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1) 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.

2) 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

3) 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.

4) 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.

5) 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.

6) 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.

7) 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.

8) Van Allen Probe B Coordinates maxmize
Resource ID:spase://ViRBO/NumericalData/BAR/1A/L2/EPHM/2/PT4S
Start:2012-10-08 00:00:03 Observatory:Radiation Belt Storm Probe Satellite Cadence:1 second
Stop:2016-05-19 13:22:33 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Coordinates

9) Van Allen Probe B Fast time resolution (50ms) Bremsstrahlung X-ray spectrum. maxmize
Resource ID:spase://ViRBO/NumericalData/BAR/1A/L2/FSPC//PT.05S
Start:2012-10-08 00:00:03 Observatory:Radiation Belt Storm Probe Satellite Cadence:1 second
Stop:2016-05-19 13:22:32 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Fast time resolution (50ms) Bremsstrahlung X-ray spectrum.

10) Van Allen Probe B Fast time resolution (50ms) Bremsstrahlung X-ray spectrum. maxmize
Resource ID:spase://ViRBO/NumericalData/BAR/1A/L2/FSPC/2/PT.05S
Start:2012-10-08 00:00:03 Observatory:Radiation Belt Storm Probe Satellite Cadence:1 second
Stop:2016-05-19 13:22:33 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Fast time resolution (50ms) Bremsstrahlung X-ray spectrum.

11) Van Allen Probe B MAG X, Y, and Z maxmize
Resource ID:spase://ViRBO/NumericalData/BAR/1A/L2/MAGN/2/PT.25S
Start:2012-10-08 00:00:03 Observatory:Radiation Belt Storm Probe Satellite Cadence:1 second
Stop:2016-05-19 13:22:33 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
MAG X, Y, and Z

12) Van Allen Probe B Rate counters for scintillator diagnostics. maxmize
Resource ID:spase://ViRBO/NumericalData/BAR/1A/L2/RCNT/2/PT4S
Start:2012-10-08 00:00:03 Observatory:Radiation Belt Storm Probe Satellite Cadence:1 second
Stop:2016-05-19 13:22:33 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Rate counters for scintillator diagnostics.

13) Van Allen Probe B Slow time resolution (32s) X-ray spectrum maxmize
Resource ID:spase://ViRBO/NumericalData/BAR/1A/L2/SSPC/2/PT.03125S
Start:2012-10-08 00:00:03 Observatory:Radiation Belt Storm Probe Satellite Cadence:1 second
Stop:2016-05-19 13:22:33 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Slow time resolution (32s) X-ray spectrum

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:2016-05-19 13:23:49 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 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:2016-05-19 13:22:48 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.

16) 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:2016-05-19 13:22:48 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.

17) 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:2016-05-19 13:22:48 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.

18) 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:2016-05-19 13:23:48 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 ...

19) 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:2016-05-19 13:23:49 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 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:2016-05-19 13:23:48 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 ...

21) 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:2016-05-19 13:22:47 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.

22) 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:2016-05-19 13:22:47 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.

23) 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:2016-05-19 13:22:48 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.

24) 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

25) 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

26) 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

27) 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

28) 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.

29) 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.

30) 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.

31) 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.

32) 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.

33) Galileo PWS Earth Flyby Daily Dynamic Spectrograms Magnetic maxmize
Resource ID:spase://VWO/DisplayData/Galileo/PWS/DS.Magnetic.P1D
Start:1990-11-08 17:00:00 Observatory:Galileo Cadence:
Stop:1992-12-17 06:30:00 Instrument:Galileo PWS Resource:DisplayData
These PWS daily spectrograms cover the time range around the time of the Galileo spacecraft's two Earth flybys on its way to Jupiter. This dataset contains magnetic field spectrograms in units of magnetic field spectral density (nT^2/Hz) spanning 6 Hz to 75 kHz. An associated dataset contains electric field spectrograms in units of electric field spectral density (V^2/m^2/Hz) spanning 6 Hz to 5.6 MHz. The sources of this browse data set are the High Frequency Receiver, Sweep Frequency Receiver, and Spectrum Analyzer which make up the Low Rate Science portion of the PWS. The high frequency receiver data that appears in the uppermost panel of the spectrograms are only taken from the electric field antennas. During the time interval spanned by the first Earth flyby, Galileo approached Earth from the local early morning sector, made a close approach to Earth by passing through the magnetosphere, plasmasphere, ionosphere, and finally exited the Earth system in the local late morning. During the time interval spanned by the second Earth flyby, Galileo approached Earth from the local late evening sector, made a close approach to Earth by passing through the magnetosphere, plasmasphere, ionosphere, and finally exited the Earth system near local dawn. +-----------------------------------------------------+ | Flyby 1 | | 1990 November 8 1700 UT | - dataset start | | 1990 December 8 | - Earth closest approach | | 1990 December 18 1700 UT | - dataset end | +-----------------------------------------------------+ +-----------------------------------------------------+ | Flyby 2 | | 1992 November 6 2100 UT | - dataset start | | 1992 December 8 | - Earth closest approach | | 1992 December 17 0630 UT | - dataset ends | +-----------------------------------------------------+

34) Galileo PWS Summary Magnetic Field Dataset maxmize
Resource ID:spase://VWO/NumericalData/Galileo/PWS/Summary.Magnetic
Start:1995-12-07 15:21:00 Observatory:Galileo Cadence:60 seconds
Stop:2003-09-21 18:45:00 Instrument:Galileo PWS Resource:NumericalData
This data set includes 1-minute averages of the electric and magnetic wave spectra obtained during the period that the Galileo plasma wave receiver was operated during the Jupiter orbital mission (prime, GEM and GMM). The parameter provided for the electric field spectrum is the electric field spectral density in units of V**2/m**2/Hz. The magnetic field spectrum is provided in units of magnetic field spectral density, nT**2/Hz. The spectral information is averaged and binned into 49 logarithmically-spaced channels from about 6 Hz to 5.6 MHz for the electric measurements and 34 channels from about 6 Hz to 75 kHz for the magnetic. Note that these 'channels' do not generally correspond to the 158 specific channels described in the instrument description document. The reduction in spectral resolution for this data set was performed in order to make the set more conducive to use as a browse data set. The sources of this browse data set are the High Frequency Receiver, Sweep Frequency Receiver, and Spectrum Analyzer which make up the Low Rate Science portion of the PWS.

35) Geotail PWI 24 hour dynamic spectrograms maxmize
Resource ID:spase://VWO/DisplayData/Geotail/PWI/DS.P1D
Start:1992-09-18 00:00:00 Observatory:Geotail Cadence:
Stop:2016-05-19 13:23:47 Instrument:Geotail Plasma Wave Investigation (PWI) Resource:DisplayData
Geotail PWI SFA and MCA dynamic spectrogram plots with frequency in Hz on the vertical axis and time in UT on the horizontal axis. Each file contains one spectrogram from the electric field antennas and one from the magnetic field search coils. The electric field spectrograms span the frequency range 5.62 to 24 Hz (the Multi-Channel Analyzer - MCA instrument) and 24 Hz to 800 kHz (the Sweep Frequency Analyzer - SFA instrument). The intensity values are color coded and are expressed in units of dBV/m/root-Hz. The magnetic field spectrograms also combine the MCA and SFA instruments and span the frequency range 5.62 Hz to 12.5 kHz. The intensity values are color coded and are expressed in units of dB nT/root-Hz. Each plot spans 24 hours. Beneath the time axis of the magnetic field spectrogram are spacecraft GSM coordinates for every 4 hours. Information on the instrument and antenna status is also provided above each spectrogram.

36) Geotail PWI 2 hour dynamic spectrograms maxmize
Resource ID:spase://VWO/DisplayData/Geotail/PWI/DS.PT2H
Start:1992-09-18 00:00:00 Observatory:Geotail Cadence:
Stop:2016-05-19 13:23:47 Instrument:Geotail Plasma Wave Investigation (PWI) Resource:DisplayData
Geotail PWI SFA and MCA dynamic spectrogram plots with frequency in Hz on the vertical axis and time in UT on the horizontal axis. Each file contains one spectrogram from the electric field antennas and one from the magnetic field search coils. The electric field spectrograms span the frequency range 5.62 to 24 Hz (the Multi-Channel Analyzer - MCA instrument) and 24 Hz to 800 kHz (the Sweep Frequency Analyzer - SFA instrument). The intensity values are color coded and are expressed in units of dBV/m/root-Hz. The magnetic field spectrograms also combine the MCA and SFA instruments and span the frequency range 5.62 Hz to 12.5 kHz. The intensity values are color coded and are expressed in units of dB nT/root-Hz. Each plot spans 2 hours. Information on the instrument and antenna status is also provided above each spectrogram.

37) AGO P1 ICESTAR.Dayplot.Fluxgate Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P1/ICESTAR.Dayplot.Fluxgate/PT10S
Start:2003-01-04 00:00:00 Observatory:AGO P1 Cadence:10 seconds
Stop:2003-01-14 23:59:50 Instrument:AGO P1 Magnetometer Instrument Resource:DisplayData
AGO P1 ICESTAR.Dayplot.Fluxgate Dayplots

38) AGO P1 ICESTAR.Dayplot.Magnetometers Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P1/ICESTAR.Dayplot.Magnetometers/PT10S
Start:2003-12-25 00:00:00 Observatory:AGO P1 Cadence:10 seconds
Stop:2004-01-31 23:59:50 Instrument:AGO P1 Magnetometer Instrument Resource:DisplayData
AGO P1 ICESTAR.Dayplot.Magnetometers Dayplots

39) AGO P1 ICESTAR.Dayplot.Overview Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P1/ICESTAR.Dayplot.Overview/PT10S
Start:1996-01-01 00:00:00 Observatory:AGO P1 Cadence:10 seconds
Stop:2007-06-21 23:59:50 Instrument:AGO P1 Magnetometer Instrument Resource:DisplayData
AGO P1 ICESTAR.Dayplot.Overview Dayplots

40) AGO P1 ICESTAR.Dayplot.Searchcoil Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P1/ICESTAR.Dayplot.Searchcoil/PT10S
Start:2003-01-04 00:00:00 Observatory:AGO P1 Cadence:10 seconds
Stop:2003-01-14 23:59:50 Instrument:AGO P1 SearchCoil Instrument Resource:DisplayData
AGO P1 ICESTAR.Dayplot.Searchcoil Dayplots

41) AGO P2 ICESTAR.Dayplot.Fluxgate Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P2/ICESTAR.Dayplot.Fluxgate/PT10S
Start:2002-12-28 00:00:00 Observatory:AGO P2 Cadence:10 seconds
Stop:2003-12-17 23:59:50 Instrument:AGO P2 Magnetometer Instrument Resource:DisplayData
AGO P2 ICESTAR.Dayplot.Fluxgate Dayplots

42) AGO P2 ICESTAR.Dayplot.Magnetometers Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P2/ICESTAR.Dayplot.Magnetometers/PT10S
Start:2003-12-18 00:00:00 Observatory:AGO P2 Cadence:10 seconds
Stop:2004-02-01 23:59:50 Instrument:AGO P2 Magnetometer Instrument Resource:DisplayData
AGO P2 ICESTAR.Dayplot.Magnetometers Dayplots

43) AGO P2 ICESTAR.Dayplot.Overview Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P2/ICESTAR.Dayplot.Overview/PT10S
Start:1996-01-01 00:00:00 Observatory:AGO P2 Cadence:10 seconds
Stop:2007-06-21 23:59:50 Instrument:AGO P2 Magnetometer Instrument Resource:DisplayData
AGO P2 ICESTAR.Dayplot.Overview Dayplots

44) AGO P2 ICESTAR.Dayplot.Searchcoil Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P2/ICESTAR.Dayplot.Searchcoil/PT10S
Start:2002-12-28 00:00:00 Observatory:AGO P2 Cadence:10 seconds
Stop:2003-12-17 23:59:50 Instrument:AGO P2 SearchCoil Instrument Resource:DisplayData
AGO P2 ICESTAR.Dayplot.Searchcoil Dayplots

45) AGO P3 ICESTAR.Dayplot.Overview Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P3/ICESTAR.Dayplot.Overview/PT10S
Start:1996-01-01 00:00:00 Observatory:AGO P3 Cadence:10 seconds
Stop:1999-06-27 23:59:50 Instrument:AGO P3 Magnetometer Instrument Resource:DisplayData
AGO P3 ICESTAR.Dayplot.Overview Dayplots

46) AGO P4 ICESTAR.Dayplot.Overview Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P4/ICESTAR.Dayplot.Overview/PT10S
Start:1996-01-01 00:00:00 Observatory:AGO P4 Cadence:10 seconds
Stop:1998-12-01 23:59:50 Instrument:AGO P4 Magnetometer Instrument Resource:DisplayData
AGO P4 ICESTAR.Dayplot.Overview Dayplots

47) AGO P5 ICESTAR.Dayplot.Fluxgate Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P5/ICESTAR.Dayplot.Fluxgate/PT10S
Start:2003-01-14 00:00:00 Observatory:AGO P5 Cadence:10 seconds
Stop:2003-02-03 23:59:50 Instrument:AGO P5 Magnetometer Instrument Resource:DisplayData
AGO P5 ICESTAR.Dayplot.Fluxgate Dayplots

48) AGO P5 ICESTAR.Dayplot.Magnetometers Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P5/ICESTAR.Dayplot.Magnetometers/PT10S
Start:2003-12-24 00:00:00 Observatory:AGO P5 Cadence:10 seconds
Stop:2004-01-31 23:59:50 Instrument:AGO P5 Magnetometer Instrument Resource:DisplayData
AGO P5 ICESTAR.Dayplot.Magnetometers Dayplots

49) AGO P5 ICESTAR.Dayplot.Overview Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P5/ICESTAR.Dayplot.Overview/PT10S
Start:1997-01-01 00:00:00 Observatory:AGO P5 Cadence:10 seconds
Stop:2007-04-24 23:59:50 Instrument:AGO P5 Magnetometer Instrument Resource:DisplayData
AGO P5 ICESTAR.Dayplot.Overview Dayplots

50) AGO P5 ICESTAR.Dayplot.Searchcoil Dayplots maxmize
Resource ID:spase://VMO/DisplayData/ICESTAR/AGO.P5/ICESTAR.Dayplot.Searchcoil/PT10S
Start:2003-01-14 00:00:00 Observatory:AGO P5 Cadence:10 seconds
Stop:2003-02-03 23:59:50 Instrument:AGO P5 SearchCoil Instrument Resource:DisplayData
AGO P5 ICESTAR.Dayplot.Searchcoil Dayplots

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