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CDAWeb Served Heliophysics Datasets Beginning with 'C'

C1_CP_FGM_SPIN: Cluster Spacecraft 1 FluxGate Magnetometer (FGM) Spin-Resolution Parameters
C1_JP_PMP: Cluster Spacecraft 1, JSOC Predicted Magnetic Positions - (Non-PI) M. Hapgood (RAL)
C1_JP_PSE: Cluster Spacecraft 1, JSOC Predicted Scientific Events - (Non-PI) M. Hapgood (RAL)
C1_PP_ASP: Cluster Spacecraft 1, ASPOC Prime Parameters - K. Torkar (IWF-OAW)
C1_PP_CIS: Cluster Spacecraft 1, CIS Prime Parameters - I. Dandouras (IRAP)
C1_PP_DWP: Cluster Spacecraft 1, DWP Prime Parameters - M. Balikhin (Univ-Sheff)
C1_PP_EDI: Cluster Spacecraft 1, EDI Prime Parameters - R. Torbert (UNH)
C1_PP_EFW: Cluster Spacecraft 1, EFW Prime Parameters - M. Andre (IRFU)
C1_PP_PEA: Cluster Spacecraft 1, PEACE Prime Parameters - A. Fazakerley (MSSL)
C1_PP_RAP: Cluster Spacecraft 1, RAPID Prime Parameters - P. W. Daly (MPI Solar System Research, Goettingen, Germany)
C1_PP_STA: Cluster Spacecraft 1, STAFF Prime Parameters - N. Cornilleau-Wehrlin (LPP)
C1_PP_WHI: Cluster Spacecraft 1, WHISPER Prime Parameters - J. G. Trotignon (LPC2E)
C1_UP_FGM: Cluster Spacecraft 1, FGM Unvalidated Prime Parameters - C. Carr (ICSTM)
C1_WAVEFORM_WBD: Cluster Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data - 2006 - Current: J. S. Pickett; 1988 - 2006: D. A. Gurnett (The University of Iowa)
C1_WAVEFORM_WBD_BM2: Cluster Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data - 2006 - Current: J. S. Pickett; 1988 - 2006: D. A. Gurnett (The University of Iowa)
C2_CP_FGM_SPIN: Cluster Spacecraft 2 FluxGate Magnetometer (FGM) Spin-Resolution Parameters
C2_JP_PMP: Cluster Spacecraft 2, JSOC Predicted Magnetic Positions - (Non-PI) M. Hapgood (RAL)
C2_JP_PSE: Cluster Spacecraft 2, JSOC Predicted Scientific Events - (Non-PI) M. Hapgood (RAL)
C2_PP_ASP: Cluster Spacecraft 2, ASPOC Prime Parameters - K. Torkar (IWF-OAW)
C2_PP_DWP: Cluster Spacecraft 2, DWP Prime Parameters - M. Balikhin (Univ-Sheff)
C2_PP_EDI: Cluster Spacecraft 2, EDI Prime Parameters - R. Torbert (UNH)
C2_PP_EFW: Cluster Spacecraft 2, EFW Prime Parameters - M. Andre (IRFU)
C2_PP_PEA: Cluster Spacecraft 2, PEACE Prime Parameters - A. Fazakerley (MSSL)
C2_PP_RAP: Cluster Spacecraft 2, RAPID Prime Parameters - P. W. Daly (MPI Solar System Research, Goettingen, Germany)
C2_PP_STA: Cluster Spacecraft 2, STAFF Prime Parameters - N. Cornilleau-Wehrlin (LPP)
C2_PP_WHI: Cluster Spacecraft 2, WHISPER Prime Parameters - J. G. Trotignon (LPC2E)
C2_UP_FGM: Cluster Spacecraft 2, FGM Unvalidated Prime Parameters - C. Carr (ICSTM)
C2_WAVEFORM_WBD: Cluster Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data - 2006 - Current: J. S. Pickett; 1988 - 2006: D. A. Gurnett (The University of Iowa)
C2_WAVEFORM_WBD_BM2: Cluster Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data - 2006 - Current: J. S. Pickett; 1988 - 2006: D. A. Gurnett (The University of Iowa)
C3_CP_FGM_SPIN: Cluster Spacecraft 3 FluxGate Magnetometer (FGM) Spin-Resolution Parameters
C3_JP_PMP: Cluster Spacecraft 3, JSOC Predicted Magnetic Positions - (Non-PI) M. Hapgood (RAL)
C3_JP_PSE: Cluster Spacecraft 3, JSOC Predicted Scientific Events - (Non-PI) M. Hapgood (RAL)
C3_PP_ASP: Cluster Spacecraft 3, ASPOC Prime Parameters - K. Torkar (IWF-OAW)
C3_PP_CIS: Cluster Spacecraft 3, CIS Prime Parameters - I. Dandouras (IRAP)
C3_PP_EDI: Cluster Spacecraft 3, EDI Prime Parameters - R. Torbert (UNH)
C3_PP_EFW: Cluster Spacecraft 3, EFW Prime Parameters - M. Andre (IRFU)
C3_PP_PEA: Cluster Spacecraft 3, PEACE Prime Parameters - A. Fazakerley (MSSL)
C3_PP_RAP: Cluster Spacecraft 3, RAPID Prime Parameters - P. W. Daly (MPI Solar System Research, Goettingen, Germany)
C3_PP_STA: Cluster Spacecraft 3, STAFF Prime Parameters - N. Cornilleau-Wehrlin (LPP)
C3_PP_WHI: Cluster Spacecraft 3, WHISPER Prime Parameters - J. G. Trotignon (LPC2E)
C3_UP_FGM: Cluster Spacecraft 3, FGM Unvalidated Prime Parameters - C. Carr (ICSTM)
C3_WAVEFORM_WBD: Cluster Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data - 2006 - Current: J. S. Pickett; 1988 - 2006: D. A. Gurnett (The University of Iowa)
C3_WAVEFORM_WBD_BM2: Cluster Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data - 2006 - Current: J. S. Pickett; 1988 - 2006: D. A. Gurnett (The University of Iowa)
C4_CP_FGM_SPIN: Cluster Spacecraft 4 FluxGate Magnetometer (FGM) Spin-Resolution Parameters
C4_JP_PMP: Cluster Spacecraft 4, JSOC Predicted Magnetic Positions - (Non-PI) M. Hapgood (RAL)
C4_JP_PSE: Cluster Spacecraft 4, JSOC Predicted Scientific Events - (Non-PI) M. Hapgood (RAL)
C4_PP_ASP: Cluster Spacecraft 4, ASPOC Prime Parameters - K. Torkar (IWF-OAW)
C4_PP_CIS: Cluster Spacecraft 4, CIS Prime Parameters - I. Dandouras (IRAP)
C4_PP_DWP: Cluster Spacecraft 4, DWP Prime Parameters - M. Balikhin (Univ-Sheff)
C4_PP_EDI: Cluster Spacecraft 4, EDI Prime Parameters - R. Torbert (UNH)
C4_PP_EFW: Cluster Spacecraft 4, EFW Prime Parameters - M. Andre (IRFU)
C4_PP_PEA: Cluster Spacecraft 4, PEACE Prime Parameters - A. Fazakerley (MSSL)
C4_PP_RAP: Cluster Spacecraft 4, RAPID Prime Parameters - P. W. Daly (MPI Solar System Research, Goettingen, Germany)
C4_PP_STA: Cluster Spacecraft 4, STAFF Prime Parameters - N. Cornilleau-Wehrlin (LPP)
C4_PP_WHI: Cluster Spacecraft 4, WHISPER Prime Parameters - J. G. Trotignon (LPC2E)
C4_UP_FGM: Cluster Spacecraft 4, FGM Unvalidated Prime Parameters - C. Carr (ICSTM)
C4_WAVEFORM_WBD: Cluster Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data - 2006 - Current: J. S. Pickett; 1988 - 2006: D. A. Gurnett (The University of Iowa)
C4_WAVEFORM_WBD_BM2: Cluster Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data - 2006 - Current: J. S. Pickett; 1988 - 2006: D. A. Gurnett (The University of Iowa)
CASSINI_HELIO1DAY_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)
CASSINI_MAG_1MIN_MAGNETIC_FIELD: 1 min averaged magnetic field - Michele Dougherty (Imperial College, London)
CL_JP_PCY: Cluster, JSOC Predicted Solar Cycle Trends - (Non-PI) M. Hapgood (RAL)
CL_JP_PGP: Cluster, JSOC Predicted Geometric Positions - (Non-PI) M. Hapgood (RAL)
CL_OR_GIFWALK: Link to Cluster orbit plots - Polar-Wind-Geotail Ground System (NASA GSFC)
CL_SP_AUX: Cluster, Auxiliary Parameters - (Non-PI) M. Tatrallyay (Wigner RCP, RMKI)
CNOFS_CINDI_IVM_500MS: CNOFS CINDI IVM ion density, composition, temperature, and drift (0.5-sec) - Dr. Roderick A. Heelis (University of Texas, Dallas)
CNOFS_PLP_PLASMA_1SEC: C/NOFS Planar Langmuir Probe 1 second average Key Parameters. "The data are PRELIMINARY, and as such, are intended for BROWSE PURPOSES ONLY" - D. E. Hunton (Air Force Research Laboratory, Space Vehicles Directorate)
CNOFS_VEFI_BFIELD_1SEC: Magnetic field solution (at 1 sample per sec) produced by VEFI on the Communication Navigation Outage Forecast System satellite. The data are PRELIMINARY, and as such, are intended for BROWSE PURPOSES ONLY. - Robert F. Pfaff (NASA GSFC)
CNOFS_VEFI_EFIELD_1SEC: Electric Field solution (at 1 sample/sec) produced by VEFI on the Communication Navigation Outage Forecast System satellite. The data are PRELIMINARY, and as such, are intended for BROWSE PURPOSES ONLY. - Robert F. Pfaff (GSFC)
CNOFS_VEFI_LD_500MS: CNOFS VEFI Lightning Detector, low rate data (eclipse portion of CNOFS orbit) - Robert H. Holzworth (University of Washington)
CN_K0_ASI: CANOPUS All Sky Imager, Key Parameters - J. Samson (U. Alberta)
CN_K0_BARS: CANOPUS Bistatic Auroral Radar System, Key Parameters - John Samson (University of Alberta)
CN_K0_MARI: CANOPUS MARI Magnetometer Key Parameters - J. Samson (U. Alberta)
CN_K0_MPA: CANOPUS Meridian Photometer Array, Key Parameters - J. Samson (U. Alberta)
CN_K1_MARI: CANOPUS MARI Riometer Key Parameters - J. Samson (U. Alberta)
COMETGS_HELIO1DAY_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)
COMETHMP_HELIO1DAY_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)
CRRES_H0_MEA: CRRES-MEA Data Archive - TBD (NSSDC)
CSSWE_REPTILE_6SEC-COUNTS-L1: CSSWE REPTile level1 6sec Counts and Position - Xinlin Li (University of Colorado at Boulder)
CSSWE_REPTILE_6SEC-FLUX-L2: CSSWE REPTile level2 6sec flux and Position - Xinlin Li (University of Colorado at Boulder)
CT_JP_PSE: Cluster centroid, JSOC Predicted Scientific Events - (Non-PI) M. Hapgood (RAL)

C1_CP_FGM_SPIN (spase://ESA/NumericalData/Cluster-Rumba/FGM/SpinResolution/PT4S)
Description
No TEXT global attribute value.
 
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C1_JP_PMP (spase://ESA/NumericalData/Cluster-Rumba/Ephemeris/JP/PredictedMagneticPosition/PT5M)
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79,
487-525 (1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF 11th generation used to calculate magnetic field and L value 
 in PMP files produced after 15 Oct 2010.
Caveats
JSOC predicted magnetic positions.
 
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C1_JP_PSE (spase://ESA/NumericalData/Cluster-Rumba/Ephemeris/JP/PredictedScientificEvent/PT0.016S)
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79,
487-525 (1997)
BS I Inbound bow shock - median ram pressure
BS O Outbound bow shock - median ram pressure
KX I Inbound L=2.4 value 1
KX O Outbound L=2.4 value 2
MP I Inbound magnetopause - median ram pressure
MP O Outbound magnetopause - median ram pressure
QL 2 Inbound critical L value 2 for auroral zone
QL B Outbound critical L value 2 for auroral zone
QL I Inbound critical L value for auroral zone
QL O Outbound critical L value for auroral zone
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
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF 10th generation pole used to calculate GSM latitude and MLT 
 in PSE files produced after 10 May 2005.
PSE files updated to support orbits >999 and six decimal figures 
 on orbit phase from 25 March 2006.
Caveats
JSOC predicted scientific events.
 
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C1_PP_ASP (spase://ESA/NumericalData/Cluster-Rumba/ASPOC/PrimeParameter/PT4S)
Description
K. Torkar et al, Active spacecraft potential control for Cluster -
implementation and first results
Ann. Geophys., 19,  pp 1289 - 1302, 2001)
Modification History
none
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
 
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C1_PP_CIS (spase://ESA/NumericalData/Cluster-Rumba/CIS/PrimeParameter/PT4S)
Description
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
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** C1_PP_CIS_20181231 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.
 
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C1_PP_DWP (spase://ESA/NumericalData/Cluster-Rumba/DWP/PrimeParameter/PT4S)
Description
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster
Space Sci. Rev., 79,  pp 209 - 231, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** C1_PP_DWP_20191030 HAS NOT BEEN VALIDATED - USE WITH CAUTION ***
This CSDS DWP product has not been validated prior to release.
 
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C1_PP_EDI (spase://ESA/NumericalData/Cluster-Rumba/EDI/PrimeParameter/PT4S)
Description
G. Paschmann et al, The Electron Drift Instrument for Cluster
Space Sci. Rev., 79,  pp 233 - 269, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
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.
 
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C1_PP_EFW (spase://ESA/NumericalData/Cluster-Rumba/EFW/PrimeParameter/PT4S)
Description
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster
Space Sci. Rev., 79,  pp 137 - 156, 1997)
Modification History
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
Caveats
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 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for E_pow_f1__C1_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for E_sigma__C1_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for U_probe_sc__C1_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
 
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C1_PP_PEA (spase://ESA/NumericalData/Cluster-Rumba/PEACE/PrimeParameter/PT4S)
Description
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment
Space Sci. Rev., 79,  pp 351 - 398, 1997)
Modification History
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
Caveats
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
 
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C1_PP_RAP (spase://ESA/NumericalData/Cluster-Rumba/RAPID/PrimeParameter/PT4S)
Description
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster
Space Sci. Rev., 79,  pp 399 - 473, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data processed on 2021-05-10T11:58:11Z
Caveats file: RAP_CAV_C1_V225.DAT; Release May 10, 2021
Caveats
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
 
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C1_PP_STA (spase://ESA/NumericalData/Cluster-Rumba/STAFF/PrimeParameter/PT4S)
Description
N. Cornilleau et al,
The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment
Space Sci. Rev., 79,  pp 107 - 136, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
PI Software Version 4.2, 25 September 2006
 
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C1_PP_WHI (spase://ESA/NumericalData/Cluster-Rumba/WHISPER/PrimeParameter/PT4S)
Description
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)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
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.
 
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C1_UP_FGM (spase://ESA/NumericalData/Cluster-Rumba/FGM/UnvalidatedParameter/PT4S)
Description
A. Balogh et al, The Cluster Magnetic Field Investigation
Space Sci. Rev., 79,  pp 65 - 92, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** C1_UP_FGM_20201231 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.
 
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C1_WAVEFORM_WBD (spase://ESA/NumericalData/Cluster-Rumba/WBD/PT0.0000046S)
Description
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 below for
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).
...
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.
...
Modification History
Created Mar 2008.Revised Dec 2008, Jan 2010
 
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C1_WAVEFORM_WBD_BM2 (spase://ESA/NumericalData/Cluster-Rumba/WBD/BM2/PT0.0000046S)
Description
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.
...
Modification History
Created Nov 2014.
 
Dataset in CDAWeb
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C2_CP_FGM_SPIN (spase://ESA/NumericalData/Cluster-Salsa/FGM/SpinResolution/PT4S)
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
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C2_JP_PMP (spase://ESA/NumericalData/Cluster-Salsa/Ephemeris/JP/PredictedMagneticPosition/PT5M)
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79,
487-525 (1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF 11th generation used to calculate magnetic field and L value 
 in PMP files produced after 15 Oct 2010.
Caveats
JSOC predicted magnetic positions.
 
Dataset in CDAWeb
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C2_JP_PSE (spase://ESA/NumericalData/Cluster-Salsa/Ephemeris/JP/PredictedScientificEvent/PT0.016S)
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79,
487-525 (1997)
BS I Inbound bow shock - median ram pressure
BS O Outbound bow shock - median ram pressure
MP I Inbound magnetopause - median ram pressure
MP O Outbound magnetopause - median ram pressure
QL I Inbound critical L value for auroral zone
QL O Outbound critical L value for auroral zone
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
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF 10th generation pole used to calculate GSM latitude and MLT 
 in PSE files produced after 10 May 2005.
PSE files updated to support orbits >999 and six decimal figures 
 on orbit phase from 25 March 2006.
Caveats
JSOC predicted scientific events.
 
Dataset in CDAWeb
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C2_PP_ASP (spase://ESA/NumericalData/Cluster-Salsa/ASPOC/PrimeParameter/PT4S)
Description
K. Torkar et al, Active spacecraft potential control for Cluster -
implementation and first results
Ann. Geophys., 19,  pp 1289 - 1302, 2001)
Modification History
none
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
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.
 
Dataset in CDAWeb
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C2_PP_DWP (spase://ESA/NumericalData/Cluster-Salsa/DWP/PrimeParameter/PT4S)
Description
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster
Space Sci. Rev., 79,  pp 209 - 231, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** C2_PP_DWP_20191031 HAS NOT BEEN VALIDATED - USE WITH CAUTION ***
This CSDS DWP product has not been validated prior to release.
 
Dataset in CDAWeb
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C2_PP_EDI (spase://ESA/NumericalData/Cluster-Salsa/EDI/PrimeParameter/PT4S)
Description
G. Paschmann et al, The Electron Drift Instrument for Cluster
Space Sci. Rev., 79,  pp 233 - 269, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
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
 
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C2_PP_EFW (spase://ESA/NumericalData/Cluster-Salsa/EFW/PrimeParameter/PT4S)
Description
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster
Space Sci. Rev., 79,  pp 137 - 156, 1997)
Modification History
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
Caveats
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 2019-12-31T04:26:00Z to 2019-12-31T06:15:00Z
Fill value inserted for E_sigma__C2_PP_EFW: No reason given
for time range 2019-12-31T04:26:00Z to 2019-12-31T06:15:00Z
Fill value inserted for E_dusk__C2_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for E_pow_f1__C2_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for E_sigma__C2_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for U_probe_sc__C2_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
 
Dataset in CDAWeb
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C2_PP_PEA (spase://ESA/NumericalData/Cluster-Salsa/PEACE/PrimeParameter/PT4S)
Description
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment
Space Sci. Rev., 79,  pp 351 - 398, 1997)
Modification History
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
Caveats
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
 
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C2_PP_RAP (spase://ESA/NumericalData/Cluster-Salsa/RAPID/PrimeParameter/PT4S)
Description
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster
Space Sci. Rev., 79,  pp 399 - 473, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data processed on 2021-05-10T11:58:12Z
Caveats file: RAP_CAV_C2_V225.DAT; Release May 10, 2021
Caveats
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
 
Dataset in CDAWeb
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C2_PP_STA (spase://ESA/NumericalData/Cluster-Salsa/STAFF/PrimeParameter/PT4S)
Description
N. Cornilleau et al,
The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment
Space Sci. Rev., 79,  pp 107 - 136, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
PI Software Version 4.2, 25 September 2006
 
Dataset in CDAWeb
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C2_PP_WHI (spase://ESA/NumericalData/Cluster-Salsa/WHISPER/PrimeParameter/PT4S)
Description
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)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
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.
 
Dataset in CDAWeb
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C2_UP_FGM (spase://ESA/NumericalData/Cluster-Salsa/FGM/UnvalidatedParameter/PT4S)
Description
A. Balogh et al, The Cluster Magnetic Field Investigation
Space Sci. Rev., 79,  pp 65 - 92, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** C2_UP_FGM_20210102 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.
 
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C2_WAVEFORM_WBD (spase://ESA/NumericalData/Cluster-Salsa/WBD/PT0.0000046S)
Description
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 below for
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).
...
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.
...
Modification History
Created Mar 2008.Revised Dec 2008, Jan 2010
 
Dataset in CDAWeb
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C2_WAVEFORM_WBD_BM2 (spase://ESA/NumericalData/Cluster-Salsa/WBD/BM2/PT0.0000046S)
Description
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.
...
Modification History
Created Nov 2014.
 
Dataset in CDAWeb
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C3_CP_FGM_SPIN (spase://ESA/NumericalData/Cluster-Samba/FGM/SpinResolution/PT4S)
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
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C3_JP_PMP (spase://ESA/NumericalData/Cluster-Samba/Ephemeris/JP/PredictedMagneticPosition/PT5M)
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79,
487-525 (1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF 11th generation used to calculate magnetic field and L value 
 in PMP files produced after 15 Oct 2010.
Caveats
JSOC predicted magnetic positions.
 
Dataset in CDAWeb
Python/ IDL  Data Access Code Examples
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C3_JP_PSE (spase://ESA/NumericalData/Cluster-Samba/Ephemeris/JP/PredictedScientificEvent/PT0.016S)
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79,
487-525 (1997)
BS I Inbound bow shock - median ram pressure
BS O Outbound bow shock - median ram pressure
MP I Inbound magnetopause - median ram pressure
MP O Outbound magnetopause - median ram pressure
QL I Inbound critical L value for auroral zone
QL O Outbound critical L value for auroral zone
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
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF 10th generation pole used to calculate GSM latitude and MLT 
 in PSE files produced after 10 May 2005.
PSE files updated to support orbits >999 and six decimal figures 
 on orbit phase from 25 March 2006.
Caveats
JSOC predicted scientific events.
 
Dataset in CDAWeb
Python/ IDL  Data Access Code Examples
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C3_PP_ASP (spase://ESA/NumericalData/Cluster-Samba/ASPOC/PrimeParameter/PT4S)
Description
K. Torkar et al, Active spacecraft potential control for Cluster -
implementation and first results
Ann. Geophys., 19,  pp 1289 - 1302, 2001)
Modification History
none
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
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.
 
Dataset in CDAWeb
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C3_PP_CIS (spase://ESA/NumericalData/Cluster-Samba/CIS/PrimeParameter/PT4S)
Description
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
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** C3_PP_CIS_20181231 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.
 
Dataset in CDAWeb
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C3_PP_EDI (spase://ESA/NumericalData/Cluster-Samba/EDI/PrimeParameter/PT4S)
Description
G. Paschmann et al, The Electron Drift Instrument for Cluster
Space Sci. Rev., 79,  pp 233 - 269, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
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.
 
Dataset in CDAWeb
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C3_PP_EFW (spase://ESA/NumericalData/Cluster-Samba/EFW/PrimeParameter/PT4S)
Description
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster
Space Sci. Rev., 79,  pp 137 - 156, 1997)
Modification History
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
Caveats
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__C3_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for E_pow_f1__C3_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for E_sigma__C3_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for U_probe_sc__C3_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
 
Dataset in CDAWeb
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C3_PP_PEA (spase://ESA/NumericalData/Cluster-Samba/PEACE/PrimeParameter/PT4S)
Description
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment
Space Sci. Rev., 79,  pp 351 - 398, 1997)
Modification History
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
Caveats
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
 
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C3_PP_RAP (spase://ESA/NumericalData/Cluster-Samba/RAPID/PrimeParameter/PT4S)
Description
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster
Space Sci. Rev., 79,  pp 399 - 473, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data processed on 2021-05-10T11:58:13Z
Caveats file: RAP_CAV_C3_V225.DAT; Release May 10, 2021
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
2021-01-31T17:43:00.000Z/2021-01-31T22:03:00.000Z: Switch to internal clock, no
time stamps possible, data suppressed.
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
2021-01-31T17:41:36Z/2021-01-31T22:04:09Z: Sun pulses missing, no time stamps,
no data.
2021-01-31T22:04:04Z/2021-01-31T23:59:59Z: Patches are inactive, data
unreliable.
 
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C3_PP_STA (spase://ESA/NumericalData/Cluster-Samba/STAFF/PrimeParameter/PT4S)
Description
N. Cornilleau et al,
The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment
Space Sci. Rev., 79,  pp 107 - 136, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
PI Software Version 4.2, 25 September 2006
 
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C3_PP_WHI (spase://ESA/NumericalData/Cluster-Samba/WHISPER/PrimeParameter/PT4S)
Description
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)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
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.
 
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C3_UP_FGM (spase://ESA/NumericalData/Cluster-Samba/FGM/UnvalidatedParameter/PT4S)
Description
A. Balogh et al, The Cluster Magnetic Field Investigation
Space Sci. Rev., 79,  pp 65 - 92, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** C3_UP_FGM_20210101 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.
 
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C3_WAVEFORM_WBD (spase://ESA/NumericalData/Cluster-Samba/WBD/PT0.0000046S)
Description
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 below for
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).
...
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.
...
Modification History
Created Mar 2008.Revised Dec 2008, Jan 2010
 
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C3_WAVEFORM_WBD_BM2 (spase://ESA/NumericalData/Cluster-Samba/WBD/BM2/PT0.0000046S)
Description
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.
...
Modification History
Created Nov 2014.
 
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C4_CP_FGM_SPIN (spase://ESA/NumericalData/Cluster-Tango/FGM/SpinResolution/PT4S)
Description
No TEXT global attribute value.
 
Dataset in CDAWeb
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C4_JP_PMP (spase://ESA/NumericalData/Cluster-Tango/Ephemeris/JP/PredictedMagneticPosition/PT5M)
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79,
487-525 (1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF 11th generation used to calculate magnetic field and L value 
 in PMP files produced after 15 Oct 2010.
Caveats
JSOC predicted magnetic positions.
 
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C4_JP_PSE (spase://ESA/NumericalData/Cluster-Tango/Ephemeris/JP/PredictedScientificEvent/PT0.016S)
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79,
487-525 (1997)
BS I Inbound bow shock - median ram pressure
BS O Outbound bow shock - median ram pressure
MP I Inbound magnetopause - median ram pressure
MP O Outbound magnetopause - median ram pressure
QL 2 Inbound critical L value 2 for auroral zone
QL B Outbound critical L value 2 for auroral zone
QL I Inbound critical L value for auroral zone
QL O Outbound critical L value for auroral zone
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
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF 10th generation pole used to calculate GSM latitude and MLT 
 in PSE files produced after 10 May 2005.
PSE files updated to support orbits >999 and six decimal figures 
 on orbit phase from 25 March 2006.
Caveats
JSOC predicted scientific events.
 
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C4_PP_ASP (spase://ESA/NumericalData/Cluster-Tango/ASPOC/PrimeParameter/PT4S)
Description
K. Torkar et al, Active spacecraft potential control for Cluster -
implementation and first results
Ann. Geophys., 19,  pp 1289 - 1302, 2001)
Modification History
none
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
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.
 
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C4_PP_CIS (spase://ESA/NumericalData/Cluster-Tango/CIS/PrimeParameter/PT4S)
Description
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
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** C4_PP_CIS_20181231 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.
 
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C4_PP_DWP (spase://ESA/NumericalData/Cluster-Tango/DWP/PrimeParameter/PT4S)
Description
L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster
Space Sci. Rev., 79,  pp 209 - 231, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** C4_PP_DWP_20191031 HAS NOT BEEN VALIDATED - USE WITH CAUTION ***
This CSDS DWP product has not been validated prior to release.
 
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C4_PP_EDI (spase://ESA/NumericalData/Cluster-Tango/EDI/PrimeParameter/PT4S)
Description
G. Paschmann et al, The Electron Drift Instrument for Cluster
Space Sci. Rev., 79,  pp 233 - 269, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
C4 EDI switched off
 
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C4_PP_EFW (spase://ESA/NumericalData/Cluster-Tango/EFW/PrimeParameter/PT4S)
Description
G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster
Space Sci. Rev., 79,  pp 137 - 156, 1997)
Modification History
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
Caveats
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 2019-12-31T06:44:00Z to 2019-12-31T23:20:00Z
Fill value inserted for E_sigma__C4_PP_EFW: No reason given
for time range 2019-12-31T06:44:00Z to 2019-12-31T23:20:00Z
Fill value inserted for E_dusk__C4_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for E_pow_f1__C4_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for E_sigma__C4_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
Fill value inserted for U_probe_sc__C4_PP_EFW: No reason given
for time range 2019-12-31T21:07:00Z to 2019-12-31T21:10:00Z
 
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C4_PP_PEA (spase://ESA/NumericalData/Cluster-Tango/PEACE/PrimeParameter/PT4S)
Description
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment
Space Sci. Rev., 79,  pp 351 - 398, 1997)
Modification History
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
Caveats
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
 
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C4_PP_RAP (spase://ESA/NumericalData/Cluster-Tango/RAPID/PrimeParameter/PT4S)
Description
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster
Space Sci. Rev., 79,  pp 399 - 473, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Data processed on 2021-05-10T11:58:18Z
Caveats file: RAP_CAV_C4_V225.DAT; Release May 10, 2021
Caveats
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
 
Dataset in CDAWeb
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C4_PP_STA (spase://ESA/NumericalData/Cluster-Tango/STAFF/PrimeParameter/PT4S)
Description
N. Cornilleau et al,
The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment
Space Sci. Rev., 79,  pp 107 - 136, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
PI Software Version 4.2, 25 September 2006
 
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C4_PP_WHI (spase://ESA/NumericalData/Cluster-Tango/WHISPER/PrimeParameter/PT4S)
Description
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)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Caveats
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.
 
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C4_UP_FGM (spase://ESA/NumericalData/Cluster-Tango/FGM/UnvalidatedParameter/PT4S)
Description
A. Balogh et al, The Cluster Magnetic Field Investigation
Space Sci. Rev., 79,  pp 65 - 92, 1997)
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
Operational version of UKCDHF Pipeline software
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
*** C4_UP_FGM_20210101 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.
 
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C4_WAVEFORM_WBD (spase://ESA/NumericalData/Cluster-Tango/WBD/PT0.0000046S)
Description
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 below for
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).
...
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.
...
Modification History
Created Mar 2008.Revised Dec 2008, Jan 2010
 
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C4_WAVEFORM_WBD_BM2 (spase://ESA/NumericalData/Cluster-Tango/WBD/BM2/PT0.0000046S)
Description
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.
...
Modification History
Created Nov 2014.
 
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CASSINI_HELIO1DAY_POSITION (spase://NASA/NumericalData/Cassini/HelioWeb/Ephemeris/P1D)
Description
No TEXT global attribute value.
 
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CASSINI_MAG_1MIN_MAGNETIC_FIELD (spase://NASA/NumericalData/Cassini/MAG/CDF/PT1M)
Description
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
 
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CL_JP_PCY (spase://ESA/NumericalData/Cluster/JSOC/Predicted/SolarCycle/P1M)
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79,
487-525 (1997)
Modification History
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.
Caveats
JSOC predicted Solar cycle trends.
Please acknowledge sunspot numbers as:
Source: WDC-SILSO, Royal Observatory of Belgium, Brussels.
 
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CL_JP_PGP (spase://ESA/NumericalData/Cluster/Ephemeris/JP/PredictedGeometricPosition/PT5M)
Description
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.
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF 11th generation pole used to calculate dipole tilt and GSE-GSM 
 angle in PGP files produced after 15 Oct 2010.
Orbit number field supports 4-digit orbits and 6 figure phase 
 in PGP files produced after 20 March 2006.
Caveats
JSOC predicted Orbits.
 Using spacecraft C3 as reference spacecraft.
 
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CL_OR_GIFWALK
Description
Pre-generated PWG plots
 
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CL_SP_AUX (spase://ESA/NumericalData/Cluster/Ephemeris/SummaryParameter/PT60S)
Description
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.
Modification History
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
Caveats
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
 
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CNOFS_CINDI_IVM_500MS (spase://NASA/NumericalData/CNOFS/CINDI/IVM/PT0.5S)
Description
 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.
 
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CNOFS_PLP_PLASMA_1SEC (spase://NASA/NumericalData/CNOFS/PLP/PT1S)
Description
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.
 
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CNOFS_VEFI_BFIELD_1SEC (spase://NASA/NumericalData/CNOFS/VEFI/BField/PT1S)
Description
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 using 16 bit A/D converters at 1 sample per
sec with a range of .. 45,000 nT.  Its primary objective on the CNOFS spacecraft
is to enable an accurate V x B measurement along the spacecraft trajectory.  In
order to provide an in-flight calibration of the magnetic field data, we compare
the most recent POMME model (the POtsdam Magnetic Model of the Earth,
http://geomag.org/models/pomme6.html) with the actual magnetometer measurements
to help determine a set of calibration parameters for the gains, offsets, and
non-orthogonality matrix of the sensor axes.  The calibrated magnetic field
measurements are provided in the data file.  The data is PRELIMINARY, and as
such, is intended for BROWSE PURPOSES ONLY.  Registering your email will allow
notification of updates.. . . 
 
 
 
 
 
 
 
 
 
 
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CNOFS_VEFI_EFIELD_1SEC (spase://NASA/NumericalData/CNOFS/VEFI/EField/PT1S)
Description
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.
 
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CNOFS_VEFI_LD_500MS (spase://NASA/NumericalData/CNOFS/VEFI/Lightning/PT0.5S)
Description
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
 
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CN_K0_ASI (spase://GBO/NumericalData/CANOPUS/ASI/KeyParameter/K0/PT1M)
Description
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.
Modification History
Created 31-DEC-1999
 
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CN_K0_BARS (spase://GBO/NumericalData/CANOPUS/BARS/KeyParameter/K0/PT1M)
Description
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.
Modification History
Created  3-OCT-1994
 
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CN_K0_MARI (spase://GBO/NumericalData/CANOPUS/MARI/PT60S)
Description
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.
Modification History
Created 31-DEC-1999
Added station Taloyoak on 29-SEP-1994
 
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CN_K0_MPA (spase://GBO/NumericalData/CANOPUS/MPA/KeyParameter/K0/PT1M)
Description
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.
Modification History
Created 31-DEC-1999
 
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CN_K1_MARI (spase://GBO/NumericalData/CANOPUS/MARI/KeyParameter/K1/PT1M)
Description
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.
Modification History
Created 31-DEC-1999
 
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COMETGS_HELIO1DAY_POSITION (spase://NASA/NumericalData/Comet/GriggSkjellerup/HelioWeb/Ephemeris/P1D)
Description
No TEXT global attribute value.
 
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COMETHMP_HELIO1DAY_POSITION (spase://NASA/NumericalData/Comet/HondaMrkosPajdusakova/HelioWeb/Ephemeris/P1D)
Description
No TEXT global attribute value.
 
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CRRES_H0_MEA (spase://NASA/NumericalData/CRRES/MEA/PT1M)
Description
CRRES MEA DataArchive         
This is the re-processed version of the   MEA data archive from the CRRES   
spacecraft.  The raw data from the NOAA archive 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 fulx 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 a model of the earth's geomagnetic
field.                            The raw high resolution (0.512 sec) data and
documentation of raw data can be found
at:ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/crres/particle_mea.
Modification History
Created May 2003
 
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CSSWE_REPTILE_6SEC-COUNTS-L1 (spase://NASA/NumericalData/CubeSat/CSSWE/REPTile/L1/Counts/PT6S)
Description
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.
 
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CSSWE_REPTILE_6SEC-FLUX-L2 (spase://NASA/NumericalData/CubeSat/CSSWE/REPTile/L2/Flux/PT6S)
Description
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.
 
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CT_JP_PSE (spase://ESA/NumericalData/Cluster/Ephemeris/JP/PredictedScientificEvent/PT5M)
Description
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79,
487-525 (1997)
B+ I Inbound bow shock - upper sextile ram pressure
B+ O Outbound bow shock - upper sextile ram pressure
B- I Inbound bow shock - lower sextile ram pressure
B- O Outbound bow shock - lower sextile ram pressure
BS I Inbound bow shock - median ram pressure
BS O Outbound bow shock - median ram pressure
M+ I Inbound magnetopause - upper sextile ram pressure
M+ O Outbound magnetopause - upper sextile ram pressure
M- I Inbound magnetopause - lower sextile ram pressure
M- O Outbound magnetopause - lower sextile ram pressure
MP I Inbound magnetopause - median ram pressure
MP O Outbound magnetopause - median ram pressure
Modification History
Produced in accordance with CSDS file specification
Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
IGRF 10th generation pole used to calculate GSM latitude and MLT 
 in PSE files produced after 10 May 2005.
PSE files updated to support orbits >999 and six decimal figures 
 on orbit phase from 25 March 2006.
Caveats
JSOC predicted scientific events.
 
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