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1) AMPTE/CCE Spin-averaged Magnetic Field Measurements maxmize
Resource ID:spase://VMO/NumericalData/AMPTE_CCE/MFE/PT5.83S
Start:1984-08-20 23:59:54 Observatory:AMPTE/CCE Cadence:5.83 seconds
Stop:1989-01-09 23:59:34 Instrument:AMPTE/CCE Magnetic Field Experiment (MFE) Resource:NumericalData
AMPTE/CCE spin-averaged DC magnetic field at ~5.83 second resolution.
2) AMPTE/IRM Magnetic Field maxmize
Resource ID:spase://VMO/NumericalData/AMPTE_IRM/MAG/PT4.4S
Start:1984-08-21 00:48:41 Observatory:AMPTE/IRM Cadence:4.4 seconds
Stop:1986-08-11 21:45:07 Instrument:AMPTE/IRM Magnetometer Resource:NumericalData
AMPTE/IRM spin-averaged magnetic field at ~4.4 second resolution.
3) AMPTE/UKS Magnetic Field Data maxmize
Resource ID:spase://VMO/NumericalData/AMPTE_UKS/FGM/PT5S
Start:1984-08-21 08:24:42 Observatory:AMPTE/UKS Cadence:5 seconds
Stop:1985-01-15 08:01:02 Instrument:AMPTE/UKS Magnetometer Resource:NumericalData
AMPTE/UKS 5-second (spin) averaged magnetic field measurements
4) BAS A80 Ground Magnetic Field Data 0.5s Data. maxmize
Resource ID:spase://VMO/NumericalData/AUGSBURG/BAS.A80/SearchCoil/PT0.5S
Start:1997-01-07 00:00:00 Observatory:BAS A80 Cadence:0.5 seconds
Stop:2003-12-08 23:59:59 Instrument:The BAS A80 Fluxgate SearchCoil Instrument. Resource:NumericalData
Ground Magnetic Field Data data from BAS A80 at 0.5s time resolution.
5) BAS A81 Ground Magnetic Field Data 0.5s Data. maxmize
Resource ID:spase://VMO/NumericalData/AUGSBURG/BAS.A81/SearchCoil/PT0.5S
Start:1996-01-11 00:00:00 Observatory:BAS A81 Cadence:0.5 seconds
Stop:2003-12-07 23:59:59 Instrument:The BAS A81 Fluxgate SearchCoil Instrument. Resource:NumericalData
Ground Magnetic Field Data data from BAS A81 at 0.5s time resolution.
6) BAS A84 Ground Magnetic Field Data 0.5s Data. maxmize
Resource ID:spase://VMO/NumericalData/AUGSBURG/BAS.A84/SearchCoil/PT0.5S
Start:1999-01-16 00:00:00 Observatory:BAS A84 Cadence:0.5 seconds
Stop:2003-12-07 23:59:59 Instrument:The BAS A84 Fluxgate SearchCoil Instrument. Resource:NumericalData
Ground Magnetic Field Data data from BAS A84 at 0.5s time resolution.
7) Halley Bay Ground Magnetic Field Data 0.5s Data. maxmize
Resource ID:spase://VMO/NumericalData/AUGSBURG/Halley.Bay/SearchCoil/PT0.5S
Start:2005-02-16 00:00:00 Observatory:Halley Bay Cadence:0.5 seconds
Stop:2007-12-31 23:59:59 Instrument:The Halley Bay Fluxgate SearchCoil Instrument. Resource:NumericalData
Ground Magnetic Field Data data from Halley Bay at 0.5s time resolution.
8) South Pole Ground Magnetic Field Data 0.5s Data. maxmize
Resource ID:spase://VMO/NumericalData/AUGSBURG/South.Pole/SearchCoil/PT0.5S
Start:2005-01-01 00:00:00 Observatory:South Pole Cadence:0.5 seconds
Stop:2007-12-31 23:59:59 Instrument:The South Pole Fluxgate SearchCoil Instrument. Resource:NumericalData
Ground Magnetic Field Data data from South Pole at 0.5s time resolution.
9) CRRES 2s magnetic field data maxmize
Resource ID:spase://VMO/NumericalData/CRRES/MAG/PT2S
Start:1990-10-11 00:00:00 Observatory:CRRES Cadence:2 seconds
Stop:1991-10-13 00:00:00 Instrument:Fluxgate Magnetometer Resource:NumericalData
This data set contains magnetic field vectors and tilt angles from the CRRES tri-axial fluxgate magnetometer data. The magnetic field vectors are at 2 s resolution and in the Vehicle Dipole Horizon (VDH) coordinate system. Also included are the magnetic field magnitude and the tilt of the magnetic field in Theta and Phi in the VDH coordinate system.
10) CRRES 30s magnetic field data maxmize
Resource ID:spase://VMO/NumericalData/CRRES/MAG/PT30S
Start:1990-10-11 00:00:00 Observatory:CRRES Cadence:30 seconds
Stop:1991-10-13 00:00:00 Instrument:Fluxgate Magnetometer Resource:NumericalData
This data set contains spin fitted magnetic field vectors and magnitudes from the CRRES tri-axial fluxgate magnetometer data. The magnetic field vectors are at 30 s resolution and in the GSE coordinate system.
11) Cluster Rumba Spin Resolution Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/FGM/SpinResolution/4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2013-05-21 01:01:59 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains spin resolution measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster Rumba spacecraft.
12) Cluster II Rumba Unvalidated Prime Parameter Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/FGM/UnvalidatedParameter/4S
Start:2006-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2013-05-21 01:01:59 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains spin resolution unvalidated prime parameter measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster 2 Rumba spacecraft. Unvalidated FGM data might sometimes contain artefacts such as spikes (duration ~ 1 spin), or short rotations (few spins). Very occasionally the data contain many spikes over several hours. Please contact Elizabeth Lucek (e.lucek@imperial.ac.uk) for more information regarding possible artefacts in specific intervals of data. The unvalidated prime parameter Data Set does not contain the spacecraft position data or additional range and telemetry mode information that the CAA parameter data set does contain.
13) Cluster II Rumba Prime Parameter Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/STAFF/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:4 seconds
Stop:2013-05-21 01:01:59 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
The Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) experiment provides magnetic field power spectral density values parallel and perpendicular to the magnetic field and the electric field power spectral density values for several frequency ranges. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The STAFF (Spatio-Temporal Analysis of Field Fluctuations) Experiment for the Cluster Mission, by N. Cornilleau-Wehrlin et al., from which this information was obtained.
14) Cluster 1 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Rumba/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM5 (Rumba) Cadence:0.0000046 seconds
Stop:2013-05-21 01:02:12 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations 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. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 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. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | 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. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...
15) Cluster II Rumba Wide Band Data (WBD) Prime Parameters maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Rumba/WBD/PrimeParameter/PT0.02S
Start:2001-02-04 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:0.02 seconds
Stop:2013-05-21 01:02:00 Instrument:Wide Band Data (WBD) Resource:NumericalData
The WBD (Wide Band Data) investigation is designed to provide high-resolution frequency/time spectra of plasma waves in the Earth's magnetosphere. These data files contain information on the band width, resolution, antenna angles, offsets, magnetic and electric field information. For more details of the Cluster mission, the spacecraft, and its instruments, see the report ``Cluster: mission, payload and supporting activities,'' March 1993, ESA SP-1159, and the included article ``The Wideband Plasma Wave Investigation,'' by D. A. Gurnett et al., from which this information was obtained.
16) Cluster Salsa Spin Resolution Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/FGM/SpinResolution/4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2013-05-21 01:01:10 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains spin resolution measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster Salsa spacecraft.
17) Cluster II Salsa Unvalidated Prime Parameter Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/FGM/UnvalidatedParameter/4S
Start:2006-01-01 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2013-05-21 01:01:10 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains spin resolution unvalidated prime parameter measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster 2 Salsa spacecraft. Unvalidated FGM data might sometimes contain artefacts such as spikes (duration ~ 1 spin), or short rotations (few spins). Very occasionally the data contain many spikes over several hours. Please contact Elizabeth Lucek (e.lucek@imperial.ac.uk) for more information regarding possible artefacts in specific intervals of data. The unvalidated prime parameter Data Set does not contain the spacecraft position data or additional range and telemetry mode information that the CAA parameter data set does contain.
18) Cluster II Salsa Prime Parameter Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/STAFF/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2013-05-21 01:01:10 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
The Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) experiment provides magnetic field power spectral density values parallel and perpendicular to the magnetic field and the electric field power spectral density values for several frequency ranges. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The STAFF (Spatio-Temporal Analysis of Field Fluctuations) Experiment for the Cluster Mission, by N. Cornilleau-Wehrlin et al., from which this information was obtained.
19) Cluster 2 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Salsa/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM6 (Salsa) Cadence:0.0000046 seconds
Stop:2013-05-21 01:02:11 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations 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. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 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. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | 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. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...
20) Cluster Samba Spin Resolution Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/FGM/SpinResolution/4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2013-05-21 01:01:40 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains spin resolution measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster Samba spacecraft.
21) Cluster II Samba Unvalidated Prime Parameter Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/FGM/UnvalidatedParameter/4S
Start:2006-01-01 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2013-05-21 01:01:40 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains spin resolution unvalidated prime parameter measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster 2 Samba spacecraft. Unvalidated FGM data might sometimes contain artefacts such as spikes (duration ~ 1 spin), or short rotations (few spins). Very occasionally the data contain many spikes over several hours. Please contact Elizabeth Lucek (e.lucek@imperial.ac.uk) for more information regarding possible artefacts in specific intervals of data. The unvalidated prime parameter Data Set does not contain the spacecraft position data or additional range and telemetry mode information that the CAA parameter data set does contain.
22) Cluster II Samba Prime Parameter Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Samba/STAFF/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:4 seconds
Stop:2013-05-21 01:01:40 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
The Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) experiment provides magnetic field power spectral density values parallel and perpendicular to the magnetic field and the electric field power spectral density values for several frequency ranges. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The STAFF (Spatio-Temporal Analysis of Field Fluctuations) Experiment for the Cluster Mission, by N. Cornilleau-Wehrlin et al., from which this information was obtained.
23) Cluster 3 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Samba/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM7 (Samba) Cadence:0.0000046 seconds
Stop:2013-05-21 01:02:12 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations 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. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 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. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | 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. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...
24) Cluster Tango Spin Resolution Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Tango/FGM/SpinResolution/4S
Start:2001-01-30 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:4 seconds
Stop:2013-05-21 01:01:31 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains spin resolution measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster Tango spacecraft.
25) Cluster II Tango Unvalidated Prime Parameter Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Tango/FGM/UnvalidatedParameter/4S
Start:2006-01-01 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:4 seconds
Stop:2013-05-21 01:01:31 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains spin resolution unvalidated prime parameter measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster 2 Tango spacecraft. Unvalidated FGM data might sometimes contain artefacts such as spikes (duration ~ 1 spin), or short rotations (few spins). Very occasionally the data contain many spikes over several hours. Please contact Elizabeth Lucek (e.lucek@imperial.ac.uk) for more information regarding possible artefacts in specific intervals of data. The unvalidated prime parameter Data Set does not contain the spacecraft position data or additional range and telemetry mode information that the CAA parameter data set does contain.
26) Cluster II Tango Prime Parameter Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Tango/STAFF/PrimeParameter/4S
Start:2000-12-09 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:4 seconds
Stop:2013-05-21 01:01:31 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
The Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) experiment provides magnetic field power spectral density values parallel and perpendicular to the magnetic field and the electric field power spectral density values for several frequency ranges. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The STAFF (Spatio-Temporal Analysis of Field Fluctuations) Experiment for the Cluster Mission, by N. Cornilleau-Wehrlin et al., from which this information was obtained.
27) Cluster 4 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Tango/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM8 (Tango) Cadence:0.0000046 seconds
Stop:2013-05-21 01:02:11 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations 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. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 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. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | 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. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...
28) Cluster II Summary Parameter Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/FGM/SummaryParameter/60S
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2013-05-21 01:01:09 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains 1 minute resolution validated summary prime parameter measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster 2 spacecraft. The summary prime parameter data set does not contain the spacecraft position data or additional range and telemetry mode information that the CAA parameter data set does contain.
29) Cluster II Unvalidated Summary Parameter Fluxgate Magnetometer (FGM) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/FGM/UnvalidatedSummaryParameter/60S
Start:2006-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2013-05-21 01:01:09 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
This dataset contains 1 minute resolution unvalidated summary prime parameter measurements of the magnetic field vector from the fluxgate magnetometer (FGM) instrument on the Cluster 2 spacecraft. Unvalidated FGM data might sometimes contain artefacts such as spikes (duration ~ 1 spin), or short rotations (few spins). Very occasionally the data contain many spikes over several hours. Please contact Elizabeth Lucek (e.lucek@imperial.ac.uk) for more information regarding possible artefacts in specific intervals of data. The unvalidated summary prime parameter data set does not contain the spacecraft position data or additional range and telemetry mode information that the CAA parameter data set does contain.
30) Cluster II Summary Parameter Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Data maxmize
Resource ID:spase://VMO/NumericalData/Cluster/STAFF/SummaryParameter/60S
Start:2001-01-09 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2013-05-21 01:01:09 Instrument:Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) Resource:NumericalData
The Spatio-Temporal Analysis of Magnetic Field Fluctuations (STAFF) experiment provides magnetic field power spectral density values parallel and perpendicular to the magnetic field and the electric field power spectral density values for several frequency ranges. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The STAFF (Spatio-Temporal Analysis of Field Fluctuations) Experiment for the Cluster Mission, by N. Cornilleau-Wehrlin et al., from which this information was obtained.
31) Dynamics Explorer 1 Magnetic Field Observations Triaxial Fluxgate Magnetometer (MAG-A) maxmize
Resource ID:spase://VMO/NumericalData/DE1/MAGA/PT0.062S
Start:1981-09-15 00:00:00 Observatory:Dynamics Explorer 1 Cadence:0.062 seconds
Stop:1991-02-18 00:00:00 Instrument:Magnetic Field Observations (MAG-A) Resource:NumericalData
Dynamics Explorer 1 Magnetic Field Observations Triaxial Fluxgate Magnetometer
32) DE 1 Magnetic Field Observations Triaxial Fluxgate Magnetometer (MAG-A) maxmize
Resource ID:spase://VMO/NumericalData/DE1/MAGA/PT6S
Start:1981-09-15 00:00:00 Observatory:Dynamics Explorer 1 Cadence:6 seconds
Stop:1991-02-18 00:00:00 Instrument:Magnetic Field Observations (MAG-A) Resource:NumericalData
Dynamics Explorer 1 Magnetic Field Observations Triaxial Fluxgate Magnetometer at 6 second resolution.
33) Dynamics Explorer 2 Combined Magnetic Field Vector Electric Field Data DC maxmize
Resource ID:spase://VMO/NumericalData/DE2/BVEFI/DC/PT0.5S
Start:1981-10-04 16:00:00 Observatory:Dynamics Explorer 2 Cadence:1 second
Stop:1981-02-19 00:00:00 Instrument:Vector Electric Field Instrument (VEFI) Resource:NumericalData
Dynamics Explorer 2 Magnetic Field and Vector Electric Field Instrument DC Data
34) Dynamics Explorer 2 Combined Magnetic Field Vector Electric Field Data Matrix maxmize
Resource ID:spase://VMO/NumericalData/DE2/BVEFI/MATRIX/PT0.5S
Start:1981-10-04 16:00:00 Observatory:Dynamics Explorer 2 Cadence:1 second
Stop:1981-02-19 00:00:00 Instrument:Vector Electric Field Instrument (VEFI) Resource:NumericalData
Dynamics Explorer 2 Magnetic Field and Vector Electric Field Instrument DC Matrix
35) Dynamics Explorer 2 Magnetic Field Observations Triaxial Fluxgate Magnetometer (MAG-B) maxmize
Resource ID:spase://VMO/NumericalData/DE2/MAGB/PT0.062S
Start:1981-09-15 00:00:00 Observatory:Dynamics Explorer 2 Cadence:0.062 seconds
Stop:1981-02-19 00:00:00 Instrument:Magnetic Field Observations (MAG-B) Resource:NumericalData
Dynamics Explorer 2 Magnetic Field Observations Triaxial Fluxgate Magnetometer
36) Dynamics Explorer 2 Vector Electric Field Instrument (VEFI) maxmize
Resource ID:spase://VMO/NumericalData/DE2/VEFI/AC/PT0.5S
Start:1981-08-10 16:00:00 Observatory:Dynamics Explorer 2 Cadence:0.5 seconds
Stop:1981-02-19 00:00:00 Instrument:Vector Electric Field Instrument (VEFI) Resource:NumericalData
Dynamics Explorer 2 Vector Electric Field Instrument AC Data
37) Double Star 1 Spacecraft Flux Gate Magnetometer (FGM) Prime Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar1/FGM/PrimeParameters/4S
Start:2004-01-08 03:43:36 Observatory:Double Star 1 Cadence:4 seconds
Stop:2007-09-16 10:41:55 Instrument:FGM (Flux Gate Magnetometer) Resource:NumericalData
The Double Star 1 Flux Gate Magnetometer (FGM) prime parameter data set contains various parameters in GSE coordinates at spin resolution. These parameters include universal time, the instrument status, the magnetic field vector in GSE coordinates, and the magnetic field variances. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.
38) Double Star 1 Spacecraft Flux Gate Magnetometer (FGM) Summary Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar1/FGM/SummaryParameters/60S
Start:2004-01-08 03:44:30 Observatory:Double Star 1 Cadence:60 seconds
Stop:2007-09-19 22:40:30 Instrument:FGM (Flux Gate Magnetometer) Resource:NumericalData
The Double Star 1 Flux Gate Magnetometer (FGM) summary parameter data set contains various parameters in GSE coordinates at 60 s resolution. These parameters include universal time, the instrument status, the magnetic field vector in GSE coordinates, and the magnetic field variances. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.
39) Double Star 1 Spacecraft Spatio-Temporal Analyzer of Field Fluctuations and Digital Wave Processor (STAFF-DWP) Prime Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar1/STAFF-DWP/PrimeParameters/4S
Start:2004-01-08 03:43:36 Observatory:Double Star 1 Cadence:4 seconds
Stop:2007-09-16 10:41:55 Instrument:STAFF-DWP (Spatio-Temporal Analyzer of Field Fluctuations and Digital Wave Processor Resource:NumericalData
The Double Star 1 Spatio-Temporal Analyzer of Field Fluctuations and Digital Wave Processor prime parameter data set contains various parameters at spin resolution. These parameters include universal time, the instrument status, and magnetic field spectral power from FGM data for various frequency ranges. Frequency ranges not clear. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.
40) Double Star 1 Spacecraft Spatio-Temporal Analyzer of Field Fluctuations and Digital Wave Processor (STAFF-DWP) Summary Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar1/STAFF-DWP/SummaryParameters/60S
Start:2004-01-08 03:43:36 Observatory:Double Star 1 Cadence:60 seconds
Stop:2007-09-16 10:41:55 Instrument:STAFF-DWP (Spatio-Temporal Analyzer of Field Fluctuations and Digital Wave Processor Resource:NumericalData
The Double Star 1 Spatio-Temporal Analyzer of Field Fluctuations and Digital Wave Processor summary parameter data set contains various parameters at 60 s. These parameters include universal time, the instrument status, and magnetic field spectral power from FGM data for various frequency ranges. Frequency ranges not clear. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.
41) Double Star 2 Spacecraft Flux Gate Magnetometer (FGM) Prime Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar2/FGM/PrimeParameters/4S
Start:2004-07-30 07:00:49 Observatory:Double Star 2 Cadence:4 seconds
Stop:2008-05-31 18:59:05 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
The Double Star 2 Flux Gate Magnetometer (FGM) prime parameter data set contains various parameters in GSE coordinates at spin resolution. These parameters include universal time, the instrument status, the magnetic field vector in GSE coordinates, and the magnetic field variances. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.
42) Double Star 2 Spacecraft Flux Gate Magnetometer (FGM) Summary Parameters Data maxmize
Resource ID:spase://VMO/NumericalData/DoubleStar2/FGM/SummaryParameters/60S
Start:2004-07-30 08:18:30 Observatory:Double Star 2 Cadence:60 seconds
Stop:2008-05-31 18:59:30 Instrument:Fluxgate Magnetometer (FGM) Resource:NumericalData
The Double Star 2 Flux Gate Magnetometer (FGM) summary parameter data set contains various parameters in GSE coordinates at 60 s resolution. These parameters include universal time, the instrument status, the magnetic field vector in GSE coordinates, and the magnetic field variances. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access.
43) FAST AC Fields, ~5 sec resolution maxmize
Resource ID:spase://VWO/NumericalData/FAST/ACF/PT5S
Start:1996-08-30 02:02:17 Observatory:FAST Cadence:5 seconds
Stop:2002-10-25 00:11:32 Instrument:Electric Field and Langmuir Probe Experiment Resource:NumericalData
FAST AC Fields Key Parameter CDF files consists of AC Electric and Magnetic fields measurements spanning a range from approximately 32 Hz to 2 MHz. The time range of each file is roughly 24 hours and consists of several passes over the auroral zone of approximately 20 minute duration, the time resolution is one spin period (approximately 5s). The orbital period of FAST is 133 minutes.
44) GOES 1 Magnetic Field Monitor at 3 sec Resolution in Spacecraft Coordinates maxmize
Resource ID:spase://VMO/NumericalData/GOES/1/MFM/PT3S
Start:1976-01-01 00:00:00 Observatory:GOES 1 Cadence:3 seconds
Stop:1978-05-31 00:00:00 Instrument:Biaxial Fluxgate Magnetometer Resource:NumericalData
A biaxial, closed-loop, fluxgate magnetometer was deployed on a boom about 0.61 m long. The magnetometer, which had one sensor aligned parallel to the spacecraft spin axis and the other perpendicular to this axis, measured the magnetic field at synchronous altitude. Each sensor had a selectable range (+50, 100, 200, or 400 nT), an offset field capability (plus or minus 1200 nT in 40-nT steps), and an inflight calibration capability.
45) GOES 10 high-resolution magnetometer data maxmize
Resource ID:spase://VMO/NumericalData/GOES/10/MAG/PT0.512S
Start:2006-12-31 23:59:58 Observatory:GOES 10 Cadence:0.512 seconds
Stop:2008-12-31 23:59:58 Instrument:GOES 10, Triaxial Fluxgate Magnetometer Resource:NumericalData
GOES 10 magnetic field data at 0.512 second time resolution. The vector magnetic field is given in the spacecraft (s/c) earth-referenced coordinate system: Hp, He, Hn, and Ht, where Hp is perpendicular to the satellite orbital plane, or parallel to Earth's spin axis in the case of a zero degree inclination orbit; He is perpendicular to Hp and directed earthwards; Hn is perpendicular to both Hp and He and directed eastwards; and Ht is the total field. This data product also provides GOES 10 satellite positions and velocities derived from SSCWEB GEI ephemeris, interpolated to one minute time resolution. The magnetometer data are downlinked from the spacecraft in real-time to the NOAA Space Weather Prediction Center (SWPC) in Boulder, CO. The data from the raw Command and Data Acquisition (CDA) telemetry stream are processed by pre-processors at SWPC and from there 1-minute averages are distributed to SWPC Space Weather Operations, as well a archived at NOAA?s National Geophysical Data Center (NGDC) and NASA?s Coordinated Data Analysis Web (http://cdaweb.gsfc.nasa.gov/). The raw high-resolution data are corrected and processed at NOAA?s SWPC, and later archived at NGDC. The major issue for processing the high-resolution data is correction for the magnetic signature of spacecraft torquer currents as briefly discussed in the magnetometer instrument descriptions. In normal operation, the magnetometer samples its three axes every 0.512 seconds, synchronized with the telemetry frames. The magnetometer has an anti-aliasing low-pass filter on each axis. As part of the attitude control on the spacecraft, there are two magnetic torquers. At the magnetometers, these torquers can generate magnetic fields larger than the ambient fields to be measured. Therefore signals from these torquer currents need to be removed. The torquer currents are measured at the same rate as the magnetometer rate, and the currents are used to correct the magnetometer measurements. However, the torquer currents were not low-pass filtered. As a result, large instantaneous steps in the torquer currents show up in the magnetometer data as a delayed, slowly rising wave with some ringing, just what one would expect from the magnetometer low-pass filters. The so-called ?Farthing coefficients? simulate, from a short past history of the torquer measurements, the effects of the magnetometer filters. The torquer current changes are asynchronous with the telemetry frames and the timing between these events must be measured to a eighth of a telemetry frame interval for good performance. The transient responses in changes in torquer currents are reduced, but not eliminated for large changes in torquer currents. There exists one opportunity at the beginning of each mission to perform a spacecraft rotation maneuver to determine magnetometer offsets. These offsets are used through the duration of each satellite's lifetime. Approximate coefficients are: * 0.8 milliampere per torquer current count * 4 counts per torquer current command step (3.2 milliampere per command step) * 410 milliamperes full scale current * 32 magnetometer counts per nT (approximate) * 8 torquer step counts can be up to approximately 0.5 nT (depends on axis, which torquer, which satellite, etc.)
46) GOES 10 Magnetometer 1-Minute Data maxmize
Resource ID:spase://VMO/NumericalData/GOES/10/MAG/PT1M
Start:1999-03-21 00:00:30 Observatory:GOES 10 Cadence:1 minute
Stop:2006-06-22 23:59:30 Instrument:GOES 10, Triaxial Fluxgate Magnetometer Resource:NumericalData
The NOAA Geostationary Operational Environment Satellite (GOES) key parameters. This data is a subset of the data available from the GOES Space Environment Monitor (SEM) instruments. It contains vector magnetic field in three coordinate systems: * (1) Spacecraft P,E,N * (2) GSM x,y,z and * (3) GSE x,y,z. Spacecraft magnetic field is defined as: * P - perpendicular to the spacecraft orbital plane or parallel to the Earth's spin axis in the case of a zero degree inclination orbit; * E - perpendicular to P and directed earhtwards; and * N - perpendicular to both P and E and directed eastwards.
47) GOES 10 Space Evironment Monitor Data at 5 min Resolution maxmize
Resource ID:spase://VMO/NumericalData/GOES/10/SEM/A/PT5M
Start:1998-08-01 00:00:00 Observatory:GOES 10 Cadence:5 minutes
Stop:2009-12-31 00:00:00 Instrument:Space Environment Monitor (SEM) Resource:NumericalData
This GOES 10 SEM data set contains various parameters at 5 min resolution. Within the data files is the Xray flux for two wavelength ranges, the magnetic field vectors, the >2 MeV uncorrected elecron fluxes, and the uncorrected alpha-particle fluxes for several energy ranges.
48) GOES 10 Space Evironment Monitor Data at 1 min Resolution maxmize
Resource ID:spase://VMO/NumericalData/GOES/10/SEM/G/PT1M
Start:1998-07-01 00:00:00 Observatory:GOES 10 Cadence:1 minute
Stop:2009-12-31 00:00:00 Instrument:Space Environment Monitor (SEM) Resource:NumericalData
This GOES 10 SEM data set contains various parameters at 1 min resolution. Within the data files is the Xray flux for two wavelength ranges, the magnetic field vectors, the >2 MeV uncorrected elecron fluxes, and the uncorrected proton fluxes for several energy ranges.
49) GOES 10 Space Evironment Monitor Data at 5 min Resolution maxmize
Resource ID:spase://VMO/NumericalData/GOES/10/SEM/G/PT5M
Start:1998-07-01 00:00:00 Observatory:GOES 10 Cadence:5 minutes
Stop:2009-12-31 00:00:00 Instrument:Space Environment Monitor (SEM) Resource:NumericalData
This GOES 10 SEM data set contains various parameters at 5 min resolution. Within the data files is the Xray flux for two wavelength ranges, the magnetic field vectors, the >2 MeV uncorrected elecron fluxes, and the uncorrected proton fluxes for several energy ranges.
50) GOES 10 Space Evironment Monitor Data at 5 min Resolution maxmize
Resource ID:spase://VMO/NumericalData/GOES/10/SEM/H/PT5M
Start:1998-07-01 00:00:00 Observatory:GOES 10 Cadence:5 minutes
Stop:2009-12-31 00:00:00 Instrument:Space Environment Monitor (SEM) Resource:NumericalData
This GOES 10 SEM data set contains various parameters at 5 min resolution. Within the data files is the Xray flux for two wavelength ranges, the magnetic field vectors, the >2 MeV uncorrected elecron fluxes, and the uncorrected proton and alpha particle fluxes for several energy ranges.
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