS-2).
*C4_CQ_CIS-CODIF_CAVEATS
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
This dataset has been calculated using the following products: - C4_CP_FGM_5VPS - CL_SP_AUX - C4_CP_AUX_POSGSE_1M
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
Level 3 quantity P is the negative of the spacecraft potential, calculated by averaging the Level 2 quantity P over 4 seconds. For more information on data quality and how the CAA data are processed, please consult the EFW CAA Users Guide and the EFW CAA Interface Control Document (ICD). Detailed quality information is provided as a 16 bit set of flags in the parameter P_bitmask__C4_CP_EFW_L3_P. The meaning of the bits is as follows (LSB numbering starting at 0): Bit 0: Reset. Bit 1: Bad bias. Bit 2: Probe latchup. Bit 3: Low density saturation (-68V). Bits 4-12: N/A Bit 13: Whisper operating. Bit 14: Saturation due to high bias current. Bit 15: N/A
The EFW (Electric Field and Wave) instrument consists of four spherical probes deployed orthogonally on 44-meter-long wire booms in the spin plane of the spacecraft. The potential differences between opposing probes, separated by 88 m tip-to-tip, are measured to provide electric field measurements in two directions, thus providing the full electric field vector in the spin plane of the spacecraft. Additionally, the potential differences between each of the probes and the spacecraft are measured, providing an estimate of the spacecraft potential relative to the plasma, which can be used as a proxy for the ambient electron density. The output analogue signals from the preamplifiers connected to the spherical probes are also provided to the wave instruments (STAFF, WHISPER and WBD) for analysis of high frequency wave phenomena.
This dataset has been calculated using the following products: - C4_CP_FGM_5VPS - CL_SP_AUX - C4_CP_AUX_POSGSE_1M
Each Cluster spacecraft carries an identical FGM instrument (Fluxgate Magnetometer) to measure the DC magnetic field vector. Each instrument, in turn, consists of two triaxial fluxgate magnetometers and an onboard data processing unit. The instrument samples the magnetic field at a cadence of 22 Hz (67 Hz in Burst mode). In order to minimise the magnetic background of the spacecraft, one of the magnetometer sensors (the outboard, or OB sensor) is located at the end of one of the two 5 m radial booms of the spacecraft, the other (the inboard, or IB sensor) at 1.5 m inboard from the end of the boom. Since the start of the scientific operations on February 1, 2001, only the outboard sensor on each satellite has been used.
*C4_CQ_FGM_CAVF
No TEXT global attribute value.
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
Research with Adaptive Particle Imaging Detectors (RAPID) The RAPID spectrometer for the Cluster mission is an advanced particle detector for the analysis of suprathermal plasma distributions in the energy range from 39-400 keV for electrons, 28-1500 keV (4000 keV) for hydrogen, and 10 keV/nuc - 1500 keV (4000 keV) for heavier ions.
*C4_CQ_RAP_CAVEATS *C4_CP_RAP_DSETTINGS
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C4_CQ_STA_CALIB_YTR_CAVEATS *C4_CQ_STA_NOTSRP_MTR_CAVEATS DATASET VERSION HISTORY Version 01: First version of dataset. Version 02: Few corrected re-deliveries. Version 03: Removal of on-board calibration records is now based on the calibration bit (instead of the step-in-cal character).
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C4_CQ_STA_SA_UNDEF_MFA_TR_CAVEATS *C4_CQ_STA_NOTSRP_MTR_CAVEATS *C4_CQ_STA_CALIB_YTR_CAVEATS DATASET VERSION HISTORY: Version 09 : Reprocessed due to FGM and/or SPD-AUX files re-deliveries. Version 08 : FGM induced gaps revised and completed. Version 07 : New calibration tables plus addition of the half-interval duration and status. Removal of onboard calibration data. Now with FGM induced gaps. FGM file used described in the FILE_CAVEATS metadata section. Warning to the users of versions lower than 07: Delta_plus of Time__C4_CP_STA_PPP variables is set to a fixed value instead of a value varying with the mode. This chosen fixed value is the minimum time resolution (4s) which is correct in most of the cases (Normal Bit Rate). Note that the data themselves are correct. The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Version 05: used the new calibration tables (feb 2013). Version 03: AUX files in CDF format used are 26 hours. Same data than version02 but less missing values. Version 02: Data format corrected. Version 01: Obsolete. Should not be used !
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C4_CQ_STA_SA_PSD_NEG_CAVEATS *C4_CQ_STA_NOTSRP_MTR_CAVEATS *C4_CQ_STA_CALIB_YTR_CAVEATS Version 07 : New calibration tables plus addition of the interval duration and status. Removal of onboard calibration data. Warning to the users of versions lower than 07: Delta_plus of Time__C4_CP_STA_PSD variables is set to a fixed value instead of a value varying with the mode. This chosen fixed value is the usual minimum time resolution (1s) which is correct in most of the time (Normal Bit Rate). The time resolution is better in High Bit Rate. Note that the data themselves are correct. Version 04 : All the headers have been updated (laboratory name and email). Introduction of a new header file (Dataset). The PSD negative values in the version 03 have been replaced by the fillvalue (-1.00E+31). Version 03: The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Phase rotation corrected + exhaustive data. Older versions are obsolete and should not be used ! The negative values must not be taken into account by the users. Version 02 : Obsolete. This version may be used if Version 03 is not available, as long as only total B and total E power are used ! Version 01 : Obsolete. Should not be used !
STAFF (Spatio Temporal Analysis of Field Fluctuations) is one of the five experiments of the Wave Experiment Consortium (WEC). The STAFF experiment comprises a boom-mounted three-axis search coil magnetometer to measure magnetic fluctuations in the frequency range 0.1 Hz - 4 kHz, a preamplifier and an electronics box that houses the two complementary data-analysis packages: a digital Spectrum Analyser, and an on-board waveform unit (SC).
*C4_CQ_STA_NOTSRP_MTR_CAVEATS *C4_CQ_STA_CALIB_YTR_CAVEATS Version 07 : New calibration tables plus addition of the interval duration and status. Removal of onboard calibration data. Warning to the users of versions lower than 07: Delta_plus of Time__C4_CP_STA_SM variables is set to a fixed value instead of a value varying with the mode. This chosen fixed value is the minimum time resolution (4s) which is correct in most of the cases (Normal Bit Rate) Note that the data themselves are correct. Version 04 : All the headers have been updated (laboratory name and email). Introduction of a new header file (Dataset). Units and Si Conversion of the variables BB and BE have been corrected. Version 03 : Phase rotation corrected + exhaustive data. The data were time tagged using TED version 2.4.3 (TED Library 4.4.3 User Patch 1), provided by the Sheffield DWP Group. Older versions are obsolete and should not be used ! Version 02 : Obsolete. Should not be used ! Version 01 : Obsolete. Should not be used !
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: dataset headers update, QUALITY changed to CONTRAST, addition of a new QUALITY variable VERSION 03: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 04: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: correction of the Spectral Frequencies parameter description VERSION 03: dataset headers update VERSION 04: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 05: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
Fill values can be present (1) in the first/last values when only a part of the on-board spectrum values is sent to ground and/or (2) inside the spectrum when a specific mode is used, sending only one value (the highest signal) for each pair of consecutive frequency bins
The Wave of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the CLUSTER project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.
DATASET VERSION HISTORY VERSION 01: first version of dataset VERSION 02: dataset headers update VERSION 03: TIME_RESOLUTION, VERSION_NUMBER, DATASET_TYPE metadata update - Aug 2020 VERSION 04: CONTACT_COORDINATES and ACKNOWLEDGEMENT metadata update - Mar 2022
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation used to calculate magnetic field and L value in PMP files produced after 23 Feb 2020.
JSOC predicted magnetic positions.
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997) AP _ Apogee CY 1 Start of visibility window at Canberra (5 deg elevation) CY 2 Start of visibility window at Canberra (5 deg elevation) CY 3 Start of visibility window at Canberra (5 deg elevation) CZ 1 End of visibility window at Canberra (5 deg elevation) CZ 2 End of visibility window at Canberra (5 deg elevation) CZ 3 End of visibility window at Canberra (5 deg elevation) CZ 4 End of visibility window at Canberra (5 deg elevation) DY 1 Start of visibility window at Vilspa (5 deg elevation) DY 2 Start of visibility window at Vilspa (5 deg elevation) DY 3 Start of visibility window at Vilspa (5 deg elevation) DY 4 Start of visibility window at Vilspa (5 deg elevation) DZ 1 End of visibility window at Vilspa (5 deg elevation) DZ 2 End of visibility window at Vilspa (5 deg elevation) DZ 3 End of visibility window at Vilspa (5 deg elevation) GY 1 Start of visibility window at Goldstone (5 deg elevation) GY 2 Start of visibility window at Goldstone (5 deg elevation) GY 3 Start of visibility window at Goldstone (5 deg elevation) GY 4 Start of visibility window at Goldstone (5 deg elevation) GZ 1 End of visibility window at Goldstone (5 deg elevation) GZ 2 End of visibility window at Goldstone (5 deg elevation) GZ 3 End of visibility window at Goldstone (5 deg elevation) JY 1 Start of visibility window at Maspalomas (5 deg elevation) JY 2 Start of visibility window at Maspalomas (5 deg elevation) JY 3 Start of visibility window at Maspalomas (5 deg elevation) JY 4 Start of visibility window at Maspalomas (5 deg elevation) JZ 1 End of visibility window at Maspalomas (5 deg elevation) JZ 2 End of visibility window at Maspalomas (5 deg elevation) JZ 3 End of visibility window at Maspalomas (5 deg elevation) KA 1 Start of visibility window at Kourou (5 deg elevation) KA 2 Start of visibility window at Kourou (5 deg elevation) KA 3 Start of visibility window at Kourou (5 deg elevation) KA 4 Start of visibility window at Kourou (5 deg elevation) KL 1 End of visibility window at Kourou (5 deg elevation) KL 2 End of visibility window at Kourou (5 deg elevation) KL 3 End of visibility window at Kourou (5 deg elevation) KL 4 End of visibility window at Kourou (5 deg elevation) MY 1 Start of visibility window at Madrid (5 deg elevation) MY 2 Start of visibility window at Madrid (5 deg elevation) MY 3 Start of visibility window at Madrid (5 deg elevation) MY 4 Start of visibility window at Madrid (5 deg elevation) MZ 1 End of visibility window at Madrid (5 deg elevation) MZ 2 End of visibility window at Madrid (5 deg elevation) MZ 3 End of visibility window at Madrid (5 deg elevation) NS S Southbound neutral sheet NT I Enter north tail lobe from inner magnetosphere PA 1 Start of visibility window at Perth (5 deg elevation) PA 2 Start of visibility window at Perth (5 deg elevation) PA 3 Start of visibility window at Perth (5 deg elevation) PA 4 Start of visibility window at Perth (5 deg elevation) PE _ Perigee PL 1 End of visibility window at Perth (5 deg elevation) PL 2 End of visibility window at Perth (5 deg elevation) PL 3 End of visibility window at Perth (5 deg elevation) PL 4 End of visibility window at Perth (5 deg elevation) PL 5 End of visibility window at Perth (5 deg elevation) QL I Inbound critical L value for auroral zone QL O Outbound critical L value for auroral zone RA 1 Start of visibility window at Redu (5 deg elevation) RA 2 Start of visibility window at Redu (5 deg elevation) RA 3 Start of visibility window at Redu (5 deg elevation) RL 1 End of visibility window at Redu (5 deg elevation) RL 2 End of visibility window at Redu (5 deg elevation) RL 3 End of visibility window at Redu (5 deg elevation) ST O Leave south tail lobe for inner magnetosphere TL I Inbound radiation belt entry for WEC TL O Outbound radiation belt exit for WEC VL I Inbound critical L value for EDI VL O Outbound critical L value for EDI WL B Outbound critical L value 2 for ASPOC WL I Inbound critical L value for ASPOC WL O Outbound critical L value for ASPOC XL I Inbound critical L value for PEACE XL O Outbound critical L value for PEACE YL I Inbound critical L value for RAPID YL O Outbound critical L value for RAPID ZL I Inbound critical L value for CIS ZL O Outbound critical L value for CIS
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation pole used to calculate GSM latitude and MLT in PSE files produced after 23 Feb 2020. PSE files updated to support orbits >999 and six decimal figures on orbit phase from 25 March 2006.
JSOC predicted scientific events.
K. Torkar et al, Active spacecraft potential control for Cluster - implementation and first results Ann. Geophys., 19, pp 1289 - 1302, 2001)
none Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats One raw data format (5.1.5 secs) of bad data may occur when the instrument is powered on.
H. Reme et al, First multispacecraft ion measurements in and near the Earth's magnetosphere with the identical Cluster Ion Spectrometry (CIS) experiment Annales Geophysicae, 19, pp 1303 - 1354, 2001
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C4_PP_CIS_20220930 pre-validated by CIS team and supplied to UKCDC for inges The user of the CIS data needs to be cautious. Please refer to the CIS Home Page: http://cluster.irap.omp.eu/index.php?page=caveats , link [Caveats for specific data intervals], for caveats concerning these data.
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster Space Sci. Rev., 79, pp 209 - 231, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C4_PP_DWP_20220701 HAS NOT BEEN VALIDATED - USE WITH CAUTION *** This CSDS DWP product has not been validated prior to release.
G. Paschmann et al, The Electron Drift Instrument for Cluster Space Sci. Rev., 79, pp 233 - 269, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats C4 EDI switched off
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster Space Sci. Rev., 79, pp 137 - 156, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data calibration may be unreliable at this early stage of the mission
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CSDS data are not for publication *** Be aware that data may be reprocessed as necessary to improve quality For questions on data validity please contact sdc-adm@plasma.kth.se Fill value inserted for E_dusk__C4_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z Fill value inserted for E_pow_f1__C4_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z Fill value inserted for E_sigma__C4_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z Fill value inserted for U_probe_sc__C4_PP_EFW: No reason given for time range 2024-05-31T09:10:00Z to 2024-05-31T09:13:00Z
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment Space Sci. Rev., 79, pp 351 - 398, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 PP & SP data is generated at MSSL, then provided to UK-CDHF
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats This is PEACE PP/SP data version 3.1, produced at MSSL Based on onboard moments but using corrected geometric factors which account for uplinked changes of the values used in onboard calibration as well as estimated changes due to variable MCP gain performance Onboard moments are calculated for up to three energy ranges. Photoelectron contamination may affect 0, 1 or 2 of these ranges EFW PP probe-spacecraft potential was used to select the energy ranges to be excluded to remove misleading photoelectron contributions. Note that the density may be underestimated if there are both plasma electrons and photoelectrons in the lowest energy range When 88h58 is used for the HEEA sensor, sometimes the entire plasma electron population and photoelectrons are in just the lowest of the 3 energy ranges. This data has been deleted in this release of the PEACE PPs Data is deleted if the spacecraft electric potential is too large for the simple correction procedure to work or there is no EFW PP data available Measured electron energies have not been corrected for their acceleration by the spacecraft electric potential Onboard moments use onboard energy tables, efficiencies and response surfaces. Any errors in these parameters cannot be corrected in ground data processing Before 2001-09-11 the onboard energy efficiencies were not accurate, which caused the density in the solar wind to be overestimated. This data has been removed in this release of the PEACE PPs The calculation of T_par, T_perp and Q_par used PP FGM data The data is for context and information only. It is not suitable for detailed analysis, but may be used for event selection The next iteration of PP/SP moments will be of a higher quality Please see links under http://www.mssl.ucl.ac.uk/www_plasma/missions/cluster/clusterII.html for more information Please contact the PEACE PI to request science quality data Automatically validated by UKCDC Product delivered pre-validated by the PI institute
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster Space Sci. Rev., 79, pp 399 - 473, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data processed on 2024-10-18T10:59:08Z Caveats file: RAP_CAV_C4_V245.DAT; Release Sep 16, 2024
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Corrected time stamps for ions and electrons. Energy threshold shifts have been applied. Changed EDB format, on-board anisotropies not possible in NM
N. Cornilleau et al, The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment Space Sci. Rev., 79, pp 107 - 136, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats PI Software Version 4.2, 25 September 2006
P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser: Performances and Perspectives for the Cluster Mission Space Sci. Rev., 79, pp 157 - 193, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Two types of parameters are provided by WHISPER: 1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding operations. The N_e_res value is calculated from an algorithm for resonance recognition, which cannot take account of all level of information available to the experimenter. The reliability of N_e_res parameters derived at the CSDS level is thus limited in an unknown manner. The N_e_res_q parameter (one value for each N_e_res data point) provides a crude idea of the probability that the N_e_res value is actually correct. A value of 0 means that the value is probably wrong, a value above 80 that it is probably correct. Anything in between reflects a crude evaluation of the chances. Refer to PI for details. 2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are related to recording of natural wave emissions. Those parameters, not affected by variations in instrument's transfer functions, are globally OK. However, two factors can affect the precision of the measurements: a) the occasional presence of spurious emissions created by operations of the EDI instrument increases the wave power values measured on SC1, SC2 and SC3, from an unknown amount, b) the limited dynamical range of the instrument leads to an underestimation of the E_pow parameters values when the voltage difference measured by the double sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp (depending of the gain chosen). As a consequence, high values have to be taken with special caution.
A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C4_UP_FGM_20230830 HAS NOT BEEN VALIDATED - USE WITH CAUTION *** For the extended mission (starting 1/1/2006) CSDS FGM products are not validated prior to release to the science community. Spikes and other artefacts that were previously removed during validation of the FGM PP/SP data may occur in these files.
High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'cluster_wbd_calibration.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data by 1000 to get V m^-1; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. ... Bandwidth Sample Rate --------- ------------ 9.5 kHz 27.443 kHz 19 kHz 54.886 kHz 77 kHz 219.544 kHz ... COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. ...
Created Mar 2008.Revised Dec 2008, Jan 2010
WARNING: 19 and 77 kHz Bandwidth modes with 8-bit resolution, and 77 kHz Bandwidth mode with 4-bit resolution (see Resolution variable) are not continuous data modes. Always check for periodic time jumps for these modes.
Also known as Conversion Frequency.
Steps of 5 dB from 0 to 75.
Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between the Xgse axis and the antenna direction. Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between Ygse axis and the projection of the antenna direction in the Ygse-Zgse plane, measured counter-clockwise from +Ygse (angle=0 deg) to +Zgse (angle=90 deg), -Ygse (angle=180 deg) and -Zgse (angle=270 deg). Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
DC Offset values may be used to reverse calibrate the data to the original raw counts and to determine the boundaries of the original transport packets. A description of the procedure may be found in the 'cluster_wbd_calibration.pdf' document (see Global attributes section of this file). In addition, sample code for reverse calibration may be found in the above mentioned document.
WARNING: If Translation is not equal to 0, this variable represents the electric field amplitude associated with the down-converted waveform. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.
Clipped data: Measurement was equal to raw data value maximum (255) or minimum (0). This does not necessarily mean the receiver was in saturation, which would be accompanied by non-linear effects.
High time resolution calibrated waveform data sampled in one of 3 frequency bandwidths in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the document 'CAA_EST_CR_WBD_v20.pdf'. Because the calibration was applied in the time domain using a simple equation the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, see 'CAA_EST_CR_WBD_v20.pdf'. The steps for converting are briefly outlined below: 1) If Electric Field, first divide calibrated data by 1000 to get V m^-1; 2) Apply window of preference, if any (such as Hanning, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth VAR_NOTES for non-continuous modes); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table in VAR_NOTES of the 'BM_Mode' variable for the appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any;7) if Translation is not equal to 0, add the appropriate translation frequency to each frequency component (see Translation CATDESC for the exact values). ... COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. ...
Created Nov 2014.
WARNING: Burst Modes 0 through 5 are not continuous data modes (see 'BM_Mode' variable). Always check for periodic time jumps for these modes.Values for Bandwidth are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Also known as Conversion Frequency.WARNING: If this variable is not equal to 0, the electric field waveform (WBD_Elec vs. Epoch variables) is the product of a down-conversion to 0.0 kHz which took place onboard within the WBD instrument. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.Values for Translation are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Values for ANTENNA are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Steps of 5 dB from 0 to 75.Values for Gain are subject to error before mode switches or gaps due to Whisper soundings. Please refer to the caveats document.
Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between the Xgse axis and the antenna direction. Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
Total angle between Ygse axis and the projection of the antenna direction in the Ygse-Zgse plane, measured counter-clockwise from +Ygse (angle=0 deg) to +Zgse (angle=90 deg), -Ygse (angle=180 deg) and -Zgse (angle=270 deg). Antenna refers to the antenna in use, either E or B. See ANTENNA variable.
DC Offset values may be used to reverse calibrate the data to the original raw counts and to determine the boundaries of the original transport packets. A description of the procedure may be found in the WBD calibration report 'CAA_EST_CR_WBD_v20.pdf' (see Global attributes section of this file). In addition, sample code for reverse calibration may be found in the above mentioned document.
WARNING: If Translation is not equal to 0, this variable represents the electric field amplitude associated with the down-converted waveform. This affects the apparent frequency content of the electric field amplitude when plotted vs. time, as well as the frequency of the derived components when an FFT is applied to the electric field data. Refer to the WBD User Guide 'CAA_EST_UG_WBD_v20.pdf' and calibration report 'CAA_EST_CR_WBD_v20.pdf' for more information.
Clipped data: Measurement was equal to raw data value maximum (255) or minimum (0). This does not necessarily mean the receiver was in saturation, which would be accompanied by non-linear effects.
The following are the sampling rates for each of the 10 defined modes: Bandwidth Burst Mode Sample Rate --------- ---------- ------------ 9.5 kHz 0, 1 27.443 kHz19.0 kHz 2, 3 54.886 kHz77.0 kHz 4, 5 219.544 kHz 9.5 kHz 6, 7 9.148 kHz 9.5 kHz 8, 9 6.861 kHz
No TEXT global attribute value.
Cassini magnetic-field 1 minute averages for the year 2020 in RTN coordinates. RTN coordinates consist of R (radial component, Sun tothe spacecraft), T (tangential component, parallel to the Solar Equatorial plane and perpendicular to R), and N (normal component, completes right handed set). This file contains a subset of all of the Cassini MAG data for 2001consisting of only the data after the day of the last Jupiter bowshock crossing (2001-01-15). This file was produced from raw (L1A) data at the PDS/PPI node usingsoftware provided by the Cassini MAG team, and employing the latest calibration available. The MAG team reports that while range-0 data are well calibrated, higher range data needs improvement (see the RANGE_CHANGES.ASC document for a time history of range changes). Thesedata will be replaced as the calibration is improved." The data are mostly from the fluxgate magnetometer (FGM). The tableat vhm.txt identifies the 52 days in 2000-2004 for which the data are solely from the vector helium magnetometer (VHM). Days not in the table contain only FGM data.VHM_mode variable indicates (value 1) whether data are from VHM The data were produced from raw (L1A) data at the PDS/PPI node using software provided by the Cassini MAG team, and employing the latest calibration available. PDS/PPI produced both 1-sec vectors and 1-min averages. The MAG team reports that while range-0 data are well calibrated for both FGM and VHM, higher range data need improvement. FGM_mode variable indicates (value 0) if data is range-0.Seehttp://www.igpp.ucla.edu/cgi-bin/ditdos?volume=COMAG_0XXX&folder=DOCU MENT/DATA_QUALITY&file=RANGE_CHANGESfor details. In particular, this documentation reports that FGM wasin range=0 for the following extended intervals (plus other brief intervals): 1999/230/05 - 1999/245/07 (YYYY/DDD/HH, inclusive)1999/245/09 - 2000/037/122000/039/00 - 2000/053/182000/053/20 - 2000/056/012000/057/23 - 2002/334/132002/334/17 - 2003/292/182003/292/22 - 2004/046/112004/046/15 - 2004/088/082004/088/12 - 2004/136/062004/136/11 - 2004/174/012004/174/06 - 2004/182/17
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 New SILSO sunspot number series used for all records in PCY files produced after 2 Aug 2015.
JSOC predicted Solar cycle trends. Please acknowledge sunspot numbers as: Source: WDC-SILSO, Royal Observatory of Belgium, Brussels.
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 1997 For geometrical configuration parameters, p328 of Tetrahedron Geometric Factors by P.Robert et al, in Analysis Methods for Multi-Spacecraft Data, ed. G.Paschmann & P.Daly, pub. 1998 by the European Space Agency and the International Space Institute, Bern.
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation pole used to calculate dipole tilt and GSE-GSM angle in PGP files produced after 23 Feb 2020. Orbit number field supports 4-digit orbits and 6 figure phase in PGP files produced after 20 March 2006.
JSOC predicted Orbits. Using spacecraft C3 as reference spacecraft.
Orbital Parameters Calculated from Short Term Orbit File of RDM For geometry configuration parameters, see p 328 of Tetrahedron Geometric Factors by P.Robert et al, in Analysis Methods for Multi-Spacecraft Data, ed. G.Paschmann & P.Daly, pub. 1998 by the European Space Agency and the International Space Institute, Bern.
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation pole used to calculate GSE-to-GSM angle and dipole tilt from 1 January 2020
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
The Communications/Navigation Outage Forecasting System (C/NOFS) is a prototype operational system designed to monitor and forecast ionospheric scintillation in real-time and on a global scale. In the space-borne segment, C/NOFS will fly a system of proven sensors on-board a three-axis stabilized satellite to detect ionospheric scintillation. This will provide data for global, real-time specification, and 4 hour forecast capability. C/NOFS is a joint effort between the DOD Space Test Program and AFRL (Air Force Research Laboratory). The space test program provides the spacecraft, launch vehicle, launch and first year on-orbit operations. AFRL is responsible for the multi-instrument payload, payload integration and test, model development, data center operations, and product generation and distribution. The C/NOFS payload consists of six instruments: the Planar Langmuir Probe (PLP) for measurements of plasma density, the Vector Electric Field Instrument (VEFI) for measurements of vector electric and magnetic fields, the Ion Velocity Meter (IVM) for measurements of plasma drift velocities and ion temperatures, the Neutral Wind Meter (NWM) for measurements of neutral winds, the C/NOFS Occultation Receiver for Ionospheric Sensing and Specification (CORISS) for remote sensing of the electron density vertical profile, the Coherent Electromagnetic Radio Tomography (CERTO) for measurements of ionospheric scintillation parameters. Both the Neutral Wind Meter (NWM) and the Ion Velocity Meter (IVM) are provided by NASA as the CINDI (Coupled Ion-Neutral Dynamics Investigation) payload, which was selected as an Explorer Mission of Opportunity. The goal of C/NOFS is to forecast scintillation three to six hours before its onset such that system operators will be able to plan in ways that will optimize mission command and control. The spacecraft will be launched into an orbit with perigee/apogee of 400/700 km, and an inclination of 13 degrees. Launch is currently planned for early 2006. Information about C/NOFS can be found at Air Force Research Laboratory page: http://www.kirtland.af.mil/shared/media/document/AFD-070404-094.pdf. The Coupled Ion-Neutral Dynamics Investigation (CINDI) payload is funded by NASA as an Explorer Mission of Opportunity. CINDI consists of two instruments: the Ion Velocity Meter (IVM) and the Neutral Wind Meter (NWM). The IVM instrument includes a ion drift meter and a retarding potential analyzer. IVM measure the ion drift vector, the ion temperature, and the major ion composition with a spatial resolution of about 4 km along the satellite track; the ion drift meter also provides vertical and horizontal ion drift components at 500 m resolution. The NWM consists of a cross track wind sensor and a ram wind sensor providing a direct measure of the neutral wind vector with a spatial resolution of about 8 km along the satellite track.
Offset and photoemission corrected, if possible. Check Offset flag variable
Offset and photoemission corrected, if possible. Check Offset flag variable
Offset and photoemission corrected, if possible. Check Offset flag variable
offset flag = 0 if offset corrected data are available, =1 if non-offset data are used.
Earth-centered inertial (ECI) coordinates with Z going through the North Pole and the X-Y plane in the equatorial plane not rotating with Earth
Earth-centered inertial (ECI) coordinates with Z going through the North Pole and the X-Y plane in the equatorial plane not rotating with Earth
Earth-centered inertial (ECI) coordinates with Z going through the North Pole and the X-Y plane in the equatorial plane not rotating with Earth
Earth-centered inertial (ECI) coordinates with Z going through the North Pole and the X-Y plane in the equatorial plane not rotating with Earth
Earth-centered inertial (ECI) coordinates with Z going through the North Pole and the X-Y plane in the equatorial plane not rotating with Earth
Earth-centered inertial (ECI) coordinates with Z going through the North Pole and the X-Y plane in the equatorial plane not rotating with Earth
International Geomagnetic Reference Field (IGRF)
International Geomagnetic Reference Field (IGRF)
International Geomagnetic Reference Field (IGRF)
The Planar Langmuir Probe on C/NOFS is a suite of 2 current measuring sensors mounted on the ram facing surface of the spacecraft. The primary sensor is an Ion Trap (conceptually similar to RPAs flown on many other spacecraft) capable of measuring ion densities as low as 1 cm-3 with a 12 bit log electrometer. The secondary senor is a swept bias planar Langmuir probe (Surface Probe) capable of measuring Ne, Te, and spacecraft potential. The ion number density is the one second average of the ion density sampled at either 32, 256, 512, or 1024 Hz (depending on the mode). The ion density standard deviation is the standard deviation of the samples used to produce the one second average number density. DeltaN/N is the detrened ion number density 1 second standard deviation divided by the mean 1 sec density. The electron density, electron temperature, and spacecraft potential are all derived from a least squares fit to the current-bias curve from the Surface Probe. The data are PRELIMINARY, and as such, are intended for BROWSE PURPOSES ONLY. Regestering your email will allow notification of updates.
From PLP Ion Trap
From PLP Ion Trap
From PLP Ion Trap
From PLP Surface Probe swept bias mode
From PLP Surface Probe swept bias mode
From PLP Surface Probe swept bias mode
Semi-major axis: 6378.137 km, Semi-minor axis 6356.752 km
Semi-major axis: 6378.137 km, Semi-minor axis 6356.752 km
Semi-major axis: 6378.137 km, Semi-minor axis 6356.752 km
Difference in geographic longitude between solar and satellite subpoints
The DC vector magnetometer on the CNOFS spacecraft is a three axis, fluxgate sensor with active thermal control situated on a 0.6m boom. This magnetometer measures the Earth's magnetic field, B, using 16 bit A/D converters at 1 sample per sec with a range of +/- 45,000 nT per sensor axis. Its primary objective on the CNOFS spacecraft is to enable the most accurate V x B and E x B measurements along the spacecraft trajectory, where V is the spacecraft velocity in the fixed frame of the earth and E is the ambient, measured electric field. The magnetic field data also provide indications of ionospheric currents as well as other geophysical phenomena. In-flight calibration of the raw magnetic field data is carried out to determine gains, offsets, and the non-orthogonality matrix in the sensor axes frame. The IGRF-11 model is used as a reference to help determine the calibration. The calibrated magnetic field measurements are provided in the data file. A full description of the instrument can be found in the published paper: The Vector Electric Field Instrument (VEFI) on the C/NOFS Satellite, Pfaff et al., 2021, doi.org/10.1007/s11214-021-00859-y.
Geodetic coordinate system, B field in the north direction with respect to the WGS-84 reference ellipsoid of the earth.
Geodetic coordinate system, B field in the up direction with respect to the WGS-84 reference ellipsoid of the earth.
Geodetic coordinate system, B field in the west direction with respect to the WGS-84 reference ellipsoid of the earth.
Geodetic coordinate system, IGRF-11 B field in the north direction with respect to the WGS-84 reference ellipsoid of the earth.
Geodetic coordinate system, IGRF-11 B field in the up direction with respect to the WGS-84 reference ellipsoid of the earth.
Geodetic coordinate system, IGRF-11 B field in the west direction with respect to the WGS-84 reference ellipsoid of the earth.
Geodetic latitude with respect to the WGS-84 earth model.
Geodetic longitude with respect to the WGS-84 earth model.
Geodetic altitude with respect to the WGS-84 earth model.
Zonal direction is defined by Bxr, where B is the local magnetic field vector and r is the radius vector from the center of the earth to the spacecraft. Sign convention is that eastward is positive. dB = delta B = measured B field - IGRF-11 model B field.
Meridional direction is defined by ZxB, where Z is the zonal vector direction and B is the local magnetic field vector. dB = delta B = measured B field - IGRF-11 model B field.
Parallel direction is defined by the local magnetic field vector. dB = delta B = measured B field - IGRF-11 model B field.
This data file contains information on the electric field solution as processed by the VEFI team at NASA/Goddard Space Flight Center. The data is PRELIMINARY, and as such, is intended for BROWSE PURPOSES ONLY. Registering your email will allow notification of updates.
Meridional direction is defined by ZxB, where Z is the zonal vector direction and B is the local magnetic field vector.
Zonal direction is defined by Bxr, where B is the local magnetic field vector and r is the radius vector from the center of the earth to the spacecraft. Sign convention is that eastward is positive.
Meridional direction is defined by ZxB, where Z is the zonal vector direction and B is the local magnetic field vector.
Zonal direction is defined by Bxr, where B is the local magnetic field vector and r is the radius vector from the center of the earth to the spacecraft. Sign convention is that eastward is positive.
Geodetic latitude with respect to the WGS-84 earth model.
Geodetic longitude with respect to the WGS-84 earth model.
Geodetic altitude with respect to the WGS-84 earth model.
This data file contains the low rate data from the VEFI lightning detector. Two photodiodes measure white light irradiance in 2 look directions and for 7 threshold values. Reference: Jacobson et al, J Atm Ocean Tech, 2011, doi:10.1175/JTECH-D-11-00047.1
Images and intensities. 557.7nm Images binned to geodetic grid References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J., McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D., Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.
Created 31-DEC-1999
North & East Velocity components at 336.5 EDFL long. from 64.2 to 67.0 EDFL lat. References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J., McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D., Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.
Created 3-OCT-1994
Magnetic Field Extrema and Location References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J., McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D., Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.
Created 31-DEC-1999 Added station Taloyoak on 29-SEP-1994
Local equivalent to AU index, but computed from magnetic field perturbations measured at specific stations of the CANOPUS array
Local equivalent to AL index, but computed from magnetic field perturbations measured at stations of the CANOPUS array
Station Status, Merged Scaled 5577A Scans and Peak Intensity Merged Scans>from 3 stations along constant Geodetic Long. of 265, from Lat. 46 to 67 References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J., McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D., Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993. 2.Samson, J.C., Lyons, L.R., Newell, P.T., Creutzberg, F. and Xu, B., Proton aurora substorm intensifications, Geophys. Res. Letters, 19, 2167, 1992. 3.Samson, J.C., Hughes, T.J., Creutzberg, F., Wallis, D.D., Greenwald, R.A. and Ruohoniemi, J.M., Observations of a detached discrete arc in association with field line resonances, J. Geophys. Res., 96, 15, 683, 1991.
Created 31-DEC-1999
Riometer measurements and Location References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J., McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D., Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.
Created 31-DEC-1999
No TEXT global attribute value.
No TEXT global attribute value.
CRRES MEA Data Archive This is the re-processed version of the MEA data archive from the CRRES spacecraft. The raw data provided by Principal Investigator A. Vampola have been processed to derive 1 min average data. The data consists of counting rates from 17 energy channels in the range of 0.1-2 MeV and 19 pitch angle bins at 1 minute time intervals. The average flux, 90 degree flux and N value are included. Also included are the spacecraft geographic coordinates and altitude, L shell, and the local and equatorial magnetic field magnitudes from the 1977 Olson-Pfitzer model of the earth's geomagnetic field. The raw high resolution (0.512 sec) data and documentation of raw data can be found at: https://spdf.gsfc.nasa.gov/pub/data/crres/particle_mea/
Created May 2003
CSSWE is a 3U-CubeSat designed and developed by students at the University of Colorado at Boulder (CU-Boulder). The objective of the science mission is to address fundamental questions pertaining to the relationship between solar flares and energetic particles. These questions include the acceleration and loss mechanisms of outer radiation belt electrons. The goal is to measure differential fluxes of relativistic electrons in the energy range of 0.58-3.8 MeV and protons in 9-40 MeV. This project is a collaborative effort between the Laboratory for Atmospheric and Space Physics (LASP) and the Department of Aerospace Engineering Sciences (AES) at the University of Colorado, which includes the participation of students, faculty, and professional engineers. The science goals of the CSSWE mission are to study: How flare location, magnitude, and frequency relate to the timing, duration, and energy spectrum of SEPs reaching Earth. How the energy spectrum of radiation belt electrons evolve and how this evolution relates to the acceleration mechanism. To accomplish these goals CSSWE has a requirement for a minimum of 3 months of science operations based on expected flare and geomagnetic storm frequency. The first month of operations will be utilized for systems stabilization and check out.
Valid field reads 1 when additional processing is required. Reasons for Valid=1 are improper pointing, periods of high temperature, etc.
CSSWE is a 3U-CubeSat designed and developed by students at the University of Colorado at Boulder (CU-Boulder). The objective of the science mission is to address fundamental questions pertaining to the relationship between solar flares and energetic particles. These questions include the acceleration and loss mechanisms of outer radiation belt electrons. The goal is to measure differential fluxes of relativistic electrons in the energy range of 0.58-3.8 MeV and protons in 9-40 MeV. This project is a collaborative effort between the Laboratory for Atmospheric and Space Physics (LASP) and the Department of Aerospace Engineering Sciences (AES) at the University of Colorado, which includes the participation of students, faculty, and professional engineers. The science goals of the CSSWE mission are to study: How flare location, magnitude, and frequency relate to the timing, duration, and energy spectrum of SEPs reaching Earth. How the energy spectrum of radiation belt electrons evolve and how this evolution relates to the acceleration mechanism. To accomplish these goals CSSWE has a requirement for a minimum of 3 months of science operations based on expected flare and geomagnetic storm frequency. The first month of operations will be utilized for systems stabilization and check out.
Valid field reads 1 when additional processing is required. Reasons for Valid=1 are improper pointing, periods of high temperature, etc.
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997) NS S Southbound neutral sheet NT I Enter north tail lobe from inner magnetosphere ST O Leave south tail lobe for inner magnetosphere
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 13th generation pole used to calculate GSM latitude and MLT in PSE files produced after 23 Feb 2020. PSE files updated to support orbits >999 and six decimal figures on orbit phase from 25 March 2006.
JSOC predicted scientific events.