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1) Aureol 3 VLF Data maxmize
Resource ID:spase://VSPO/NumericalData/Aureol3/ONCH-TBF/VLF/PT0.3S
Start:1981-09-30 00:00:00 Observatory:Aureol 3 Cadence:0.3 seconds
Stop:1984-07-21 23:59:59 Instrument:Electric and Magnetic Field Probes (ONCH-TBF) Resource:NumericalData
This data set contains power of electromagnetic wave components from narrow band (10%) filters at 140, 450, 800, 4500, and 15000 Hz. For any given time segment the power for any one of five predefined pairs of the five measurable field components (EZ, EH, BZ, BX, BX45) were measured and are included. The components of electromagnetic field are named by their direction in the satellite frame. Spacecraft position in geographic and magnetic coordinates are also included, along with time and an indication of which pair of components were measured. Each data file corresponds to one memory readout, and typically consists of a few continuous-data segments. The first several records in each file constitute a header giving the time spans of the segments, the time resolution, and other common information. The data records are in ASCII.

2) 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:2016-09-14 07:56:57 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Coordinates

3) 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:2016-09-14 07:56:57 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Fast time resolution (50ms) Bremsstrahlung X-ray spectrum.

4) 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:2016-09-14 07:56:57 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Fast time resolution (50ms) Bremsstrahlung X-ray spectrum.

5) 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:2016-09-14 07:56:57 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
MAG X, Y, and Z

6) 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:2016-09-14 07:56:57 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Rate counters for scintillator diagnostics.

7) 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:2016-09-14 07:56:57 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Slow time resolution (32s) X-ray spectrum

8) Cluster Rumba Wide Band Data (WBD) Plasma Waves at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Rumba/WBD/CSA/PT0.000035S
Start:2001-02-04 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:0.000035 seconds
Stop:2006-12-30 03:59:59 Instrument:Wide Band Data (WBD) Resource:NumericalData
The Cluster Wide Band Data (WBD) products at the Cluster Active Archive include full time resolution calibrated waveform data obtained in one of three frequency bandwidths: 9.5 kHz, 19 kHz, or 77 kHz in the range of 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. Calibrated electric field data are divided by 1000 to get V m^-1. Because of the high sampling rate of the WBD data (27.4 to 219.5 kilosamples per second), the time resolution of the WBD data (~36 to 5 microseconds in the time domain) is very high. This results in a very large data volume. Because of this the WBD data are stored in CEF files (and in CDF files from which the CEF files were generated) with maximum length of 10 minutes and size of a few hundred Mbytes. The user of WBD data is thus cautioned to take this into consideration when requesting WBD data downloads from the CAA. The 10 minute CDF files can also be downloaded from NASA's CDAWeb. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet.

9) Cluster Rumba WBD High Time Resolution Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Cluster-Rumba/WBD/DS.GIF.PT30S
Start:2001-02-03 05:26:00 Observatory:Cluster FM5 (Rumba) Cadence:
Stop:2016-09-14 08:00:14 Instrument:Wide Band Data (WBD) Resource:DisplayData
This dataset contains 30 s duration survey spectrogram plots from the WBD instrument on the Cluster spacecraft. The spectrograms are created by 1024 point FFTs and plotted with frequency on the vertical axis, increasing time on the horizontal, and color indicating power spectral density, in relative dB. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW 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 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 are sampled at 4.6 microseconds in the time domain, 4.7 milliseconds in the frequency domain (generally the 77 kHz bandwidth mode). The lowest time resolution data are sampled at 36.5 microseconds in the time domain, 37.3 milliseconds in the frequency domain (generally the 9.5 kHz bandwidth mode). Above the spectrogram plot are a line plot panel, followed by four status lines. The line plot panel at the top provides the gain state (0 to 75 dB, in 5 dB steps) of the instrument. The four status lines provide the following information according to the color code in the upper right corner: Data mode - whether from DSN mode (real time telemetry), or from BM2 mode (recorded onboard in Burst Mode 2) as digitally filtered or duty cycled. Antenna - the electric field (Ey or Ez) or the magnetic field (Bx or By) antenna used. Resolution - the data digitization level, which can be 1 bit, 4 bit or 8 bit. Translation - the translation from base frequency of 0 kHz. In the lower right-hand corner are the ephemeris values applicable to the start time of the plot. At the middle right-hand side are given the date and start time of the plot as well as the spacecraft number. The University of Iowa repository maintains two types of high time resolution spectrogram plots in GIF format: a ten minute (PT10M Display Cadence) and a 30 second time span (PT30S Display Cadence). Both types of files provide information on WBD gain and operational mode, the spectral data from one spacecraft, the start date and time and ephemeris data. Overview spectrograms are also available. The availability of these files depends on times of DSN and Pansak 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 (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues can be found at http://www-pw.physics.uiowa.edu/cluster/interpretation_issues/interpretation.html 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.

10) 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:2016-09-14 08:00:14 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 ...

11) 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:2016-09-14 07:58:16 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.

12) Cluster Salsa Wide Band Data (WBD) Data at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Salsa/FGM/CSA/PT0.000005S
Start:2001-02-04 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:0.000005 seconds
Stop:2006-12-04 03:59:59 Instrument:Wide Band Data (WBD) Resource:NumericalData
The Cluster Wide Band Data (WBD) products at the Cluster Active Archive include full time resolution calibrated waveform data obtained in one of three frequency bandwidths: 9.5 kHz, 19 kHz, or 77 kHz in the range of 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. Calibrated electric field data are divided by 1000 to get V m^-1. Because of the high sampling rate of the WBD data (27.4 to 219.5 kilosamples per second), the time resolution of the WBD data (~36 to 5 microseconds in the time domain) is very high. This results in a very large data volume. Because of this the WBD data are stored in CEF files (and in CDF files from which the CEF files were generated) with maximum length of 10 minutes and size of a few hundred Mbytes. The user of WBD data is thus cautioned to take this into consideration when requesting WBD data downloads from the CAA. The 10 minute CDF files can also be downloaded from NASA's CDAWeb. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet.

13) Cluster Salsa WBD High Time Resolution Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Cluster-Salsa/WBD/DS.GIF.PT30S
Start:2001-02-03 05:26:00 Observatory:Cluster FM6 (Salsa) Cadence:
Stop:2016-09-14 08:00:14 Instrument:Wide Band Data (WBD) Resource:DisplayData
This dataset contains 30 s duration survey spectrogram plots from the WBD instrument on the Cluster spacecraft. The spectrograms are created by 1024 point FFTs and plotted with frequency on the vertical axis, increasing time on the horizontal, and color indicating power spectral density, in relative dB. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW 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 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 are sampled at 4.6 microseconds in the time domain, 4.7 milliseconds in the frequency domain (generally the 77 kHz bandwidth mode). The lowest time resolution data are sampled at 36.5 microseconds in the time domain, 37.3 milliseconds in the frequency domain (generally the 9.5 kHz bandwidth mode). Above the spectrogram plot are a line plot panel, followed by four status lines. The line plot panel at the top provides the gain state (0 to 75 dB, in 5 dB steps) of the instrument. The four status lines provide the following information according to the color code in the upper right corner: Data mode - whether from DSN mode (real time telemetry), or from BM2 mode (recorded onboard in Burst Mode 2) as digitally filtered or duty cycled. Antenna - the electric field (Ey or Ez) or the magnetic field (Bx or By) antenna used. Resolution - the data digitization level, which can be 1 bit, 4 bit or 8 bit. Translation - the translation from base frequency of 0 kHz. In the lower right-hand corner are the ephemeris values applicable to the start time of the plot. At the middle right-hand side are given the date and start time of the plot as well as the spacecraft number. The University of Iowa repository maintains two types of high time resolution spectrogram plots in GIF format: a ten minute (PT10M Display Cadence) and a 30 second time span (PT30S Display Cadence). Both types of files provide information on WBD gain and operational mode, the spectral data from one spacecraft, the start date and time and ephemeris data. Overview spectrograms are also available. The availability of these files depends on times of DSN and Pansak 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 (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues can be found at http://www-pw.physics.uiowa.edu/cluster/interpretation_issues/interpretation.html 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.

14) 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:2016-09-14 08:00:15 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 Wide Band Data (WBD) Prime Parameters maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Salsa/WBD/PrimeParameter/PT0.02S
Start:2001-02-04 13:45:07 Observatory:Cluster FM6 (Salsa) Cadence:0.02 seconds
Stop:2002-07-29 10:15:25 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 Samba Wide Band Data (WBD) Plasma Waves at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/WBD/CSA/PT0.000035S
Start:2001-02-04 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:0.000035 seconds
Stop:2006-12-30 03:59:59 Instrument:Wide Band Data (WBD) Resource:NumericalData
The Cluster Wide Band Data (WBD) products at the Cluster Active Archive include full time resolution calibrated waveform data obtained in one of three frequency bandwidths: 9.5 kHz, 19 kHz, or 77 kHz in the range of 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. Calibrated electric field data are divided by 1000 to get V m^-1. Because of the high sampling rate of the WBD data (27.4 to 219.5 kilosamples per second), the time resolution of the WBD data (~36 to 5 microseconds in the time domain) is very high. This results in a very large data volume. Because of this the WBD data are stored in CEF files (and in CDF files from which the CEF files were generated) with maximum length of 10 minutes and size of a few hundred Mbytes. The user of WBD data is thus cautioned to take this into consideration when requesting WBD data downloads from the CAA. The 10 minute CDF files can also be downloaded from NASA's CDAWeb. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet.

17) Cluster Samba WBD High Time Resolution Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Cluster-Samba/WBD/DS.GIF.PT30S
Start:2001-02-03 05:26:00 Observatory:Cluster FM7 (Samba) Cadence:
Stop:2016-09-14 08:00:14 Instrument:Wide Band Data (WBD) Resource:DisplayData
This dataset contains 30 s duration survey spectrogram plots from the WBD instrument on the Cluster spacecraft. The spectrograms are created by 1024 point FFTs and plotted with frequency on the vertical axis, increasing time on the horizontal, and color indicating power spectral density, in relative dB. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW 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 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 are sampled at 4.6 microseconds in the time domain, 4.7 milliseconds in the frequency domain (generally the 77 kHz bandwidth mode). The lowest time resolution data are sampled at 36.5 microseconds in the time domain, 37.3 milliseconds in the frequency domain (generally the 9.5 kHz bandwidth mode). Above the spectrogram plot are a line plot panel, followed by four status lines. The line plot panel at the top provides the gain state (0 to 75 dB, in 5 dB steps) of the instrument. The four status lines provide the following information according to the color code in the upper right corner: Data mode - whether from DSN mode (real time telemetry), or from BM2 mode (recorded onboard in Burst Mode 2) as digitally filtered or duty cycled. Antenna - the electric field (Ey or Ez) or the magnetic field (Bx or By) antenna used. Resolution - the data digitization level, which can be 1 bit, 4 bit or 8 bit. Translation - the translation from base frequency of 0 kHz. In the lower right-hand corner are the ephemeris values applicable to the start time of the plot. At the middle right-hand side are given the date and start time of the plot as well as the spacecraft number. The University of Iowa repository maintains two types of high time resolution spectrogram plots in GIF format: a ten minute (PT10M Display Cadence) and a 30 second time span (PT30S Display Cadence). Both types of files provide information on WBD gain and operational mode, the spectral data from one spacecraft, the start date and time and ephemeris data. Overview spectrograms are also available. The availability of these files depends on times of DSN and Pansak 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 (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues can be found at http://www-pw.physics.uiowa.edu/cluster/interpretation_issues/interpretation.html 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.

18) 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:2016-09-14 08:00:15 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 Samba Wide Band Data (WBD) Prime Parameters maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Samba/WBD/PrimeParameter/PT0.02S
Start:2001-02-03 00:00:00 Observatory:Cluster FM7 (Samba) Cadence:0.02 seconds
Stop:2002-07-29 09:00:00 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.

20) Cluster Tango Wide Band Data (WBD) Plasma Waves at the ESA Cluster Science Archive maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Tango/WBD/CSA/PT0.000035S
Start:2001-02-04 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:0.000035 seconds
Stop:2006-12-30 03:59:59 Instrument:Wide Band Data (WBD) Resource:NumericalData
The Cluster Wide Band Data (WBD) products at the Cluster Active Archive include full time resolution calibrated waveform data obtained in one of three frequency bandwidths: 9.5 kHz, 19 kHz, or 77 kHz in the range of 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. Calibrated electric field data are divided by 1000 to get V m^-1. Because of the high sampling rate of the WBD data (27.4 to 219.5 kilosamples per second), the time resolution of the WBD data (~36 to 5 microseconds in the time domain) is very high. This results in a very large data volume. Because of this the WBD data are stored in CEF files (and in CDF files from which the CEF files were generated) with maximum length of 10 minutes and size of a few hundred Mbytes. The user of WBD data is thus cautioned to take this into consideration when requesting WBD data downloads from the CAA. The 10 minute CDF files can also be downloaded from NASA's CDAWeb. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet.

21) Cluster Tango WBD High Time Resolution Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Cluster-Tango/WBD/DS.GIF.PT30S
Start:2001-02-03 05:26:00 Observatory:Cluster FM8 (Tango) Cadence:
Stop:2016-09-14 08:00:14 Instrument:Wide Band Data (WBD) Resource:DisplayData
This dataset contains 30 s duration survey spectrogram plots from the WBD instrument on the Cluster spacecraft. The spectrograms are created by 1024 point FFTs and plotted with frequency on the vertical axis, increasing time on the horizontal, and color indicating power spectral density, in relative dB. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW 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 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 are sampled at 4.6 microseconds in the time domain, 4.7 milliseconds in the frequency domain (generally the 77 kHz bandwidth mode). The lowest time resolution data are sampled at 36.5 microseconds in the time domain, 37.3 milliseconds in the frequency domain (generally the 9.5 kHz bandwidth mode). Above the spectrogram plot are a line plot panel, followed by four status lines. The line plot panel at the top provides the gain state (0 to 75 dB, in 5 dB steps) of the instrument. The four status lines provide the following information according to the color code in the upper right corner: Data mode - whether from DSN mode (real time telemetry), or from BM2 mode (recorded onboard in Burst Mode 2) as digitally filtered or duty cycled. Antenna - the electric field (Ey or Ez) or the magnetic field (Bx or By) antenna used. Resolution - the data digitization level, which can be 1 bit, 4 bit or 8 bit. Translation - the translation from base frequency of 0 kHz. In the lower right-hand corner are the ephemeris values applicable to the start time of the plot. At the middle right-hand side are given the date and start time of the plot as well as the spacecraft number. The University of Iowa repository maintains two types of high time resolution spectrogram plots in GIF format: a ten minute (PT10M Display Cadence) and a 30 second time span (PT30S Display Cadence). Both types of files provide information on WBD gain and operational mode, the spectral data from one spacecraft, the start date and time and ephemeris data. Overview spectrograms are also available. The availability of these files depends on times of DSN and Pansak 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 (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues can be found at http://www-pw.physics.uiowa.edu/cluster/interpretation_issues/interpretation.html 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.

22) 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:2016-09-14 08:00:15 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 ...

23) Cluster Tango Wide Band Data (WBD) Prime Parameters maxmize
Resource ID:spase://VSPO/NumericalData/Cluster-Tango/WBD/PrimeParameter/PT0.02S
Start:2001-03-26 00:00:00 Observatory:Cluster FM8 (Tango) Cadence:0.02 seconds
Stop:2002-07-28 19:00:00 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.

24) Cluster WBD Survey Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Cluster/WBD/Survey.PNG.PT2H
Start:2001-02-03 05:26:00 Observatory:Cluster FM5 (Rumba) Cadence:
Stop:2016-09-14 08:00:14 Instrument:Wide Band Data (WBD) Resource:DisplayData
This dataset contains survey spectrogram plots of varying time durations from the WBD Plasma Wave Receivers on the four Cluster spacecraft. Due to the nature of the WBD real-time operations at the DSN, data from all four spacecraft are not always available. The time span of these plots varies based on the time span of the telemetry received in real-time from the DSN and Panska Ves ground stations and can range from 30 minutes to 8 hours, 2 hours being typical. Panels are included in the overview plots for all of the spacecraft for which WBD data are available at any given time. The spectrograms are created by 1024 point FFTs and plotted with frequency in kHz on the vertical axis, increasing time on the horizontal, and color indicating the power spectral density. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW 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 instrument as a sensor. When the data shown in the overview plot are from an electric field antenna, the power spectral density is given in units of V^2/m^2/Hz. When the data shown in the overview plot are the WBD magnetic field measurements, the power spectral density is given in relative dB. The WBD antenna used is marked on the left-hand side of each plot panel, and the spacecraft name and number are provided on the right-hand side of each panel. Below the time labels on the horizontal axis, are the ephemeris values applicable to the times marked on the horizontal axis. The ephemeris values are provided for the spacecraft whose data are shown in the bottom panel of the plot, just above the time axis labels. These ephemeris values are provided only as an indication of the general location of the Cluster quartet within the magnetosphere. Due to varying spacecraft separations, the ephemeris values for the spacecraft shown in the other plot panels may be considerably different from the values given for the spacecraft in the bottom panel. At the very bottom of the page are given the date and start time of the plots. At the top of the page, the WBD mode is noted, along with the FFT length and overlap. 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. There will typically be a separate survey spectrogram plot for each operating mode. The time resolution of the data shown in the plots is determined from the WBD instrument mode and FFT length. The highest time resolution data are sampled at 4.6 microseconds in the time domain, 4.7 milliseconds in the frequency domain (generally the 77 kHz bandwidth mode). The lowest time resolution data are sampled at 36.5 microseconds in the time domain, 37.3 milliseconds in the frequency domain (generally the 9.5 kHz bandwidth mode). When data from multiple spacecraft are shown in the overview plots, the time span in which WBD data are available for each spacecraft may be different. Periods when no data were available will appear white on the overview plots. On the lower right-hand corner of the page, UIowa appears next to the date on which the plot was generated in the format YYMMDD. Please note that during operations in certain magnetospheric regions, the WBD Plasma Wave Receiver may cycle between electric and magnetic field antennas or through the 125.454 kHz, 250.908 kHz, and 501.816 kHz conversion frequencies. When the instrument cycles through different modes, separate ps overview plots are generated for each antenna or conversion frequency used over the entire duration of the operation. In these plots, only data from one mode are shown on each plot, and the data are dilated across the intervals when another mode was used. The modes used and the length of the cycling intervals are provided on the left-hand side of the ps overview plot, along with a note that the plot is not intended for publication. Please contact the WBD PI if you wish to publish or present data from periods with cyclical switching between instrument modes. Higher time resolution spectrograms are also available for each spacecraft separately. These data are presented as ten minute time span and 30 second time span GIF image files. Details on Cluster WBD Interpretation Issues can be found at http://www-pw.physics.uiowa.edu/cluster/interpretation_issues/interpretation.html 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 (http://caa.estec.esa.int/caa). 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.

25) Cluster WBD Spectrograms maxmize
Resource ID:spase://VSPO/DisplayData/Cluster/WBD/UIOWA
Start:2000-12-10 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:
Stop:2016-09-14 07:59:48 Instrument:Wide Band Data (WBD) Resource:DisplayData
Cluster WBD Spectrograms, E and B in 25 Hz to 577 kHz range

26) Geotail PWI 64-sec Key Parameters maxmize
Resource ID:spase://VSPO/NumericalData/GEOTAIL/PWI/KP/PT64S
Start:1992-09-08 07:30:05 Observatory:Geotail Cadence:64 seconds
Stop:2016-09-14 07:59:51 Instrument:Geotail Plasma Wave Investigation (PWI) Resource:NumericalData
This set of key paraments from the Geotail Plasma Wave Instrument includes: Peak and average electric and magnetic spectra from the multichannel analyzer MCA (at 5 frequencies from 5.6 Hz to 311 kHz for the electric antenna and at 4 frequencies from 5.6 Hz to 10 kHz for the magnetic coils); Peak and average spectra intentsities (scala only) averaged over 64 seconds from the Sweep Frequency Analyzer SFA (24 Hz to 800 kHz); Frequency corresponding to the peak of the spectral intensities (scalar only); and spacecraft position in GSE cartesian coordinates.

27) 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:2016-09-14 08:00:14 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.

28) 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:2016-09-14 08:00:14 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.

29) GPS Total Electron Content (TEC) 2-hr data maxmize
Resource ID:spase://VSPO/NumericalData/IGS/GPS_Receiver/TEC/PT120M
Start:1998-06-01 00:00:00 Observatory:International GNSS Service (IGS) Cadence:120 minutes
Stop:2016-09-14 07:59:52 Instrument:International GNSS Service (IGS) GPS Receiver Resource:NumericalData
This date set contains total electron content (TEC) and global ionospheric maps estimated every two hours by the International GNSS Service (IGS) Analysis Centre. IGS uses the averages of 4 methods, including CODE (U Bern Switzerland), ESA (ESOC Darmstadt Germany), JPL (Jet Propulsion Lab. in Pasadena USA), and UPC (U Politec. Catalonia Barcelona Spain). The data set contains rapid and final TEC global maps and movies of TEC (10^16 m-2) in cylindrical projection; rapid and final RMS maps and errors of TEC in cylindrical projection; and rapid and final TEC maps and movies in polar projection. Continuous coverage is not guaranteed.

30) GPS Total Electron Content (TEC) 15-min data maxmize
Resource ID:spase://VSPO/NumericalData/IGS/GPS_Receiver/TEC/PT15M
Start:2010-04-10 00:00:00 Observatory:International GNSS Service (IGS) Cadence:15 minutes
Stop:2016-09-14 07:59:52 Instrument:International GNSS Service (IGS) GPS Receiver Resource:NumericalData
This date set contains total electron content (TEC) and global ionospheric maps estimated every 15 minutes by the International GNSS Service (IGS) Analysis Centre. IGS uses the averages of 4 methods, including CODE (U Bern Switzerland), ESA (ESOC Darmstadt Germany), JPL (Jet Propulsion Lab. in Pasadena USA), and UPC (U Politec. Catalonia Barcelona Spain). The data set contains rapid TEC global maps and movies of TEC (10^16 m-2) in cylindrical projection; rapid RMS maps and errors of TEC in cylindrical projection; and rapid TEC maps and movies in polar projection. Continuous coverage is not guaranteed.

31) GPS Total Electron Content (TEC) 1-hr data maxmize
Resource ID:spase://VSPO/NumericalData/IGS/GPS_Receiver/TEC/PT60M
Start:2010-10-01 00:00:00 Observatory:International GNSS Service (IGS) Cadence:60 minutes
Stop:2016-09-14 07:59:52 Instrument:International GNSS Service (IGS) GPS Receiver Resource:NumericalData
This date set contains total electron content (TEC) and global ionospheric maps estimated every hour by the International GNSS Service (IGS) Analysis Centre. IGS uses the averages of 4 methods, including CODE (U Bern Switzerland), ESA (ESOC Darmstadt Germany), JPL (Jet Propulsion Lab. in Pasadena USA), and UPC (U Politec. Catalonia Barcelona Spain). The data set contains rapid TEC global maps and movies of TEC (10^16 m-2) in cylindrical projection; rapid RMS maps and errors of TEC in cylindrical projection; and rapid TEC maps and movies in polar projection. Continuous coverage is not guaranteed.

32) Injun 5 VLF Electric and Magnetic Field Data maxmize
Resource ID:spase://VSPO/NumericalData/Injun5/VLF/Field/PT0.001S
Start:1968-08-29 00:00:00 Observatory:Injun 5 Cadence:0.001 seconds
Stop:1968-11-25 00:00:00 Instrument:Injun 5 Very Low Frequency (VLF) Receiver Resource:NumericalData
This set of data came from the Injun 5 Very Low Frequency experiment that covered the frequency range from dc to 105 kHz for electric fields and from 30 Hz to 10 kHz for magnetic fields. Magnitudes of naturally occurring magnetospheric electric fields were measured to an accuracy of 30 mv/m. Each record covers ten milliseconds of data.

33) Polar Plasma Wave Instrument, High Frequency Waveform Receiver, 25kHz bandwidth interferometry fields maxmize
Resource ID:spase://VWO/NumericalData/POLAR/PWI/HFWR.25kHz.Interferometry.PT0.000014S
Start:1996-04-04 15:00:00 Observatory:POLAR Cadence:0.000014 seconds
Stop:1997-09-14 19:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
PWI>Plasma Wave Instrument Reference: Gurnett, D.A. et al, The Polar Plasma Wave Instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995. donald-gurnett@uiowa.edu An FFT on 1024 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series. Coordinate system used: antenna coordinate system, where the u-axis is offset by -45 degrees from the spacecraft x-axis, the v-axis is offset by -45 degrees from the spacecraft y-axis, and the z-axis is identical to the spacecraft z-axis. Effective bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t. These data come in snapshots of 190902 points distributed among 2 to 6 channels every 9.2 seconds, where the duration of the snapshot is 0.045 seconds. Since Epoch time is in milliseconds, the times for the data points will not be unique unless the Delta_T in milliseconds is added to the Epoch time for the snapshot. The unattenuated frequency range for this file type is 20Hz to 25000Hz. The cadence value given here is computed from the inverse of the sampling rate (71.43 kHz). For a description of the PWI receivers and the different operational modes see: http://www-pw.physics.uiowa.edu/plasma-wave/istp/polar/modes.html

34) Polar Plasma Wave Instrument, High Frequency Waveform Receiver, 25kHz bandwidth, 6-channel fields maxmize
Resource ID:spase://VWO/NumericalData/POLAR/PWI/HFWR.25kHz.PT0.000014S
Start:1996-03-26 15:00:00 Observatory:POLAR Cadence:0.000014 seconds
Stop:1997-09-16 17:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
PWI>Plasma Wave Instrument Reference: Gurnett, D.A. et al, The Polar Plasma Wave Instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995. donald-gurnett@uiowa.edu An FFT on 1024 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series. Coordinate system used: local magnetic field-aligned, a spacecraft centered coordinate system where Z is parallel to the local B-field determined from Polar MFE, X points outward and lies in the plane defined by the Z-axis and the radial vector from the earth to the spacecraft, and Y completes a right-handed system and points eastward. The X- and Z-axes are contained in the north-south plane. Effective bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t. These data come in snapshots of 31816 points per channel, every 9.2 seconds, where the duration of each snapshot is 0.045 seconds. The time for individual samples is the epoch time of the snapshot incremented by delta_t in milliseconds for each successive sample. That is: sample_time = epoch_time + sample_offset * delta_t The data in this file will be in sets of 31744 (31*1024) points per channel because the FFT size does not come out even within the number of points per snapshot. To obtain the time for each point in the snapshot, increment each Epoch time after the first with Delta_T (in ms). The unattenuated frequency range for this file type is 20Hz to 25000Hz. The cadence value given here is computed from the inverse of the sampling rate (71.43 kHz). For a description of the PWI receivers and the different operational modes see: http://www-pw.physics.uiowa.edu/plasma-wave/istp/polar/modes.html

35) Polar PWI Key Parameters maxmize
Resource ID:spase://VSPO/NumericalData/POLAR/PWI/KeyParameters/PT300S
Start:1996-02-27 12:20:27 Observatory:POLAR Cadence:300 seconds
Stop:1997-09-16 16:51:41 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
This set of key parameters comes from the Polar Plasma Wave Instrument. The data set contains the observed electron, proton, and oxygen cyclotron frequencies, plus the average and peak electric and magnetic fields in 160 frequencies from the two swept frequency receivers (SFRs), at 5-minute resolution. Additional related mode and antenna information is also given, plus spacecraft position in magnetic coordinates, and the variables Epoch (Time standard for CDF) and Time_PB5 (Time standard for ISTP data). The electron, ion and cyclotron frequencies are derived from the following: Fce = 0.028 kHz*B, where B is the magnitude of the ambient magnetic field measured in nT. Fcp = Fce/1837 in kHz. FcO+ = Fcp/16 in kHz. All frequencies in the Key parameters are converted to Hz. Since the SFR frequency steps vary with the mode, the measured SFR frequencies will be mapped to a fixed array of 160 approximately logarithmically spaced frequency values, 32 frequency values for each of the five SFR channels. In the log mode, the 64 frequency steps of the fourth and fifth frequency channels will be mapped to 32 frequency steps each, using geometric averaging. In the linear mode, the 448 linearly spaced frequency steps of the five frequency channels will be mapped to the fixed array of 160 logarithmically spaced frequency values using a windowing technique. The magnetic and electric field values corresponding to each SFR frequency step will be similarly mapped to 160-point fixed arrays corresponding to the mapped frequency array.

36) Polar Plasma Wave Instrument, Low Frequency Waveform Receiver, ~0.01 sec resolution fields maxmize
Resource ID:spase://VWO/NumericalData/POLAR/PWI/LFWR.PT0.01S
Start:1996-03-25 00:00:16 Observatory:POLAR Cadence:0.01 seconds
Stop:1997-09-16 16:52:55 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
The Low-Frequency Waveform Receiver (LFWR) is designed to provide an extension of the High Frequency Waveform Receiver into the frequency range below 25 Hz. The LFWR consists of six parallel low-pass filters connected to the three orthogonal electric field sensors and to the triaxial search coils. The input signals are band limited to a frequency range from 0.1 to 25 Hz and are sam- pled by a 12-bit analog-to-digital converter. The six LFWR channels are sampled simultaneously at a rate of 100 samples s-1. The dynamic range of the LFWRis approximately 72 dB with fixed gain. An FFT on 256 or 464 values, depending on the snapshot size, was used in calibrating the data; i.e., perform FFT, calibrate andin frequency domain, perform inverse FFT to get calibrated time series. Coordinate System Used: local magnetic field-aligned, a spacecraft centered coordinate system where Z is parallel to the local B-field determined from Polar MFE, X points outward and lies in the plane defined by the Z-axis and the radial vector from the earth to the spacecraft, and Y completes a right-handed system and points eastward. The X- and Z-axes are contained in the north-south plane. The three orthogonal magnetic field components are given in units of nT/Sec rather than nT because the response of the searchcoils across the passband is not flat. In order to obtain units of nT, the data would need to be digitally filtered to the frequency of interest and then integrated over time. Integrating over the entire passband could possibly destroy the resolution of the higher frequency components since the low frequency noise, if present, will dominate. Data are bandpass filtered. The valid range of data in the frequency domain is from 0.5 to 22.5 Hz. Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.

37) Polar Plasma Wave Instrument, High Frequency Waveform Receiver, 16 kHz, Time Domain Fields. maxmize
Resource ID:spase://VWO/NumericalData/POLAR/PWI/LHFWR.16kHz.Interferometry.PT0.000028S
Start:1996-03-25 00:00:00 Observatory:POLAR Cadence:0.000028 seconds
Stop:1997-09-15 00:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
The unattenuated frequency range for this file type is 20Hz to 16000Hz. The cadence value given here is computed from the inverse of the sampling rate (35.71 kHz). For a description of the PWI receivers and the different operational modes see: http://www-pw.physics.uiowa.edu/plasma-wave/istp/polar/modes.html

38) Polar Plasma Wave Instrument, High Frequency Waveform Receiver, 16 kHz bandwidth, 6-channel Fields maxmize
Resource ID:spase://VWO/NumericalData/POLAR/PWI/LHFWR.16kHz.PT0.000028S
Start:1996-03-25 00:00:00 Observatory:POLAR Cadence:0.000028 seconds
Stop:1997-09-17 00:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
PWI>Plasma Wave Instrument Reference: Gurnett, D.A. et al, The Polar Plasma Wave Instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995. donald-gurnett@uiowa.edu An FFT on 1024 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series. Coordinate system used: local magnetic field-aligned, a spacecraft centered coordinate system where Z is parallel to the local B-field determined from Polar MFE, X points outward and lies in the plane defined by the Z-axis and the radial vector from the earth to the spacecraft, and Y completes a right-handed system and points eastward. The X- and Z-axes are contained in the north-south plane. Effective bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t. These data come in snapshots of 31816 points per channel, every 9.2 seconds, where the duration of each snapshot is 0.045 seconds. The time for individual samples is the epoch time of the snapshot incremented by delta_t in milliseconds for each successive sample. That is: sample_time = epoch_time + sample_offset * delta_t The data in this file will be in sets of 31744 (31*1024) points per channel because the FFT size does not come out even within the number of points per snapshot. To obtain the time for each point in the snapshot, increment each Epoch time after the first with Delta_T (in ms). The unattenuated frequency range for this file type is 20Hz to 16000Hz. The cadence value given here is computed from the inverse of the sampling rate (35.71 kHz). For a description of the PWI receivers and the different operational modes see: http://www-pw.physics.uiowa.edu/plasma-wave/istp/polar/modes.html

39) Polar Plasma Wave Instrument, High Frequency Waveform Receiver, 2 kHz, Time Domain Fields maxmize
Resource ID:spase://VWO/NumericalData/POLAR/PWI/LHFWR.2kHz.PT0.000224S
Start:1996-03-26 00:00:00 Observatory:POLAR Cadence:0.000224 seconds
Stop:1997-09-17 00:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
An FFT on 2048 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series. Data are lowpass filtered so that the data are valid only up to 2 kHz. The three orthogonal magnetic field components are given in units of nT/Sec rather than nT because the response of the searchcoils across the passband is not flat. In order to obtain units of nT, the data would need to be digitally filtered to the frequency of interest and then integrated over time. Integrating over the entire passband could possibly destroy the resolution of the higher frequency components since the low frequency noise, if present, will dominate. Effective Bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t. The unattenuated frequency range for this file type is 20Hz to 2000Hz. The cadence value given here is computed from the inverse of the sampling rate (4.46 kHz). For a description of the PWI receivers and the different operational modes see: http://www-pw.physics.uiowa.edu/plasma-wave/istp/polar/modes.html

40) Polar PWI MCA Survey Spectrograms maxmize
Resource ID:spase://VWO/DisplayData/POLAR/PWI/MCA.DS.P1D
Start:1996-03-25 00:00:00 Observatory:POLAR Cadence:
Stop:1997-09-16 17:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:DisplayData
The Polar PWI Multichannel Analyzer (MCA) collected data from March 1996 to September 1997. The MCA data has very good time resolution (~1 s) but relatively poor frequency resolution. An electric field measurement covers 5.6 Hz to 311 kHz in 20 channels logarithmically spaced. The magnetic field measurements cover a range from 5.6 Hz to 10 kHz in 14 channels logarithmically spaced. Each file consists of two plots. Each plot contains the power spectral density (color scale) of received signal (upper plot: electric (V^2 m^-2 Hz^-1), lower plot: magnetic (nT^2 Hz^-1) ) as a function of operating frequency (in a logarithmic scale on vertical axis) and time (horizontal axis). At the top of each plot is a title indicating the Instrument, Receiver and Antenna used along with the time span for the spectrogram. Overlaid on each image is a trace of the electron gyrofrequency. Beneath the time labels on the horizontal axis of the lower plot are ephemeris data: position of the spacecraft in radial distance (Earth radii), geomagnetic latitude, magnetic local time, and McIlwain L-shell. Overlaid on each image is a trace of the electron gyrofrequency. Reference: Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.

41) Polar Plasma Wave Instrument, Multichannel Analyzer - 1.3 sec resolution fields maxmize
Resource ID:spase://VWO/NumericalData/POLAR/PWI/MCA.PT1.3S
Start:1996-03-25 00:00:00 Observatory:POLAR Cadence:1.3 seconds
Stop:1997-09-16 17:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
The PO_H0_PWI Multichannel Analyzer (MCA) CDF files provide good time resolution with relatively poor frequency resolution. An electric field measurement covers 5.6 Hz to 311 kHz in 20 channels logarithmically spaced. The magnetic field measurements cover a range from 5.6 Hz to 10 kHz in 14 channels logarithmically spaced. Reference: Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995. Note: The electron cyclotron frequencies are derived from the following: Fce = 0.028 kHz*B, where B is the magnitude of the ambient magnetic field measured in nT.

42) Polar Plasma Wave Instrument HFWR Data maxmize
Resource ID:spase://VSPO/NumericalData/POLAR/PWI/PT0.0000015S
Start:1996-02-27 12:20:27 Observatory:POLAR Cadence:0.0000015 seconds
Stop:1997-09-16 16:51:41 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
This set of plasma waves in the Earth's polar regions comes from the high-frequency waveform receiver (HFWR) of the Polar Plasma Wave Instrument (PWI) in 6 channels from 20 Hz to 25 kHz in 1.5 microsecond resolution. Data comes in snapshots of 31816 points per channel, every 9.2 seconds, where the duration of each snapshot is 0.045 seconds. Since Epoch time is in milliseconds, the times for the data points will not be unique unless the Delta_T in milliseconds is added to the Epoch time for the snapshot.

43) Polar Plasma Wave Instrument HFWR Wideband Receiver Data maxmize
Resource ID:spase://VSPO/NumericalData/POLAR/PWI/PT0.000016S
Start:1996-02-27 12:20:27 Observatory:POLAR Cadence:0.000016 seconds
Stop:1997-09-16 16:51:41 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
This set of electric plasma wave components in the Earth's polar regions comes the Wide Band Receiver of the Polar Plasma Wave Instrument (PWI) sampled at 16 microseconds resolution. The frequency filters used for the wideband receiver have a range that limit the calibration. The following table specifies the range of frequencies for which the calibration is certified. Outside this range the amplitude values may be in error and should not be used. (Translation, Filter, Freq Range) (0 kHz, 90 kHz, 7.5 kHz-90.0 kHz) (125 kHz, 90 kHz, 131.9 kHz-214.8 kHz) (250 kHz, 90 kHz, 254.3 kHz-341.2 kHz) (500 kHz, 90 kHz, 504.79 kHz-591.1 kHz) (0 kHz, 10 kHz, 0.035 kHz-11.64 kHz) (0 kHz, 22 kHz, 0.065 kHz-21.59 kHz) (0 kHz, 1-3 kHz, 1.0 kHz-3.0 kHz) (0 kHz, 3-6 kHz, 3.0 kHz-6.0 kHz).

44) PWI digital data at full resolution, 1996-7 maxmize
Resource ID:spase://VSPO/NumericalData/POLAR/PWI/PT600.00S
Start:1996-02-27 00:00:00 Observatory:POLAR Cadence:600.00 seconds
Stop:1967-09-16 00:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
PWI Sweep Frequency Receiver and Multi Channel Analyzer digital data at full resolution, accessible as ASCII tables

45) Polar PWI SFR-A Daily Dynamic Spectrograms maxmize
Resource ID:spase://VWO/DisplayData/POLAR/PWI/SFR.A.DS.P1D
Start:1996-03-25 00:00:00 Observatory:POLAR Cadence:
Stop:1997-09-16 17:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:DisplayData
The Polar Sweep Frequency Receiver-A (SFR-A) made use of either the Eu (130 m, spin-plane) or Ez (14 m, spin axis) two-sphere electric dipole antennas. Between March 25, 1996 and May 26, 1996, the Eu antenna was the default antenna, from May 27, 1996 through February 9, 1997 the Ez antenna was used and from February 10, 1997 until September 17, 1997 the SFR-A returned to using the Eu antenna. The SFR-A receiver spanned the frequency range from 26 Hz to 808 kHz in 5 bands: 26-200 Hz, 0.2 - 1.6 kHz, 1.7 - 12.6 kHz, 13-100 kHz, 100-808 kHz. Each image is a daily plot of the power spectral density (V^2 m^-2 Hz^-1) of received signal (color scale) as a function of operating frequency (in a logarithmic scale on vertical axis) and time (horizontal axis). At the top of each plot is a title indicating the Instrument, Receiver and Antenna used followed by the time span for the spectrogram. Beneath the time labels on the horizontal axis are ephemeris data: position of the spacecraft in radial distance (Earth radii), geomagnetic latitude, magnetic local time, and McIlwain L-shell. Overlaid on each image is a trace of the electron gyrofrequency.

46) Polar Plasma Wave Instrument, Sweep Frequency Receivers A and B - 2 sec resolution fields maxmize
Resource ID:spase://VWO/NumericalData/POLAR/PWI/SFR.AB.PT2S
Start:1996-03-25 00:00:00 Observatory:POLAR Cadence:2 seconds
Stop:1997-09-16 17:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
The PO_H1_PWI CDF files contain spectral densities of magnetic and electric field measurements from the Sweep Frequency Receiver-A and B. These files also contain correlation, electron cyclotron frequency, upper hybrid frequency and electron number density data. A full frequency sweep for the SFR takes about 33 seconds. From about 12.5 kHz to 800 kHz a full frequency spectrum can be obtained every 2.4 sec in the log mode. There are 224 SFR frequency bands, logarithmically spaced. When SFR_MODE is Linear, the 448 linear frequency bands are mapped to 224 logarithmic bands. The Polar Sweep Frequency Receiver-A (SFR-A) made use of either the Eu (130 m, spin-plane) or Ez (14 m, spin axis) two-sphere electric dipole antennas. Between March 25, 1996 and May 26, 1996, the Eu antenna was the default antenna, from May 27, 1996 through February 9, 1997 the Ez antenna was used and from February 10, 1997 until September 17, 1997 the SFR-A returned to using the Eu antenna. The SFR-A receiver spanned the frequency range from 26 Hz to 808 kHz in 5 bands: 26-200 Hz, 0.2 - 1.6 kHz, 1.7 - 12.6 kHz, 13-100 kHz, 100-808 kHz. The Polar PWI Sweep Frequency Receiver-B (SFR-B) collected data from March 1996 to September 1997. The SFR-B used the magnetic loop antenna (mounted on a 6m boom and oriented parallel to the Eu antenna). The SFR-B receiver spanned the frequency range from 26 Hz to 808 kHz in 5 bands: 26-200 Hz, 0.2 - 1.6 kHz, 1.7 - 12.6 kHz, 13-100 kHz, 100-808 kHz.

47) Polar PWI SFR-B Daily Dynamic Spectrograms maxmize
Resource ID:spase://VWO/DisplayData/POLAR/PWI/SFR.B.DS.P1D
Start:1996-03-25 00:00:00 Observatory:POLAR Cadence:
Stop:1997-09-16 17:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:DisplayData
The Polar PWI Sweep Frequency Receiver-B (SFR-B) collected data from March 1996 to September 1997. The SFR-B used the magnetic loop antenna (mounted on a 6m boom and oriented parallel to the Eu antenna). The SFR-B receiver spanned the frequency range from 26 Hz to 808 kHz in 5 bands: 26-200 Hz, 0.2 - 1.6 kHz, 1.7 - 12.6 kHz, 13-100 kHz, 100-808 kHz. Each image is a daily plot of the power spectral density (nT^2 Hz^-1) of received signal (color scale) as a function of operating frequency (in a logarithmic scale on vertical axis) and time (horizontal axis). At the top of each plot is a title indicating the Instrument, Receiver and Antenna used followed by the time span for the spectrogram. Beneath the time labels on the horizontal axis are ephemeris data: position of the spacecraft in radial distance (Earth radii), geomagnetic latitude, magnetic local time, and McIlwain L-shell. Overlaid on each image is a trace of the electron gyrofrequency.

48) Polar Plasma Wave Instrument, Wideband Receiver (WBR) 4.016 microsecond resolution maxmize
Resource ID:spase://VWO/NumericalData/POLAR/PWI/WBR.PT0.000004016S
Start:1996-03-25 10:00:00 Observatory:POLAR Cadence:0.000004016 seconds
Stop:1997-09-17 00:00:00 Instrument:Polar Plasma Waves Investigation (PWI) Resource:NumericalData
PWI>Plasma Wave Instrument Reference: Gurnett, D.A. et al, The Polar Plasma Wave Instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995. donald-gurnett@uiowa.edu An FFT on 1992 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series. Coordinate system used: antenna coordinate system, where the u-axis is offset by -45 degrees from the spacecraft x-axis, the v-axis is offset by -45 degrees from the spacecraft y-axis, and the z-axis is identical to the spacecraft z-axis. The effective noise bandwidth is the data sampling frequency divided by the size of the FFT (number of input samples) multiplied by 1.5 to to correct for the effects of a Hanning window applied to the time- domain samples. Hence, the effective noise bandwidth is 1.5 * delta_f. These data come in snapshots of 1992 or 3984 points every 0.064 seconds. Duration of a snapshot is less when the instrument is in duty cycle modes. Since Epoch time is in milliseconds, the times for the data points will not be unique unless the fmsec (fraction of milliseconds) is appended to the Epoch0 time for that point. The frequency filters used for the wideband receiver have a range that limits the calibration. The following table specifies the range of frequencies for which the calibration is certified. Outside this range the amplitude values may be in error and should not be used. +------------------------------------------------+ |Translation| Filter| | Freq Range| |------------------------------------------------| | 0 kHz| 90 kHz| | 7.5 kHz- 90.0 kHz| | 125 kHz| 90 kHz| | 131.9 kHz-214.8 kHz| | 250 kHz| 90 kHz| | 254.3 kHz-341.2 kHz| | 500 kHz| 90 kHz| | 504.79 kHz-591.1 kHz| | 0 kHz| 10 kHz| | 0.035 kHz- 11.64 kHz| | 0 kHz| 22 kHz| | 0.065 kHz- 21.59 kHz| | 0 kHz| 1-3 kHz| | 1.0 kHz- 3.0 kHz| | 0 kHz| 3-6 kHz| | 3.0 kHz- 6.0 kHz| +------------------------------------------------+ The cadence value given here is computed from the inverse of the sampling rate (249 kHz). For a description of the PWI receivers and the different operational modes see: http://www-pw.physics.uiowa.edu/plasma-wave/istp/polar/modes.html

49) Van Allen Probe A Fluxgate Magnetometer high resolution data in GEI coordinates maxmize
Resource ID:spase://VSPO/NumericalData/RBSP/A/EMFISIS/GEI/PT0.015625S
Start:2012-10-08 00:00:03 Observatory:Radiation Belt Storm Probe Satellite Cadence:0.015625 seconds
Stop:2016-09-14 07:59:50 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Fluxgate magnetometer data - Craig Kletzing (University of Iowa)

50) Van Allen Probe A Fluxgate Magnetometer 1 second resolution data in GEI coordinates maxmize
Resource ID:spase://VSPO/NumericalData/RBSP/A/EMFISIS/GEI/PT1S
Start:2012-10-08 00:00:03 Observatory:Radiation Belt Storm Probe Satellite Cadence:1 second
Stop:2016-09-14 07:59:50 Instrument:Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) Resource:NumericalData
Fluxgate magnetometer data - Craig Kletzing (University of Iowa)

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