No TEXT global attribute value.
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M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
JSOC predicted magnetic positions.
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M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997) AP _ Apogee CY 1 Start of visibility window at Canberra (5 deg elevation) CY 2 Start of visibility window at Canberra (5 deg elevation) CY 3 Start of visibility window at Canberra (5 deg elevation) CZ 1 End of visibility window at Canberra (5 deg elevation) CZ 2 End of visibility window at Canberra (5 deg elevation) CZ 3 End of visibility window at Canberra (5 deg elevation) CZ 4 End of visibility window at Canberra (5 deg elevation) DY 1 Start of visibility window at Vilspa (5 deg elevation) DY 2 Start of visibility window at Vilspa (5 deg elevation) DY 3 Start of visibility window at Vilspa (5 deg elevation) DY 4 Start of visibility window at Vilspa (5 deg elevation) DY 5 Start of visibility window at Vilspa (5 deg elevation) DZ 1 End of visibility window at Vilspa (5 deg elevation) DZ 2 End of visibility window at Vilspa (5 deg elevation) DZ 3 End of visibility window at Vilspa (5 deg elevation) DZ 4 End of visibility window at Vilspa (5 deg elevation) GY 1 Start of visibility window at Goldstone (5 deg elevation) GY 2 Start of visibility window at Goldstone (5 deg elevation) GY 3 Start of visibility window at Goldstone (5 deg elevation) GY 4 Start of visibility window at Goldstone (5 deg elevation) GZ 1 End of visibility window at Goldstone (5 deg elevation) GZ 2 End of visibility window at Goldstone (5 deg elevation) GZ 3 End of visibility window at Goldstone (5 deg elevation) JY 1 Start of visibility window at Maspalomas (5 deg elevation) JY 2 Start of visibility window at Maspalomas (5 deg elevation) JY 3 Start of visibility window at Maspalomas (5 deg elevation) JY 4 Start of visibility window at Maspalomas (5 deg elevation) JZ 1 End of visibility window at Maspalomas (5 deg elevation) JZ 2 End of visibility window at Maspalomas (5 deg elevation) JZ 3 End of visibility window at Maspalomas (5 deg elevation) KA 1 Start of visibility window at Kourou (5 deg elevation) KA 2 Start of visibility window at Kourou (5 deg elevation) KA 3 Start of visibility window at Kourou (5 deg elevation) KA 4 Start of visibility window at Kourou (5 deg elevation) KL 1 End of visibility window at Kourou (5 deg elevation) KL 2 End of visibility window at Kourou (5 deg elevation) KL 3 End of visibility window at Kourou (5 deg elevation) KL 4 End of visibility window at Kourou (5 deg elevation) MY 1 Start of visibility window at Madrid (5 deg elevation) MY 2 Start of visibility window at Madrid (5 deg elevation) MY 3 Start of visibility window at Madrid (5 deg elevation) MY 4 Start of visibility window at Madrid (5 deg elevation) MZ 1 End of visibility window at Madrid (5 deg elevation) MZ 2 End of visibility window at Madrid (5 deg elevation) MZ 3 End of visibility window at Madrid (5 deg elevation) NS S Southbound neutral sheet NT I Enter north tail lobe from inner magnetosphere PA 1 Start of visibility window at Perth (5 deg elevation) PA 2 Start of visibility window at Perth (5 deg elevation) PA 3 Start of visibility window at Perth (5 deg elevation) PA 4 Start of visibility window at Perth (5 deg elevation) PE _ Perigee PL 1 End of visibility window at Perth (5 deg elevation) PL 2 End of visibility window at Perth (5 deg elevation) PL 3 End of visibility window at Perth (5 deg elevation) PL 4 End of visibility window at Perth (5 deg elevation) PL 5 End of visibility window at Perth (5 deg elevation) QL I Inbound critical L value for auroral zone QL O Outbound critical L value for auroral zone RA 1 Start of visibility window at Redu (5 deg elevation) RA 2 Start of visibility window at Redu (5 deg elevation) RA 3 Start of visibility window at Redu (5 deg elevation) RA 4 Start of visibility window at Redu (5 deg elevation) RL 1 End of visibility window at Redu (5 deg elevation) RL 2 End of visibility window at Redu (5 deg elevation) RL 3 End of visibility window at Redu (5 deg elevation) RL 4 End of visibility window at Redu (5 deg elevation) RL 5 End of visibility window at Redu (5 deg elevation) ST O Leave south tail lobe for inner magnetosphere TL I Inbound radiation belt entry for WEC TL O Outbound radiation belt exit for WEC VL I Inbound critical L value for EDI VL O Outbound critical L value for EDI XL I Inbound critical L value for PEACE XL O Outbound critical L value for PEACE YL I Inbound critical L value for RAPID YL O Outbound critical L value for RAPID ZL I Inbound critical L value for CIS ZL O Outbound critical L value for CIS
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF2000 pole used to calculate GSM latitude and MLT in PSE files produced after 25 June 2001.
JSOC predicted scientific events.
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K. Torkar et al, Active spacecraft potential control for Cluster - implementation and first results Ann. Geophys., 19, pp 1289 - 1302, 2001)
none Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
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H. Reme et al, First multispacecraft ion measurements in and near the Earth's magnetosphere with the identical Cluster Ion Spectrometry (CIS) experiment Annales Geophysicae, 19, pp 1303 - 1354, 2001
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats The user of the CIS data needs to be cautious. Please refer to the CIS Home Page: http://cis.cesr.fr:8000/CIS_sw_home-en.htm , link "Caveats for the CIS data", for caveats concerning these data.
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L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster Space Sci. Rev., 79, pp 209 - 231, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Refer to the PI or NDC for access to ongoing caveat information Use correlator data with caution Status set to 0: WEC powered off for time range 2008-07-31T15:15:06Z to 2008-07-31T23:59:59Z
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G. Paschmann et al, The Electron Drift Instrument for Cluster Space Sci. Rev., 79, pp 233 - 269, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats 1) EDI's automated analysis algorithm has a known susceptibility to producing occasional incorrect values of the drift velocities (and electric fields). The code attempts to prevent these bad values to be output to the cdf file. No further removal is done in the validation process. 2) When drift velocities become sufficiently large, there can be a 180-degree ambiguity in drift direction that is usually flagged in bit 7 (counting from 0) of Status Byte 3. 3) There are two methods to analyze a spin's worth of EDI data. If bits 5 6 in Status Byte 3 are NOT set, the employed method was triangulation. If either bit 5 or 6 are set, then the results are from time-of-flight analysis. 4) The reported drift velocities and electric field refer to inertial coordinates, i.e., have been corrected for spacecraft velocity. However, the magnitude errors (in %) and the angle errors (in degrees), reported in Status Bytes 5 & 6, respectively, refer to the spacecraft frame and have NOT yet been converted to inertial coordinates. 5) The reduced chi-square reported as a data word is a measure of the goodness-of-fit of the triangulation analysis.
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G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster Space Sci. Rev., 79, pp 137 - 156, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data calibration may be unreliable at this early stage of the mission
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CSDS data are not for publication *** Be aware that data may be reprocessed as necessary to improve quality For questions on data validity please contact sdc-adm@plasma.kth.se Fill value inserted for E_dusk__C1_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_pow_f1__C1_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_sigma__C1_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for U_probe_sc__C1_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z
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A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CAUTION Preliminary calibrations used: not for publication ***
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A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment Space Sci. Rev., 79, pp 351 - 398, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 PP & SP data is generated at MSSL, then provided to UK-CDHF
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats This is PEACE PP/SP data version 3.1, produced at MSSL Based on onboard moments but using corrected geometric factors which account for uplinked changes of the values used in onboard calibration as well as estimated changes due to variable MCP gain performance Onboard moments are calculated for up to three energy ranges. Photoelectron contamination may affect 0, 1 or 2 of these ranges EFW PP probe-spacecraft potential was used to select the energy ranges to be excluded to remove misleading photoelectron contributions. Note that the density may be underestimated if there are both plasma electrons and photoelectrons in the lowest energy range When 88h58 is used for the HEEA sensor, sometimes the entire plasma electron population and photoelectrons are in just the lowest of the 3 energy ranges. This data has been deleted in this release of the PEACE PPs Data is deleted if the spacecraft electric potential is too large for the simple correction procedure to work or there is no EFW PP data available Measured electron energies have not been corrected for their acceleration by the spacecraft electric potential Onboard moments use onboard energy tables, efficiencies and response surfaces. Any errors in these parameters cannot be corrected in ground data processing Before 2001-09-11 the onboard energy efficiencies were not accurate, which caused the density in the solar wind to be overestimated. This data has been removed in this release of the PEACE PPs The calculation of T_par, T_perp and Q_par used PP FGM data The data is for context and information only. It is not suitable for detailed analysis, but may be used for event selection The next iteration of PP/SP moments will be of a higher quality Please see links under http://www.mssl.ucl.ac.uk/www_plasma/missions/cluster/clusterII.html for more information Please contact the PEACE PI to request science quality data Automatically validated by UKCDC Product delivered pre-validated by the PI institute
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B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster Space Sci. Rev., 79, pp 399 - 473, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data processed on 2009-02-06T07:49:36Z Caveats file: RAP_CAV_C1_V109.DAT; Release Feb 5, 2009
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats RAPID Data produced with best-effort general calibration files. Corrected: error that made ion fluxes 50% too large in 2006-2008 data. 1901-01-01T00:00:00.000Z/9999-12-31T23:59:59.999Z: Electrons: lowest energy channel needs correction for reduced sensitivity. 2001-09-13T00:00:00.000Z/9999-12-31T23:59:59.000Z: Central ion head not functioning since 2001-09-13, no sensitivity near ecliptic. 2007-03-16T06:00:00.000Z/9999-12-31T23:59:59.000Z: IIMS stops functioning since 2007-03-16, no ion data. Corrected time stamps for ions and electrons. Energy threshold shifts have been applied. Changed EDB format, on-board anisotropies not possible in NM 2008-12-31T15:19:43Z/2008-12-31T15:20:39Z: Sun pulses missing, no time stamps, no data.
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N. Cornilleau et al, The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment Space Sci. Rev., 79, pp 107 - 136, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats PI Software Version 4.1, 27 March 2006
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P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser: Performances and Perspectives for the Cluster Mission Space Sci. Rev., 79, pp 157 - 193, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Two types of parameters are provided by WHISPER: 1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding operations. The N_e_res value is calculated from an algorithm for resonance recognition, which cannot take account of all level of information available to the experimenter. The reliability of N_e_res parameters derived at the CSDS level is thus limited in an unknown manner. The N_e_res_q parameter (one value for each N_e_res data point) provides a crude idea of the probability that the N_e_res value is actually correct. A value of 0 means that the value is probably wrong, a value above 80 that it is probably correct. Anything in between reflects a crude evaluation of the chances. Refer to PI for details. 2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are related to recording of natural wave emissions. Those parameters, not affected by variations in instrument's transfer functions, are globally OK. However, two factors can affect the precision of the measurements: a) the occasional presence of spurious emissions created by operations of the EDI instrument increases the wave power values measured on SC1, SC2 and SC3, from an unknown amount, b) the limited dynamical range of the instrument leads to an underestimation of the E_pow parameters values when the voltage difference measured by the double sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp (depending of the gain chosen). As a consequence, high values have to be taken with special caution.
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A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C1_UP_FGM_20080930 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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No TEXT global attribute value.
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M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
JSOC predicted magnetic positions.
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M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997) AP _ Apogee CY 1 Start of visibility window at Canberra (5 deg elevation) CY 2 Start of visibility window at Canberra (5 deg elevation) CY 3 Start of visibility window at Canberra (5 deg elevation) CZ 1 End of visibility window at Canberra (5 deg elevation) CZ 2 End of visibility window at Canberra (5 deg elevation) CZ 3 End of visibility window at Canberra (5 deg elevation) CZ 4 End of visibility window at Canberra (5 deg elevation) DY 1 Start of visibility window at Vilspa (5 deg elevation) DY 2 Start of visibility window at Vilspa (5 deg elevation) DY 3 Start of visibility window at Vilspa (5 deg elevation) DY 4 Start of visibility window at Vilspa (5 deg elevation) DZ 1 End of visibility window at Vilspa (5 deg elevation) DZ 2 End of visibility window at Vilspa (5 deg elevation) DZ 3 End of visibility window at Vilspa (5 deg elevation) GY 1 Start of visibility window at Goldstone (5 deg elevation) GY 2 Start of visibility window at Goldstone (5 deg elevation) GY 3 Start of visibility window at Goldstone (5 deg elevation) GY 4 Start of visibility window at Goldstone (5 deg elevation) GZ 1 End of visibility window at Goldstone (5 deg elevation) GZ 2 End of visibility window at Goldstone (5 deg elevation) GZ 3 End of visibility window at Goldstone (5 deg elevation) JY 1 Start of visibility window at Maspalomas (5 deg elevation) JY 2 Start of visibility window at Maspalomas (5 deg elevation) JY 3 Start of visibility window at Maspalomas (5 deg elevation) JY 4 Start of visibility window at Maspalomas (5 deg elevation) JZ 1 End of visibility window at Maspalomas (5 deg elevation) JZ 2 End of visibility window at Maspalomas (5 deg elevation) JZ 3 End of visibility window at Maspalomas (5 deg elevation) KA 1 Start of visibility window at Kourou (5 deg elevation) KA 2 Start of visibility window at Kourou (5 deg elevation) KA 3 Start of visibility window at Kourou (5 deg elevation) KA 4 Start of visibility window at Kourou (5 deg elevation) KL 1 End of visibility window at Kourou (5 deg elevation) KL 2 End of visibility window at Kourou (5 deg elevation) KL 3 End of visibility window at Kourou (5 deg elevation) KL 4 End of visibility window at Kourou (5 deg elevation) MY 1 Start of visibility window at Madrid (5 deg elevation) MY 2 Start of visibility window at Madrid (5 deg elevation) MY 3 Start of visibility window at Madrid (5 deg elevation) MY 4 Start of visibility window at Madrid (5 deg elevation) MZ 1 End of visibility window at Madrid (5 deg elevation) MZ 2 End of visibility window at Madrid (5 deg elevation) MZ 3 End of visibility window at Madrid (5 deg elevation) NS S Southbound neutral sheet NT I Enter north tail lobe from inner magnetosphere PA 1 Start of visibility window at Perth (5 deg elevation) PA 2 Start of visibility window at Perth (5 deg elevation) PA 3 Start of visibility window at Perth (5 deg elevation) PE _ Perigee PL 1 End of visibility window at Perth (5 deg elevation) PL 2 End of visibility window at Perth (5 deg elevation) PL 3 End of visibility window at Perth (5 deg elevation) PL 4 End of visibility window at Perth (5 deg elevation) QL I Inbound critical L value for auroral zone QL O Outbound critical L value for auroral zone RA 1 Start of visibility window at Redu (5 deg elevation) RA 2 Start of visibility window at Redu (5 deg elevation) RA 3 Start of visibility window at Redu (5 deg elevation) RA 4 Start of visibility window at Redu (5 deg elevation) RL 1 End of visibility window at Redu (5 deg elevation) RL 2 End of visibility window at Redu (5 deg elevation) RL 3 End of visibility window at Redu (5 deg elevation) RL 4 End of visibility window at Redu (5 deg elevation) ST O Leave south tail lobe for inner magnetosphere TL I Inbound radiation belt entry for WEC TL O Outbound radiation belt exit for WEC VL I Inbound critical L value for EDI VL O Outbound critical L value for EDI WL I Inbound critical L value for ASPOC WL O Outbound critical L value for ASPOC XL I Inbound critical L value for PEACE XL O Outbound critical L value for PEACE YL I Inbound critical L value for RAPID YL O Outbound critical L value for RAPID ZL I Inbound critical L value for CIS ZL O Outbound critical L value for CIS
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF2000 pole used to calculate GSM latitude and MLT in PSE files produced after 25 June 2001.
JSOC predicted scientific events.
Back to top
K. Torkar et al, Active spacecraft potential control for Cluster - implementation and first results Ann. Geophys., 19, pp 1289 - 1302, 2001)
none Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats One raw data format (5.1.5 secs) of bad data may occur when the instrument is powered on.
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H. Reme et al, First multispacecraft ion measurements in and near the Earth's magnetosphere with the identical Cluster Ion Spectrometry (CIS) experiment Annales Geophysicae, 19, pp 1303 - 1354, 2001
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats CIS Switched-OFF on this s/c
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L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster Space Sci. Rev., 79, pp 209 - 231, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Refer to the PI or NDC for access to ongoing caveat information Use correlator data with caution
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G. Paschmann et al, The Electron Drift Instrument for Cluster Space Sci. Rev., 79, pp 233 - 269, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
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G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster Space Sci. Rev., 79, pp 137 - 156, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data calibration may be unreliable at this early stage of the mission
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CSDS data are not for publication *** Be aware that data may be reprocessed as necessary to improve quality For questions on data validity please contact sdc-adm@plasma.kth.se Fill value inserted for E_dusk__C2_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_pow_f1__C2_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_sigma__C2_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for U_probe_sc__C2_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z
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A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software WARNING - No Sun Pulse - Spin Phase is Invalid No FGM science data available
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C2_PP_FGM_20080210 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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A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment Space Sci. Rev., 79, pp 351 - 398, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 PP & SP data is generated at MSSL, then provided to UK-CDHF
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats This is PEACE PP/SP data version 3.1, produced at MSSL Based on onboard moments but using corrected geometric factors which account for uplinked changes of the values used in onboard calibration as well as estimated changes due to variable MCP gain performance Onboard moments are calculated for up to three energy ranges. Photoelectron contamination may affect 0, 1 or 2 of these ranges EFW PP probe-spacecraft potential was used to select the energy ranges to be excluded to remove misleading photoelectron contributions. Note that the density may be underestimated if there are both plasma electrons and photoelectrons in the lowest energy range When 88h58 is used for the HEEA sensor, sometimes the entire plasma electron population and photoelectrons are in just the lowest of the 3 energy ranges. This data has been deleted in this release of the PEACE PPs Data is deleted if the spacecraft electric potential is too large for the simple correction procedure to work or there is no EFW PP data available Measured electron energies have not been corrected for their acceleration by the spacecraft electric potential Onboard moments use onboard energy tables, efficiencies and response surfaces. Any errors in these parameters cannot be corrected in ground data processing Before 2001-09-11 the onboard energy efficiencies were not accurate, which caused the density in the solar wind to be overestimated. This data has been removed in this release of the PEACE PPs The calculation of T_par, T_perp and Q_par used PP FGM data The data is for context and information only. It is not suitable for detailed analysis, but may be used for event selection The next iteration of PP/SP moments will be of a higher quality Please see links under http://www.mssl.ucl.ac.uk/www_plasma/missions/cluster/clusterII.html for more information Please contact the PEACE PI to request science quality data Automatically validated by UKCDC Product delivered pre-validated by the PI institute
Back to top
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster Space Sci. Rev., 79, pp 399 - 473, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data processed on 2009-02-06T07:49:44Z Caveats file: RAP_CAV_C2_V109.DAT; Release Feb 5, 2009
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats RAPID Data produced with best-effort general calibration files. Corrected: error that made ion fluxes 50% too large in 2006-2008 data. 1901-01-01T00:00:00.000Z/9999-12-31T23:59:59.999Z: Electrons: lowest energy channel needs correction for reduced sensitivity. 2001-01-12T00:00:00.000Z/9999-12-31T23:59:59.000Z: Central ion head not functioning since 2001-01-12, no sensitivity near ecliptic. Corrected time stamps for ions and electrons. Energy threshold shifts have been applied. Changed EDB format, on-board anisotropies not possible in NM
Back to top
N. Cornilleau et al, The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment Space Sci. Rev., 79, pp 107 - 136, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats PI Software Version 4.1, 27 March 2006
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P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser: Performances and Perspectives for the Cluster Mission Space Sci. Rev., 79, pp 157 - 193, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Two types of parameters are provided by WHISPER: 1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding operations. The N_e_res value is calculated from an algorithm for resonance recognition, which cannot take account of all level of information available to the experimenter. The reliability of N_e_res parameters derived at the CSDS level is thus limited in an unknown manner. The N_e_res_q parameter (one value for each N_e_res data point) provides a crude idea of the probability that the N_e_res value is actually correct. A value of 0 means that the value is probably wrong, a value above 80 that it is probably correct. Anything in between reflects a crude evaluation of the chances. Refer to PI for details. 2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are related to recording of natural wave emissions. Those parameters, not affected by variations in instrument's transfer functions, are globally OK. However, two factors can affect the precision of the measurements: a) the occasional presence of spurious emissions created by operations of the EDI instrument increases the wave power values measured on SC1, SC2 and SC3, from an unknown amount, b) the limited dynamical range of the instrument leads to an underestimation of the E_pow parameters values when the voltage difference measured by the double sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp (depending of the gain chosen). As a consequence, high values have to be taken with special caution.
Back to top
A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C2_UP_FGM_20080930 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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No TEXT global attribute value.
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M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
JSOC predicted magnetic positions.
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M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997) AP _ Apogee CY 1 Start of visibility window at Canberra (5 deg elevation) CY 2 Start of visibility window at Canberra (5 deg elevation) CY 3 Start of visibility window at Canberra (5 deg elevation) CZ 1 End of visibility window at Canberra (5 deg elevation) CZ 2 End of visibility window at Canberra (5 deg elevation) CZ 3 End of visibility window at Canberra (5 deg elevation) CZ 4 End of visibility window at Canberra (5 deg elevation) DY 1 Start of visibility window at Vilspa (5 deg elevation) DY 2 Start of visibility window at Vilspa (5 deg elevation) DY 3 Start of visibility window at Vilspa (5 deg elevation) DZ 1 End of visibility window at Vilspa (5 deg elevation) DZ 2 End of visibility window at Vilspa (5 deg elevation) DZ 3 End of visibility window at Vilspa (5 deg elevation) GY 1 Start of visibility window at Goldstone (5 deg elevation) GY 2 Start of visibility window at Goldstone (5 deg elevation) GY 3 Start of visibility window at Goldstone (5 deg elevation) GY 4 Start of visibility window at Goldstone (5 deg elevation) GZ 1 End of visibility window at Goldstone (5 deg elevation) GZ 2 End of visibility window at Goldstone (5 deg elevation) GZ 3 End of visibility window at Goldstone (5 deg elevation) JY 1 Start of visibility window at Maspalomas (5 deg elevation) JY 2 Start of visibility window at Maspalomas (5 deg elevation) JY 3 Start of visibility window at Maspalomas (5 deg elevation) JY 4 Start of visibility window at Maspalomas (5 deg elevation) JZ 1 End of visibility window at Maspalomas (5 deg elevation) JZ 2 End of visibility window at Maspalomas (5 deg elevation) JZ 3 End of visibility window at Maspalomas (5 deg elevation) KA 1 Start of visibility window at Kourou (5 deg elevation) KA 2 Start of visibility window at Kourou (5 deg elevation) KA 3 Start of visibility window at Kourou (5 deg elevation) KA 4 Start of visibility window at Kourou (5 deg elevation) KL 1 End of visibility window at Kourou (5 deg elevation) KL 2 End of visibility window at Kourou (5 deg elevation) KL 3 End of visibility window at Kourou (5 deg elevation) KL 4 End of visibility window at Kourou (5 deg elevation) MY 1 Start of visibility window at Madrid (5 deg elevation) MY 2 Start of visibility window at Madrid (5 deg elevation) MY 3 Start of visibility window at Madrid (5 deg elevation) MY 4 Start of visibility window at Madrid (5 deg elevation) MZ 1 End of visibility window at Madrid (5 deg elevation) MZ 2 End of visibility window at Madrid (5 deg elevation) MZ 3 End of visibility window at Madrid (5 deg elevation) NS S Southbound neutral sheet NT I Enter north tail lobe from inner magnetosphere PA 1 Start of visibility window at Perth (5 deg elevation) PA 2 Start of visibility window at Perth (5 deg elevation) PA 3 Start of visibility window at Perth (5 deg elevation) PE _ Perigee PL 1 End of visibility window at Perth (5 deg elevation) PL 2 End of visibility window at Perth (5 deg elevation) PL 3 End of visibility window at Perth (5 deg elevation) PL 4 End of visibility window at Perth (5 deg elevation) QL I Inbound critical L value for auroral zone QL O Outbound critical L value for auroral zone RA 1 Start of visibility window at Redu (5 deg elevation) RA 2 Start of visibility window at Redu (5 deg elevation) RA 3 Start of visibility window at Redu (5 deg elevation) RA 4 Start of visibility window at Redu (5 deg elevation) RL 1 End of visibility window at Redu (5 deg elevation) RL 2 End of visibility window at Redu (5 deg elevation) RL 3 End of visibility window at Redu (5 deg elevation) ST O Leave south tail lobe for inner magnetosphere TL I Inbound radiation belt entry for WEC TL O Outbound radiation belt exit for WEC VL I Inbound critical L value for EDI VL O Outbound critical L value for EDI WL I Inbound critical L value for ASPOC WL O Outbound critical L value for ASPOC XL I Inbound critical L value for PEACE XL O Outbound critical L value for PEACE YL I Inbound critical L value for RAPID YL O Outbound critical L value for RAPID ZL I Inbound critical L value for CIS ZL O Outbound critical L value for CIS
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF2000 pole used to calculate GSM latitude and MLT in PSE files produced after 25 June 2001.
JSOC predicted scientific events.
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K. Torkar et al, Active spacecraft potential control for Cluster - implementation and first results Ann. Geophys., 19, pp 1289 - 1302, 2001)
none Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats One raw data format (5.1.5 secs) of bad data may occur when the instrument is powered on.
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H. Reme et al, First multispacecraft ion measurements in and near the Earth's magnetosphere with the identical Cluster Ion Spectrometry (CIS) experiment Annales Geophysicae, 19, pp 1303 - 1354, 2001
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats The user of the CIS data needs to be cautious. Please refer to the CIS Home Page: http://cis.cesr.fr:8000/CIS_sw_home-en.htm , link "Caveats for the CIS data", for caveats concerning these data.
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L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster Space Sci. Rev., 79, pp 209 - 231, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Refer to the PI or NDC for access to ongoing caveat information Use correlator data with caution
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G. Paschmann et al, The Electron Drift Instrument for Cluster Space Sci. Rev., 79, pp 233 - 269, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats 1) EDI's automated analysis algorithm has a known susceptibility to producing occasional incorrect values of the drift velocities (and electric fields). The code attempts to prevent these bad values to be output to the cdf file. No further removal is done in the validation process. 2) When drift velocities become sufficiently large, there can be a 180-degree ambiguity in drift direction that is usually flagged in bit 7 (counting from 0) of Status Byte 3. 3) There are two methods to analyze a spin's worth of EDI data. If bits 5 6 in Status Byte 3 are NOT set, the employed method was triangulation. If either bit 5 or 6 are set, then the results are from time-of-flight analysis. 4) The reported drift velocities and electric field refer to inertial coordinates, i.e., have been corrected for spacecraft velocity. However, the magnitude errors (in %) and the angle errors (in degrees), reported in Status Bytes 5 & 6, respectively, refer to the spacecraft frame and have NOT yet been converted to inertial coordinates. 5) The reduced chi-square reported as a data word is a measure of the goodness-of-fit of the triangulation analysis.
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G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster Space Sci. Rev., 79, pp 137 - 156, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data calibration may be unreliable at this early stage of the mission
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CSDS data are not for publication *** Be aware that data may be reprocessed as necessary to improve quality For questions on data validity please contact sdc-adm@plasma.kth.se Fill value inserted for E_dusk__C3_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_pow_f1__C3_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_sigma__C3_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for U_probe_sc__C3_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z
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A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CAUTION Preliminary calibrations used: not for publication ***
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A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment Space Sci. Rev., 79, pp 351 - 398, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 PP & SP data is generated at MSSL, then provided to UK-CDHF
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats This is PEACE PP/SP data version 3.1, produced at MSSL Based on onboard moments but using corrected geometric factors which account for uplinked changes of the values used in onboard calibration as well as estimated changes due to variable MCP gain performance Onboard moments are calculated for up to three energy ranges. Photoelectron contamination may affect 0, 1 or 2 of these ranges EFW PP probe-spacecraft potential was used to select the energy ranges to be excluded to remove misleading photoelectron contributions. Note that the density may be underestimated if there are both plasma electrons and photoelectrons in the lowest energy range When 88h58 is used for the HEEA sensor, sometimes the entire plasma electron population and photoelectrons are in just the lowest of the 3 energy ranges. This data has been deleted in this release of the PEACE PPs Data is deleted if the spacecraft electric potential is too large for the simple correction procedure to work or there is no EFW PP data available Measured electron energies have not been corrected for their acceleration by the spacecraft electric potential Onboard moments use onboard energy tables, efficiencies and response surfaces. Any errors in these parameters cannot be corrected in ground data processing Before 2001-09-11 the onboard energy efficiencies were not accurate, which caused the density in the solar wind to be overestimated. This data has been removed in this release of the PEACE PPs The calculation of T_par, T_perp and Q_par used PP FGM data The data is for context and information only. It is not suitable for detailed analysis, but may be used for event selection The next iteration of PP/SP moments will be of a higher quality Please see links under http://www.mssl.ucl.ac.uk/www_plasma/missions/cluster/clusterII.html for more information Please contact the PEACE PI to request science quality data Automatically validated by UKCDC Product delivered pre-validated by the PI institute
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B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster Space Sci. Rev., 79, pp 399 - 473, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data processed on 2009-02-06T07:49:52Z Caveats file: RAP_CAV_C3_V109.DAT; Release Feb 5, 2009
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats RAPID Data produced with best-effort general calibration files. Corrected: error that made ion fluxes 50% too large in 2006-2008 data. 1901-01-01T00:00:00.000Z/9999-12-31T23:59:59.999Z: Electrons: lowest energy channel needs correction for reduced sensitivity. 2001-12-13T00:00:00.000Z/9999-12-31T23:59:59.000Z: Central ion head not functioning since 2001-12-13, no sensitivity near ecliptic. Corrected time stamps for ions and electrons. Energy threshold shifts have been applied. Solar noise removed from electrons. Solar noise file is c3_saa_noise.dat from 2009-Feb-05 10:20:28 Changed EDB format, on-board anisotropies not possible in NM
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N. Cornilleau et al, The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment Space Sci. Rev., 79, pp 107 - 136, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats PI Software Version 4.1, 27 March 2006
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P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser: Performances and Perspectives for the Cluster Mission Space Sci. Rev., 79, pp 157 - 193, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Two types of parameters are provided by WHISPER: 1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding operations. The N_e_res value is calculated from an algorithm for resonance recognition, which cannot take account of all level of information available to the experimenter. The reliability of N_e_res parameters derived at the CSDS level is thus limited in an unknown manner. The N_e_res_q parameter (one value for each N_e_res data point) provides a crude idea of the probability that the N_e_res value is actually correct. A value of 0 means that the value is probably wrong, a value above 80 that it is probably correct. Anything in between reflects a crude evaluation of the chances. Refer to PI for details. 2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are related to recording of natural wave emissions. Those parameters, not affected by variations in instrument's transfer functions, are globally OK. However, two factors can affect the precision of the measurements: a) the occasional presence of spurious emissions created by operations of the EDI instrument increases the wave power values measured on SC1, SC2 and SC3, from an unknown amount, b) the limited dynamical range of the instrument leads to an underestimation of the E_pow parameters values when the voltage difference measured by the double sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp (depending of the gain chosen). As a consequence, high values have to be taken with special caution.
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A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C3_UP_FGM_20080930 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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No TEXT global attribute value.
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M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
JSOC predicted magnetic positions.
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M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997) AP _ Apogee CY 1 Start of visibility window at Canberra (5 deg elevation) CY 2 Start of visibility window at Canberra (5 deg elevation) CY 3 Start of visibility window at Canberra (5 deg elevation) CZ 1 End of visibility window at Canberra (5 deg elevation) CZ 2 End of visibility window at Canberra (5 deg elevation) CZ 3 End of visibility window at Canberra (5 deg elevation) CZ 4 End of visibility window at Canberra (5 deg elevation) DY 1 Start of visibility window at Vilspa (5 deg elevation) DY 2 Start of visibility window at Vilspa (5 deg elevation) DY 3 Start of visibility window at Vilspa (5 deg elevation) DY 4 Start of visibility window at Vilspa (5 deg elevation) DZ 1 End of visibility window at Vilspa (5 deg elevation) DZ 2 End of visibility window at Vilspa (5 deg elevation) DZ 3 End of visibility window at Vilspa (5 deg elevation) GY 1 Start of visibility window at Goldstone (5 deg elevation) GY 2 Start of visibility window at Goldstone (5 deg elevation) GY 3 Start of visibility window at Goldstone (5 deg elevation) GY 4 Start of visibility window at Goldstone (5 deg elevation) GZ 1 End of visibility window at Goldstone (5 deg elevation) GZ 2 End of visibility window at Goldstone (5 deg elevation) GZ 3 End of visibility window at Goldstone (5 deg elevation) JY 1 Start of visibility window at Maspalomas (5 deg elevation) JY 2 Start of visibility window at Maspalomas (5 deg elevation) JY 3 Start of visibility window at Maspalomas (5 deg elevation) JY 4 Start of visibility window at Maspalomas (5 deg elevation) JZ 1 End of visibility window at Maspalomas (5 deg elevation) JZ 2 End of visibility window at Maspalomas (5 deg elevation) JZ 3 End of visibility window at Maspalomas (5 deg elevation) KA 1 Start of visibility window at Kourou (5 deg elevation) KA 2 Start of visibility window at Kourou (5 deg elevation) KA 3 Start of visibility window at Kourou (5 deg elevation) KA 4 Start of visibility window at Kourou (5 deg elevation) KL 1 End of visibility window at Kourou (5 deg elevation) KL 2 End of visibility window at Kourou (5 deg elevation) KL 3 End of visibility window at Kourou (5 deg elevation) KL 4 End of visibility window at Kourou (5 deg elevation) MY 1 Start of visibility window at Madrid (5 deg elevation) MY 2 Start of visibility window at Madrid (5 deg elevation) MY 3 Start of visibility window at Madrid (5 deg elevation) MY 4 Start of visibility window at Madrid (5 deg elevation) MZ 1 End of visibility window at Madrid (5 deg elevation) MZ 2 End of visibility window at Madrid (5 deg elevation) MZ 3 End of visibility window at Madrid (5 deg elevation) NS S Southbound neutral sheet NT I Enter north tail lobe from inner magnetosphere PA 1 Start of visibility window at Perth (5 deg elevation) PA 2 Start of visibility window at Perth (5 deg elevation) PA 3 Start of visibility window at Perth (5 deg elevation) PA 4 Start of visibility window at Perth (5 deg elevation) PE _ Perigee PL 1 End of visibility window at Perth (5 deg elevation) PL 2 End of visibility window at Perth (5 deg elevation) PL 3 End of visibility window at Perth (5 deg elevation) PL 4 End of visibility window at Perth (5 deg elevation) PL 5 End of visibility window at Perth (5 deg elevation) QL I Inbound critical L value for auroral zone QL O Outbound critical L value for auroral zone RA 1 Start of visibility window at Redu (5 deg elevation) RA 2 Start of visibility window at Redu (5 deg elevation) RA 3 Start of visibility window at Redu (5 deg elevation) RL 1 End of visibility window at Redu (5 deg elevation) RL 2 End of visibility window at Redu (5 deg elevation) RL 3 End of visibility window at Redu (5 deg elevation) ST O Leave south tail lobe for inner magnetosphere TL I Inbound radiation belt entry for WEC TL O Outbound radiation belt exit for WEC VL I Inbound critical L value for EDI VL O Outbound critical L value for EDI WL B Outbound critical L value 2 for ASPOC WL I Inbound critical L value for ASPOC WL O Outbound critical L value for ASPOC XL I Inbound critical L value for PEACE XL O Outbound critical L value for PEACE YL I Inbound critical L value for RAPID YL O Outbound critical L value for RAPID ZL I Inbound critical L value for CIS ZL O Outbound critical L value for CIS
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF2000 pole used to calculate GSM latitude and MLT in PSE files produced after 25 June 2001.
JSOC predicted scientific events.
Back to top
K. Torkar et al, Active spacecraft potential control for Cluster - implementation and first results Ann. Geophys., 19, pp 1289 - 1302, 2001)
none Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats One raw data format (5.1.5 secs) of bad data may occur when the instrument is powered on.
Back to top
H. Reme et al, First multispacecraft ion measurements in and near the Earth's magnetosphere with the identical Cluster Ion Spectrometry (CIS) experiment Annales Geophysicae, 19, pp 1303 - 1354, 2001
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats The user of the CIS data needs to be cautious. Please refer to the CIS Home Page: http://cis.cesr.fr:8000/CIS_sw_home-en.htm , link "Caveats for the CIS data", for caveats concerning these data.
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L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster Space Sci. Rev., 79, pp 209 - 231, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Refer to the PI or NDC for access to ongoing caveat information Use correlator data with caution
Back to top
G. Paschmann et al, The Electron Drift Instrument for Cluster Space Sci. Rev., 79, pp 233 - 269, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats C4 EDI switched off
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G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster Space Sci. Rev., 79, pp 137 - 156, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data calibration may be unreliable at this early stage of the mission
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CSDS data are not for publication *** Be aware that data may be reprocessed as necessary to improve quality For questions on data validity please contact sdc-adm@plasma.kth.se Fill value inserted for E_dusk__C4_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_pow_f1__C4_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_sigma__C4_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for U_probe_sc__C4_PP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z
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A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CAUTION Preliminary calibrations used: not for publication ***
Back to top
A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment Space Sci. Rev., 79, pp 351 - 398, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 PP & SP data is generated at MSSL, then provided to UK-CDHF
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats This is PEACE PP/SP data version 3.1, produced at MSSL Based on onboard moments but using corrected geometric factors which account for uplinked changes of the values used in onboard calibration as well as estimated changes due to variable MCP gain performance Onboard moments are calculated for up to three energy ranges. Photoelectron contamination may affect 0, 1 or 2 of these ranges EFW PP probe-spacecraft potential was used to select the energy ranges to be excluded to remove misleading photoelectron contributions. Note that the density may be underestimated if there are both plasma electrons and photoelectrons in the lowest energy range When 88h58 is used for the HEEA sensor, sometimes the entire plasma electron population and photoelectrons are in just the lowest of the 3 energy ranges. This data has been deleted in this release of the PEACE PPs Data is deleted if the spacecraft electric potential is too large for the simple correction procedure to work or there is no EFW PP data available Measured electron energies have not been corrected for their acceleration by the spacecraft electric potential Onboard moments use onboard energy tables, efficiencies and response surfaces. Any errors in these parameters cannot be corrected in ground data processing Before 2001-09-11 the onboard energy efficiencies were not accurate, which caused the density in the solar wind to be overestimated. This data has been removed in this release of the PEACE PPs The calculation of T_par, T_perp and Q_par used PP FGM data The data is for context and information only. It is not suitable for detailed analysis, but may be used for event selection The next iteration of PP/SP moments will be of a higher quality Please see links under http://www.mssl.ucl.ac.uk/www_plasma/missions/cluster/clusterII.html for more information Please contact the PEACE PI to request science quality data Automatically validated by UKCDC Product delivered pre-validated by the PI institute
Back to top
B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster Space Sci. Rev., 79, pp 399 - 473, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data processed on 2009-02-06T07:50:05Z Caveats file: RAP_CAV_C4_V109.DAT; Release Feb 5, 2009
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats RAPID Data produced with best-effort general calibration files. Corrected: error that made ion fluxes 50% too large in 2006-2008 data. 1901-01-01T00:00:00.000Z/9999-12-31T23:59:59.999Z: Electrons: lowest energy channel needs correction for reduced sensitivity. 2001-12-12T00:00:00.000Z/9999-12-31T23:59:59.000Z: Central ion head not functioning since 2001-12-12, no sensitivity near ecliptic. 2006-09-15T15:04:00.000Z/9999-12-31T23:59:59.000Z: Omnidirectional electrons: excludes detectors 7 & 9, pedestal contamination. 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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N. Cornilleau et al, The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment Space Sci. Rev., 79, pp 107 - 136, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats PI Software Version 4.1, 27 March 2006
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P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser: Performances and Perspectives for the Cluster Mission Space Sci. Rev., 79, pp 157 - 193, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Two types of parameters are provided by WHISPER: 1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding operations. The N_e_res value is calculated from an algorithm for resonance recognition, which cannot take account of all level of information available to the experimenter. The reliability of N_e_res parameters derived at the CSDS level is thus limited in an unknown manner. The N_e_res_q parameter (one value for each N_e_res data point) provides a crude idea of the probability that the N_e_res value is actually correct. A value of 0 means that the value is probably wrong, a value above 80 that it is probably correct. Anything in between reflects a crude evaluation of the chances. Refer to PI for details. 2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are related to recording of natural wave emissions. Those parameters, not affected by variations in instrument's transfer functions, are globally OK. However, two factors can affect the precision of the measurements: a) the occasional presence of spurious emissions created by operations of the EDI instrument increases the wave power values measured on SC1, SC2 and SC3, from an unknown amount, b) the limited dynamical range of the instrument leads to an underestimation of the E_pow parameters values when the voltage difference measured by the double sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp (depending of the gain chosen). As a consequence, high values have to be taken with special caution.
Back to top
A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** C4_UP_FGM_20080930 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.
Back to top
M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
JSOC predicted Solar cycle trends.
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M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 1997 For geometrical configuration parameters, p328 of Tetrahedron Geometric Factors by P.Robert et al, in Analysis Methods for Multi-Spacecraft Data, ed. G.Paschmann & P.Daly, pub. 1998 by the European Space Agency and the International Space Institute, Bern.
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF2000 pole used to calculate dipole tilt and GSE-GSM angle in PGP files produced after 25 June 2001.
JSOC predicted Orbits. Using spacecraft C3 as reference spacecraft.
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Pre-generated PWG plots
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K. Torkar et al, Active spacecraft potential control for Cluster - implementation and first results Ann. Geophys., 19, pp 1289 - 1302, 2001)
none Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats One raw data format (5.1.5 secs) of bad data may occur when the instrument is powered on.
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Orbital Parameters Calculated from Short Term Orbit File of RDM For geometry configuration parameters, see p 328 of Tetrahedron Geometric Factors by P.Robert et al, in Analysis Methods for Multi-Spacecraft Data, ed. G.Paschmann & P.Daly, pub. 1998 by the European Space Agency and the International Space Institute, Bern.
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF 10th generation pole used to calculate GSE-to-GSM angle and dipole tilt from 1 January 2005
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats
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H. Reme et al, First multispacecraft ion measurements in and near the Earth's magnetosphere with the identical Cluster Ion Spectrometry (CIS) experiment Annales Geophysicae, 19, pp 1303 - 1354, 2001
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats The user of the CIS data needs to be cautious. Please refer to the CIS Home Page: http://cis.cesr.fr:8000/CIS_sw_home-en.htm , link "Caveats for the CIS data", for caveats concerning these data.
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L. J. C. Woolliscroft et al, The Digital Wave-Processing Experiment on Cluster Space Sci. Rev., 79, pp 209 - 231, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software SP file for S/C Cluster 3
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Refer to the PI or NDC for access to ongoing caveat information Use correlator data with caution
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G. Paschmann et al, The Electron Drift Instrument for Cluster Space Sci. Rev., 79, pp 233 - 269, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats 1) EDI's automated analysis algorithm has a known susceptibility to producing occasional incorrect values of the drift velocities (and electric fields). The code attempts to prevent these bad values to be output to the cdf file. No further removal is done in the validation process. 2) When drift velocities become sufficiently large, there can be a 180-degree ambiguity in drift direction that is usually flagged in bit 7 (counting from 0) of Status Byte 3. 3) There are two methods to analyze a spin's worth of EDI data. If bits 5 6 in Status Byte 3 are NOT set, the employed method was triangulation. If either bit 5 or 6 are set, then the results are from time-of-flight analysis. 4) The reported drift velocities and electric field refer to inertial coordinates, i.e., have been corrected for spacecraft velocity. However, the magnitude errors (in %) and the angle errors (in degrees), reported in Status Bytes 5 & 6, respectively, refer to the spacecraft frame and have NOT yet been converted to inertial coordinates. 5) The reduced chi-square reported as a data word is a measure of the goodness-of-fit of the triangulation analysis.
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G. Gustafsson et al, The Electric Field and Wave Experiment for Cluster Space Sci. Rev., 79, pp 137 - 156, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Data calibration may be unreliable at this early stage of the mission
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CSDS data are not for publication *** Be aware that data may be reprocessed as necessary to improve quality For questions on data validity please contact sdc-adm@plasma.kth.se Fill value inserted for U_probe_sc__CL_SP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_dusk__CL_SP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_pow_f1__CL_SP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z Fill value inserted for E_sigma__CL_SP_EFW: No reason given for time range 2008-03-31T23:14:00Z to 2008-03-31T23:17:00Z
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A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software SP file for S/C Cluster 3
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CAUTION Preliminary calibrations used: not for publication ***
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A. D. Johnstone et al, Peace, A Plasma Electron and Current Experiment Space Sci. Rev., 79, pp 351 - 398, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 PP & SP data is generated at MSSL, then provided to UK-CDHF
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats This is PEACE PP/SP data version 3.1, produced at MSSL Based on onboard moments but using corrected geometric factors which account for uplinked changes of the values used in onboard calibration as well as estimated changes due to variable MCP gain performance Onboard moments are calculated for up to three energy ranges. Photoelectron contamination may affect 0, 1 or 2 of these ranges EFW PP probe-spacecraft potential was used to select the energy ranges to be excluded to remove misleading photoelectron contributions. Note that the density may be underestimated if there are both plasma electrons and photoelectrons in the lowest energy range When 88h58 is used for the HEEA sensor, sometimes the entire plasma electron population and photoelectrons are in just the lowest of the 3 energy ranges. This data has been deleted in this release of the PEACE PPs Data is deleted if the spacecraft electric potential is too large for the simple correction procedure to work or there is no EFW PP data available Measured electron energies have not been corrected for their acceleration by the spacecraft electric potential Onboard moments use onboard energy tables, efficiencies and response surfaces. Any errors in these parameters cannot be corrected in ground data processing Before 2001-09-11 the onboard energy efficiencies were not accurate, which caused the density in the solar wind to be overestimated. This data has been removed in this release of the PEACE PPs The calculation of T_par, T_perp and Q_par used PP FGM data The data is for context and information only. It is not suitable for detailed analysis, but may be used for event selection The next iteration of PP/SP moments will be of a higher quality Please see links under http://www.mssl.ucl.ac.uk/www_plasma/missions/cluster/clusterII.html for more information Please contact the PEACE PI to request science quality data Automatically validated by UKCDC Product delivered pre-validated by the PI institute
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B. Wilken et al, RAPID, The Imaging Energetic Particle Spectrometer on Cluster Space Sci. Rev., 79, pp 399 - 473, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Summary parameters derived from C3_PP_RAP_20081231 Data processed on 2009-02-06T07:49:52Z Caveats file: RAP_CAV_C3_V109.DAT; Release Feb 5, 2009
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats RAPID Data produced with best-effort general calibration files. Corrected: error that made ion fluxes 50% too large in 2006-2008 data. 1901-01-01T00:00:00.000Z/9999-12-31T23:59:59.999Z: Electrons: lowest energy channel needs correction for reduced sensitivity. 2001-12-13T00:00:00.000Z/9999-12-31T23:59:59.000Z: Central ion head not functioning since 2001-12-13, no sensitivity near ecliptic. Corrected time stamps for ions and electrons. Energy threshold shifts have been applied. Solar noise removed from electrons. Solar noise file is c3_saa_noise.dat from 2009-Feb-05 10:20:28 Changed EDB format, on-board anisotropies not possible in NM
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N. Cornilleau et al, The Cluster Spatio-Temporal Analysis of Field Fluctuations (Staff) Experiment Space Sci. Rev., 79, pp 107 - 136, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats PI Software Version 4.1, 27 March 2006
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Reference to uiowa cluster site
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P. M. E. Decreau et al, WHISPER, A Resonance Sounder and Wave Analyser: Performances and Perspectives for the Cluster Mission Space Sci. Rev., 79, pp 157 - 193, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats Two types of parameters are provided by WHISPER: 1) Density values (and quality): N_e_res and N_e_res_q, are related to sounding operations. The N_e_res value is calculated from an algorithm for resonance recognition, which cannot take account of all level of information available to the experimenter. The reliability of N_e_res parameters derived at the CSDS level is thus limited in an unknown manner. The N_e_res_q parameter (one value for each N_e_res data point) provides a crude idea of the probability that the N_e_res value is actually correct. A value of 0 means that the value is probably wrong, a value above 80 that it is probably correct. Anything in between reflects a crude evaluation of the chances. Refer to PI for details. 2) Wave power values: E_pow_f4, E_pow_f5, E_pow_f6, E_pow_su and E_var_ts, are related to recording of natural wave emissions. Those parameters, not affected by variations in instrument's transfer functions, are globally OK. However, two factors can affect the precision of the measurements: a) the occasional presence of spurious emissions created by operations of the EDI instrument increases the wave power values measured on SC1, SC2 and SC3, from an unknown amount, b) the limited dynamical range of the instrument leads to an underestimation of the E_pow parameters values when the voltage difference measured by the double sphere antenna signal in the 2 - 80 kHz band is higher than 150 mVp or 600 mVp (depending of the gain chosen). As a consequence, high values have to be taken with special caution.
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A. Balogh et al, The Cluster Magnetic Field Investigation Space Sci. Rev., 79, pp 65 - 92, 1997)
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 Operational version of UKCDHF Pipeline software
See CSDS User's Guide, DS-MPA-TN-0015, for post processing caveats *** CL_US_FGM_20080930 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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Images and intensities. 557.7nm Images binned to geodetic grid References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J., McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D., Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.
Created 29-DEC-1994
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North & East Velocity components at 336.5 EDFL long. from 64.2 to 67.0 EDFL lat. References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J., McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D., Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.
Created 18-JUL-1994
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Magnetic Field Extrema and Location References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J., McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D., Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.
Created 19-AUG-1994
More sites => greater quality
Geodetic latitude of station that measured the extrema used to compute the local auroral electrojet idex CL
Geodetic latitude of station that measured the extrema used to compute the local auroral electrojet idex CU
Geodetic longitude of station that measured the extrema used to compute the local auroral electrojet idex CL
Geodetic longitude of station that measured the extrema used to compute the local auroral electrojet idex CU
Local equivalent to AL index, but computed from magnetic field perturbations measured at stations of the CANOPUS array
Local equivalent to AU index, but computed from magnetic field perturbations measured at specific stations of the CANOPUS array
Station Status, Merged Scaled 5577A Scans and Peak Intensity Merged Scans>from 3 stations along constant Geodetic Long. of 265, from Lat. 46 to 67 References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J., McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D., Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993. 2.Samson, J.C., Lyons, L.R., Newell, P.T., Creutzberg, F. and Xu, B., Proton aurora substorm intensifications, Geophys. Res. Letters, 19, 2167, 1992. 3.Samson, J.C., Hughes, T.J., Creutzberg, F., Wallis, D.D., Greenwald, R.A. and Ruohoniemi, J.M., Observations of a detached discrete arc in association with field line resonances, J. Geophys. Res., 96, 15, 683, 1991.
Created 18-DEC-1994
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Riometer measurements and Location References: 1.Rostoker, G., Samson, J.C., Creutzberg, F., Hughes, T.J., McDiarmid, D.R., McNamara, A.G., Vallance Jones, A., Wallis, D.D., Cogger, L.L.; CANOPUS - a ground based instrument array for remote sensing the high latitude ionosphere during the ISTP/GGS program, Space Sci. Rev., submitted for publication, 1993.
Created 19-AUG-1994
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CRRES MEA Data Archive This is the re-processed version of the MEA data archive from the CRRES spacecraft. The raw data provided by Principal Investigator A. Vampola have been processed to derive 1 min average data. The data consists of counting rates from 17 energy channels in the range of 0.1-2 MeV and 19 pitch angle bins at 1 minute time intervals. The average flux, 90 degree flux and N value are included. Also included are the spacecraft geographic coordinates and altitude, L shell, and the local and equatorial magnetic field magnitudes from the 1977 Olson-Pfitzer model of the earth's geomagnetic field. The raw high resolution (0.512 sec) data and documentation of raw data can be found at:ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/crres/particle_mea.
Created May 2003
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M.A. Hapgood et al, The Joint Science Operations Centre, Space Sci. Rev. 79, 487-525 (1997) NS S Southbound neutral sheet NT I Enter north tail lobe from inner magnetosphere ST O Leave south tail lobe for inner magnetosphere
Produced in accordance with CSDS file specification Reference Document for CSDS CDF File Design, DS-QMW-TN-0003 IGRF2000 pole used to calculate GSM latitude and MLT in PSE files produced after 25 June 2001.
JSOC predicted scientific events.
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