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1) Alouette-2 Topside Sounder Ionogram Data maxmize
Resource ID:spase://VWO/NumericalData/Alouette2/SFS/PT31S
Start:1965-11-29 13:42:37 Observatory:Alouette 2 Cadence:31 seconds
Stop:1968-01-01 04:11:45 Instrument:Alouette 2 Sweep-Frequency Sounder Resource:NumericalData
These ionograms were digitized from the original Alouette 2 7-track analog telemetry tapes using the facilities of the former Data Evaluation Laboratory at the NASA/GSFC. This data restoration project is headed by Dr. R.F. Benson (NASA/GSFC). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.75 km. The ionograms consist of swept-frequency operation (there is no fixed-frequency operation as in ISIS-1 and ISIS-2). The time resolution between ionograms is typically 31 seconds.

2) CALLISTO Solar Spectrogram FITS files maxmize
Resource ID:spase://VWO/NumericalData/CALLISTO/FAS.PT0.25S
Start:2002-09-07 12:08:00 Observatory: Cadence:
Stop:2016-05-19 13:23:49 Instrument: Resource:NumericalData
This dataset contains solar dynamic spectrogram FITS files of the CALLISTO spectrometer data from the e-Callisto network of stations. The FITS file is composed of four parts: the ASCII-format header, the binary spectrum and two BIN tables. One table is for the time axis and the other for the frequency axis. FITSvfiles contain the keyword BUNIT in the primary header. If the BUNIT = 'SFU', then data are calibrated. If the BUNIT = 'digits', then data are raw data without any calibration. The naming convention for each file is of the form: STATION_YYYYMMDD_HHMMSS_CODE.fit.gz where STATION is a variable length station name and following the Date (YYYYMMDD) and UT time (HHMMSS) CODE is a two digit number that is an individual description of the front-end of the system. From the website http://e-callisto.org - The CALLISTO spectrometer is a programmable heterodyne receiver built in the framework of IHY2007 and ISWI by former Radio and Plasma Physics Group (PI Christian Monstein) at ETH Zurich, Switzerland. The main applications are observation of solar radio bursts and rfi-monitoring for astronomical science, education and outreach. The instrument natively operates between 45 and 870 MHz using a modern, commercially available broadband cable-TV tuner CD1316 having a frequency resolution of 62.5 KHz. The data obtained from CALLISTO are FIT-files with up to 400 frequencies per sweep. The data are transferred via a RS-232 cable to a computer and saved locally. Time resolution is 0.25 sec at 200 channels per spectrum (800 pixels per second). The integration time is 1 msec and the radiometric bandwidth is about 300 KHz. The overall dynamic range is larger than 50 dB. For convenient data handling several IDL- and Python-routines were written. Many CALLISTO instruments have already been deployed, including: 5 spectrometers in India (2 in Ooty, 1 in Gauribidanur, 1 in Pune, 1 in Ahmedabad), one in Badary near Irkutsk, Russian Federation, two in South Korea, three in Australia (Perth, Melbourne and Heathcote), two in Hawaii, two in Mexico, one in Costa Rica, two in Brazil, three in Mauritius, four in Ireland, one in Czech Republic, two in Mongolia, four in Germany, two in Alaska, two in Kazakhstan, one in Cairo, one in Nairobi, one in Sri Lanka, three in Trieste, one in Hurbanovo/Slovakia, two in Belgium, two in Finland, 8 in Switzerland, one in Sardinia, two in Spain, 5 in Malaysia, two in Indonesia, one in Scotland/UK one in Roztoky/Slovakia, one in Peru, one in Rwanda, one in Pakistan, one in Denmark, one in Japan and one in South Africa. Through the IHY/UNBSSI and ISWI instrument deployment program, CALLISTO is able to continuously observe the solar radio spectrum for 24h per day through all the year. All Callisto spectrometers together form the e-Callisto network. Callisto in addition is dedicated to do radio-monitoring within its frequency range with 13,200 channels per spectrum. The frequency range can be expanded to any range by switching-in a heterodyne up- or a down-converter. Instrument deployment including education and training of observers was financially supported by SNF, SSAA, NASA, Institute for Astronomy and North-South Center of ETH Zurich and a few private sponsors.

3) Callisto Quicklook Solar Spectrogram Plots maxmize
Resource ID:spase://VWO/DisplayData/Callisto/FAS.PT15M
Start:2002-09-07 12:08:00 Observatory: Cadence:
Stop:2016-05-19 13:23:47 Instrument: Resource:DisplayData
This dataset contains solar dynamic spectrogram PNG plots of the Callisto spectrometer data from the e-Callisto network of stations. Each plot spans 15 minutes. The naming convention for each file is of the form: STATION_YYYYMMDD_HHMMSS_CODE.fit.gz.png where STATION is a variable length station name and following the Date (YYYYMMDD) and UT time (HHMMSS) CODE is a two digit number that is an individual description of the front-end of the system. From the website http://e-callisto.org - The CALLISTO spectrometer is a programmable heterodyne receiver built in the framework of IHY2007 and ISWI by former Radio and Plasma Physics Group (PI Christian Monstein) at ETH Zurich, Switzerland. The main applications are observation of solar radio bursts and rfi-monitoring for astronomical science, education and outreach. The instrument natively operates between 45 and 870 MHz using a modern, commercially available broadband cable-TV tuner CD1316 having a frequency resolution of 62.5 KHz. The data obtained from CALLISTO are FIT-files with up to 400 frequencies per sweep. The data are transferred via a RS-232 cable to a computer and saved locally. Time resolution is 0.25 sec at 200 channels per spectrum (800 pixels per second). The integration time is 1 msec and the radiometric bandwidth is about 300 KHz. The overall dynamic range is larger than 50 dB. For convenient data handling several IDL- and Python-routines were written. Many CALLISTO instruments have already been deployed, including: 5 spectrometers in India (2 in Ooty, 1 in Gauribidanur, 1 in Pune, 1 in Ahmedabad), one in Badary near Irkutsk, Russian Federation, two in South Korea, three in Australia (Perth, Melbourne and Heathcote), two in Hawaii, two in Mexico, one in Costa Rica, two in Brazil, three in Mauritius, four in Ireland, one in Czech Republic, two in Mongolia, four in Germany, two in Alaska, two in Kazakhstan, one in Cairo, one in Nairobi, one in Sri Lanka, three in Trieste, one in Hurbanovo/Slovakia, two in Belgium, two in Finland, 8 in Switzerland, one in Sardinia, two in Spain, 5 in Malaysia, two in Indonesia, one in Scotland/UK one in Roztoky/Slovakia, one in Peru, one in Rwanda, one in Pakistan, one in Denmark, one in Japan and one in South Africa. Through the IHY/UNBSSI and ISWI instrument deployment program, CALLISTO is able to continuously observe the solar radio spectrum for 24h per day through all the year. All Callisto spectrometers together form the e-Callisto network. Callisto in addition is dedicated to do radio-monitoring within its frequency range with 13,200 channels per spectrum. The frequency range can be expanded to any range by switching-in a heterodyne up- or a down-converter. Instrument deployment including education and training of observers was financially supported by SNF, SSAA, NASA, Institute for Astronomy and North-South Center of ETH Zurich and a few private sponsors.

4) Cassini RPWS Key Parameter 60S maxmize
Resource ID:spase://VWO/NumericalData/Cassini/RPWS/KP_PT60S
Start:1997-10-25 00:00:00 Observatory:Cassini Cadence:60 seconds
Stop:2015-07-24 13:23:48 Instrument:Cassini RPWS Resource:NumericalData
The Cassini Radio and Plasma Wave Science (RPWS) calibrated summary key parameter data set includes reduced temporal and spectral resolution spectral information calibrated in units of spectral density for the entire Cassini mission. This data set includes calibrated values binned and averaged within 1 minute by 0.1 decade spectral channels for all times during the mission including the two Venus flybys, the Earth flyby, the Jupiter flyby, interplanetary cruise, and the entire Saturn tour. Data for this data set are acquired by the RPWS Low Frequency Receiver (LFR), Medium Frequency Receiver (MFR), and High Frequency Receiver (HFR). Data are presented in a set of fixed-record-length tables. This data set is intended to provide numerical summary data which can be used in conjunction with other Cassini fields and particles key parameter data sets to establish trends, select events, or simply as a browse data set for the Cassini RPWS archive. This data set should be among the first used by a user of any of the RPWS archive as it will lead one to information required to search for more detailed or highly specialized products.

5) Cassini RPWS Low Rate Full Resolution maxmize
Resource ID:spase://VWO/NumericalData/Cassini/RPWS/LRFULL_PT32S
Start:1997-10-25 00:00:00 Observatory:Cassini Cadence:32 seconds
Stop:2015-07-24 13:23:48 Instrument:Cassini RPWS Resource:NumericalData
The Cassini Radio and Plasma Wave Science (RPWS) Low Rate Full Resolution Calibrated (RPWS_LOW_RATE_FULL) is a data set including all spectral density measurements acquired by the RPWS in units of electric or magnetic field spectral density. This data set includes calibrated values for each frequency channel for each sensor for all times during the mission including the two Venus flybys, the Earth flyby, the Jupiter flyby, interplanetary cruise, and the entire Saturn tour. Data for this data set are acquired from the RPWS Low Frequency Receiver (LFR), Medium Frequency Receiver (MFR), Medium Frequency Digital Receiver (MFDR) (which can be used to replace MFR band 2 data) and High Frequency Receiver (HFR). Data are presented in a set of tables organized so as to have fixed-length records for ease in data handling. This data set is intended to be the most comprehensive and complete data set included in the Cassini RPWS archive. A browse data set is included with these data which provides for a graphical search of the data using a series of thumbnail and full-sized spectrograms which lead the user to the particular data file(s) of interest. This data set should be among the first used by a user of any of the RPWS archive as it will lead one to information required to search for more detailed or highly specialized products.

6) 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:2016-05-19 13:23:47 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.

7) 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:2016-05-19 13:23:46 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.

8) 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:2016-05-19 13:23:47 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.

9) 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:2016-05-19 13:23:47 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 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:2016-05-19 13:23:46 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.

11) Cluster WHISPER Combined Daily Dynamic Spectrograms maxmize
Resource ID:spase://VWO/DisplayData/Cluster/WHISPER/DS.JPG.P1D
Start:2001-01-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:
Stop:2013-12-31 23:59:59 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:DisplayData
These WHISPER daily dynamic spectrograms from each of the four Cluster spacecraft are plots of the received signal (the color scale indicates the voltage spectral density as Vrms Hz^-1/2) as a function of receiver frequency (on vertical axis) and time (horizontal axis). At the top of the image is the name of the instrument and date and above each plot the overflow status is indicated by a color code. Each spectrogram spans a frequency range from 2 through 80 kHz. Beneath the time labels on the horizontal axis are ephemeris data: position of the spacecraft in radial distance (Earth radii), latitude, and local time (GSE coordinates). The plots include data when the instruments are operating in both passive and active mode.

12) DE1 PWI Low Frequency Correlator Electric and Magnetic Field Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/DynamicsExplorer1/PWI/LFC.PT0.25S
Start:1981-09-16 05:21:48 Observatory:Dynamics Explorer 1 Cadence:0.25 seconds
Stop:1984-06-28 05:53:31 Instrument:Dynamics Explorer 1 Plasma Waves Instrument (PWI) Resource:NumericalData
Two Dynamics Explorer (DE) spacecraft were launched August 3, 1981, and placed into coplanar polar orbits with DE-1 in a highly elliptical orbit and DE-2 in a lower more circular orbit. The primary objective of the DE program was to investigate magnetosphere-ionosphere-atmosphere coupling processes. The DE mission provided a wealth of new information on a wide variety of magnetospheric plasma wave phenomena including auroral kilometric radiation, auroral hiss, Z mode radiation, narrow-band electromagnetic emissions associated with equatorial upper hybrid waves, whistler mode emissions, wave-particle interactions stimulated by ground VLF transmitters, equatorial ion cyclotron emissions, ion Bernstein mode emissions, and electric field turbulence along the auroral field lines. These files contain calibrated, full resolution, data from the DE-1 Plasma Wave Instrument (PWI). This instrument was designed and built by the plasma wave group at The University of Iowa, Department of Physics and Astronomy, in collaboration with investigators at Stanford University's STAR Laboratory. It measured plasma wave phenomena and quasi-static electric fields using paired combinations of five PWI sensors: a 200m tip-to-tip long wire electric antenna deployed in the spacecraft spin plane, a 9m tip-to-tip tubular electric antenna deployed along the spacecraft spin axis, a short 0.6m electric antenna, mounted on the boom and oriented parallel to the long wire antenna, a magnetic loop antenna mounted on the boom and oriented to measure the component of the magnetic field parallel to the long wire antenna, and a magnetic search coil antenna, also mounted on a boom and oriented to measure the magnetic field parallel to the spacecraft spin axis. The PWI main electronics unit consisted of a Step Frequency Correlator (SFC), a Low Frequency Correlator (LFC), a Wideband Analog Receiver (WBR) and a Linear Wave Receiver (LWR). Only the LFC data are included in these files. The SFC data were provided in a companion fileset. A dataset containing available high rate WBR LWR data may be provided in future archive products. The LFC consisted of two receivers (LFR-A and LFR-B) with 8 analog channels each. The analog channels were centered at 1.78, 3.12, 5.62, 10.0, 17.8, 31.2, 56.2 and 100 Hz. Each channel's band-edge was at +/-15% of the center value. Each LFR in the LFC could be connected to either the Ex, Es, Ez, or H antenna during an 8 second major frame. In addition, the Low Frequency Correlator provided in-phase and quadrature-phase correlations of signals from any selected antenna pair. Phase data are not provided in this file set.

13) DE1 PWI Step Frequency Correlator Electric and Magnetic Field Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/DynamicsExplorer1/PWI/SFC.PT0.25S
Start:1981-09-16 05:21:48 Observatory:Dynamics Explorer 1 Cadence:0.25 seconds
Stop:1984-06-28 20:35:55 Instrument:Dynamics Explorer 1 Plasma Waves Instrument (PWI) Resource:NumericalData
Two Dynamics Explorer (DE) spacecraft were launched August 3, 1981, and placed into coplanar polar orbits with DE-1 in a highly elliptical orbit and DE-2 in a lower more circular orbit. The primary objective of the DE program was to investigate magnetosphere-ionosphere-atmosphere coupling processes. The DE mission provided a wealth of new information on a wide variety of magnetospheric plasma wave phenomena including auroral kilometric radiation, auroral hiss, Z mode radiation, narrow-band electromagnetic emissions associated with equatorial upper hybrid waves, whistler mode emissions, wave-particle interactions stimulated by ground VLF transmitters, equatorial ion cyclotron emissions, ion Bernstein mode emissions, and electric field turbulence along the auroral field lines. These files contain calibrated, full resolution, data from the DE-1 Plasma Wave Instrument (PWI). This instrument was designed and built by the plasma wave group at The University of Iowa, Department of Physics and Astronomy, in collaboration with investigators at Stanford University's STAR Laboratory. It measured plasma wave phenomena and quasi-static electric fields using paired combinations of five PWI sensors: a 200m tip-to-tip long wire electric antenna deployed in the spacecraft spin plane, a 9m tip-to-tip tubular electric antenna deployed along the spacecraft spin axis, a short 0.6m electric antenna, mounted on the boom and oriented parallel to the long wire antenna, a magnetic loop antenna mounted on the boom and oriented to measure the component of the magnetic field parallel to the long wire antenna, and a magnetic search coil antenna, also mounted on a boom and oriented to measure the magnetic field parallel to the spacecraft spin axis. The PWI main electronics unit consisted of a Step Frequency Correlator (SFC), a Low Frequency Correlator (LFC), a Wideband Analog Receiver (WBR) and a Linear Wave Receiver (LWR). Only the SFC data are included in these files. The LFC data were provided in a companion fileset. A dataset containing available high rate WBR LWR data may be provided in the future. The SFC consisted of two Step Frequency Receivers (SFR-A and SFR-B) which provided amplitude measurements of the electric and magnetic fields from 100 Hz to 400 kHz and in-phase and quadrature-phase correlations of signals from any selected antenna pair. Phase data are not provided in these datasets.

14) 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.

15) Galileo PWS Earth Flyby Daily Dynamic Spectrograms Electric maxmize
Resource ID:spase://VWO/DisplayData/Galileo/PWS/DS.Electric.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 electric field spectrograms in units of electric field spectral density (V^2/m^2/Hz) spanning 6 Hz to 5.6 MHz. An associated dataset contains magnetic field spectrograms in units of magnetic field spectral density (nT^2/Hz) spanning 6 Hz to 75 kHz. 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 | +-----------------------------------------------------+

16) 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 | +-----------------------------------------------------+

17) 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.

18) 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.

19) Hawkeye Multi-Instrument Summary Plots maxmize
Resource ID:spase://VWO/DisplayData/Hawkeye/VLF/Multi.Instrument.PT51H
Start:1974-06-06 03:00:00 Observatory:Hawkeye Cadence:
Stop:1978-04-28 17:00:00 Instrument:Hawkeye VLF Resource:DisplayData
To help the user in searching through the Hawkeye data set, summary plots of the entire Hawkeye archive have been generated. Each summary plot consists of an entire orbit's worth of data from all of the instruments, along with the spacecraft position. Solar wind plasma pressure and IMF data have been added to the plots to help the user in data selection. HAWKEYE SUMMARY PLOT LAYOUT Title The orbit number is the orbit number at start of the plot time interval. Day 1 = January 1. First (top) panel Solar Wind pressure (red curve and red dots). Solar Wind IMF Bz component (in GSM) (blue dots). IMP-8 spacecraft Bz (in GSM) component (black curve). Second Panel The two numbers above the second panel are the positions of IMP-8 in degrees ( sign(y_gsm) * atan(sqrt(y_gsm^2+z_gsm^2)/x_gsm) ), at the start of and at the end of the plot time interval. Usually, if IMP-8 lies between -110 and +110 degrees it is in the solar wind. Solar Wind IMF magnetic field magnitude |B| (blue dots). IMP-8 magnetic Field magnitude |B| (black curve). Hawkeye magnetic Field magnitude |B| (red curve). Third Panel The two numbers above the third panel are: (left corner) The angle between the sun vector and spacecraft spin plane. Because the Hawkeye particle instrument's (LEPEDEA) field view is +/- 15 degrees out the the spin plane, this angle has to be less than 15 degrees in order to detect the solar wind when the spacecraft is located in the solar wind. (right corner)The spin period of the spacecraft in seconds. The electron energy-time spectrogram averaged over the solid angle sampled by LEPEDEA is plotted. Fourth Panel The ion energy-time spectrogram averaged over the solid angle sampled by LEPEDEA Fifth Panel The frequency-time spectrogram of the magnetic field as measured by the loop antenna The electron cyclotron frequency (white curve) as determined by the on-board magnetometer Sixth (bottom) Panel The electric field frequency-time spectrogram as measured by the dipole antenna The electron cyclotron frequency (white curve) as determined by the on-board magnetometer Time Axis Labels The universal time (hr:mm). The spacecraft position in Earth radii (RE) in units of RE. The spacecraft position in magnetic latitude (MLAT) in units of degrees. The spacecraft position in magnetic local time (MLT) in units of degrees. The spacecraft position in X-GSM in units of RE.

20) Hawkeye Electric and Magnetic Field Radio Frequency Spectrum Analyzer High Time Resolution maxmize
Resource ID:spase://VWO/NumericalData/Hawkeye/VLF/PT22S
Start:1974-06-08 06:45:10 Observatory:Hawkeye Cadence:22 seconds
Stop:1978-04-26 15:59:05 Instrument:Hawkeye VLF Resource:NumericalData
The CDF file contains approximately 22 second time resolution Electric and Magnetic field data, average magnetic field magnitude, and orbital position data from Hawkeye 1. The VLF experiment measured electric and magnetic fields using a 42.45-m electric dipole (tip-to-tip) which extended perpendicular to the spin axis and a search coil antenna deployed 1.58 m from the spacecraft. The electric field spectrum measurements were made in 16 logarithmically spaced frequency channels extending from 1.78 Hz to 178 kHz, and dc electric fields were also measured. The bandwidth of these channels varied from 7.5% to 30% depending on center frequency. Channel sensitivity and dynamic range were 1E-6 V/m and 100 dB, respectively. A wideband receiver was also used, with two selectable bandwidth ranges: 0.15 to 10 kHz or 1 to 45 kHz. The magnetic field spectrum was measured in eight discrete, logarithmically spaced channels from 1.78 Hz to 5.62 kHz. The bandwidth of these channels varied from 7.5% to 30% depending on frequency. The dynamic range was 100 dB, and the sensitivity ranged from 0.1 nT at 1.78 Hz to 3.4E-4 nT at 5.62 kHz. The wideband receiver described above could be used with the magnetic antenna. Each discrete channel was sampled once every 11.52 s.

21) IMAGE RPI Daily Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/IMAGE/RPI/DS.P1D
Start:2000-04-21 20:24:42 Observatory:IMAGE Cadence:5 minutes
Stop:2005-12-18 07:50:00 Instrument:Radio Plasma Imager (RPI) Resource:DisplayData
Collection of RPI Daily Dynamic Spectrogram plots at NASA GSFC, covering complete mission period from 2000-04-21 to 2005-12-18. Dynamic Spectrograms present the time history of natural radio emissions in space between 3 and 1009 kHz while the IMAGE spacecraft orbits the Earth. This operating frequency range was selected by the RPI team to provide an optimal temporal resolution to the wave observations. Each image is a daily plot of the voltage spectral density of received signal (color scale) as function of operating frequency (vertical axis) and time (horizontal axis). Commonly used in the analysis of noise generators, spectral density is a frequency-dependent characteristic that describes how much power is generated by the emission source in a 1 Hz bandwidth. RPI Dynamic Spectograms plot a Voltage Spectral Density, which is root of power spectral density, measured in [V/root-Hz] units. Note that conversion of antenna voltage to electric field strength depends on effective length of receive antennas, and such conversion is not performed here. RPI is capable of detecting input radio emissions above its noise floor of 5 nV/root-Hz, which is determined by the internal white noise of the RPI antenna pre-amplifiers.

22) RPI Dynamic Spectrogram data in CDF at NASA CDAWeb maxmize
Resource ID:spase://VWO/NumericalData/IMAGE/RPI/DS.PT5M
Start:2000-04-21 20:24:42 Observatory:IMAGE Cadence:5 minutes
Stop:2005-12-18 07:50:00 Instrument:Radio Plasma Imager (RPI) Resource:NumericalData
RPI passive wave measurement capturing voltage spectral density of the radio emissions in space as a function of frequency, typically between 3 and 1009 kHz. This operating frequency range was selected by the RPI team to provide optimal temporal resolution of the wave observations. Commonly used in the analysis of noise generators, spectral density is a frequency-dependent characteristic that describes how much power is generated by the emission source in a 1 Hz bandwidth. The original description of emissions was done in terms of thermal noise measurements, though the same approach also applies to non-thermal emissions such as AKR. CDF_DS_PT5M stores calibrated data from all three RPI antennas X, Y, and Z individually and a combined X+Y antenna channel. The data are presented as the Voltage Spectral Density (VSD), which is the root of power spectral density, measured in [V/root-Hz] units. Note that conversion of antenna voltage to electric field strength depends on the effective length of the receive antenna, and such conversion is not performed here. (See spase://SMWG/Instrument/IMAGE/RPI for a time history of the lengths of the three mutually orthogonal RPI dipole antennas.) RPI is capable of detecting input radio emissions above its noise floor of 5 nV/root-Hz, which is determined by the internal white noise of the RPI antenna pre-amplifiers. The VSD in RPI spectrogram data is presented in dB relative to 1 V/root-Hz (logarithmic scale), units of dB(V/root-Hz). The RPI instrument noise floor is 5 nV/root-Hz = -166 dB(V/root-Hz) at the receiver input. Software suggested by the science team for CDF file visualization: (1) Plotting tool at the CDAWeb portal, (2) For analysis beyond static image inspection, including color scale optimization, zooming, text export, alternative data representations in physical units, detailed frequency and time information, overlaid model fpe and fce graphs, and EPS quality figures, use BinBrowser software at UML, http://ulcar.uml.edu/rpi.html

23) RPI Plasmagram data in CDF at NASA CDAWeb maxmize
Resource ID:spase://VWO/NumericalData/IMAGE/RPI/PGM.CDF.PT5M
Start:2000-03-26 07:51:50 Observatory:IMAGE Cadence:5 minutes
Stop:2005-12-18 07:40:47 Instrument:Radio Plasma Imager (RPI) Resource:NumericalData
Software suggested by the science team for CDF file visualization: (1) Plotting tool at the CDAWeb portal, (2) For analysis beyond static image inspection, including color scale optimization, zooming, text export, alternative data representations in physical units, detailed frequency and time information, overlaid model fpe and fce graphs, and EPS quality figures, use BinBrowser software at UML, http://ulcar.uml.edu/rpi.html

24) ISEE1 PWI Spectrum Analyzer - Rapid Sample maxmize
Resource ID:spase://VWO/NumericalData/ISEE1/PWE/SA-rapid.PT0.125S
Start:1977-10-27 00:00:00 Observatory:ISEE 1 Cadence:0.125 seconds
Stop:1987-09-26 06:07:59 Instrument:ISEE-1 Plasma wave experiment Resource:NumericalData
'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978. The International Sun-Earth Explorer (ISEE) Program consisted of three satellites intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2 were launched on October 22, 1977 into highly elliptical geocentric orbits. The satellites passed through the magnetosphere and into the magnetosheath during each orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a 'halo orbit' about the the libration point situated about 240 earth radii (Re) upstream between the earth and the sun. Plasma passing this point arrives at the Earth about one hour later where it may cause changes that can be observed by ISEE 1 and ISEE-2. These two spacecraft, separated by a variable distance and with similar instrument complements, were intended to resolve the space-time ambiguity associated with measurements by a single spacecraft on thin boundaries which may be in motion such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S. contributions to the International Magnetospheric Study. ISEE-2 was built and managed by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo orbit' to explore the earth's deep tail region through much of 1983 on its way to an encounter with the comet Giacobini Zinner in September 1985. ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma, and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination of wave characteristics over a broad frequency range, including high-frequency resolution spectrum scans, simultaneous high-time resolution electric and magnetic frequency spectrum measurements, wave normal and Poynting flux measurements, and wide-band waveform measurements. PWI sampled the environment using three electric dipole antennas with lengths of 215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns of wire and a preamplifier for magnetic-field measurements. The experiment's main electronics consisted of four main elements: 1) a narrow-band sweep frequency receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These elements could be electrically connected to the six antennas in various combinations in flight. Data for this file originate with an electric antenna and were measured via the Electric Spectrum Analyzer (ESA). The PWI ESA was designed to provide high time resolution spectrum measurements for resolving wave emissions that are bursty or of a nonlinear nature. The ESA was a 20-channel analyzer covering the range from 5.62 Hz to 311 kHz. It had a relatively coarse frequency resolution, with four frequency channels per decade and bandwidths of +/-15 percent up to 10 kHz and +/-7.5 percent for 10 kHz and above. The ESA was nominally intended for electric field measurements, though 2.2 percent of all ESA measurements were made using the Z-axis magnetic search coil. The ISEE spacecraft collected two separate data products with the PWI ESA. 1) A full frequency range 20-channel spectra and 2) a single-channel, rapid-sample series. The 'E_series' variable in this file provides ESA rapid-sample measurements. Full frequency range 20-channel spectra are provided in a companion file set. The rapid-sample series data were collected at 8-times the data rate of the 20-channel spectra, thus there are 32 samples per second in high rate telemetry mode and 4 per second in low-rate mode. Regardless of the telemetry mode, every 16 seconds the rapid sample channel is incremented until reaching the highest frequency band of the ESA (311 kHz), where it rolls over to the 5th band (56.2 Hz). Only the upper 16 channels of the ESA were sampled in this manner. Altogether this provides a 16-channel frequency sweep every 4 minutes and 16 seconds. Unlike the SFR data, the time to preform a complete frequency sweep is not affected by the telemetry mode, though the number of samples in a sweep does increase by a factor of 4. Given the slowly changing nature of the frequency channel compared to the sampling time these data are stored as a time series, with the current frequency relegated to a status variable. Nonetheless, frequency-time spectrograms may be constructed from these measurements if desired. For a detailed description of the Plasma Wave Instrument, the reader is referred to the IEEE Geoscience Electronics reference above. A common acronym for the plasma waves instrument in older documentation is GUM, which stands for for Gurnett Mother. Since this acronym is not easily recognizable by the space physics community and since no official acronym is provided in the instrument paper, the more common short hand 'PWI' is used to refer to the Plasma Wave Instrument in this archive.

25) ISEE1 PWI Spectrum Analyzer maxmize
Resource ID:spase://VWO/NumericalData/ISEE1/PWE/SA.PT1S
Start:1977-10-22 19:13:20 Observatory:ISEE 1 Cadence:1 second
Stop:1987-09-26 06:07:59 Instrument:ISEE-1 Plasma wave experiment Resource:NumericalData
'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978. The International Sun-Earth Explorer (ISEE) Program consisted of three satellites intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2 were launched on October 22, 1977 into highly elliptical geocentric orbits. The satellites passed through the magnetosphere and into the magnetosheath during each orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a 'halo orbit' about the the libration point situated about 240 earth radii (Re) upstream between the earth and the sun. Plasma passing this point arrives at the Earth about one hour later where it may cause changes that can be observed by ISEE 1 and ISEE-2. These two spacecraft, separated by a variable distance and with similar instrument complements, were intended to resolve the space-time ambiguity associated with measurements by a single spacecraft on thin boundaries which may be in motion such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S. contributions to the International Magnetospheric Study. ISEE-2 was built and managed by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo orbit' to explore the earth's deep tail region through much of 1983 on its way to an encounter with the comet Giacobini Zinner in September 1985. ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma, and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination of wave characteristics over a broad frequency range, including high-frequency resolution spectrum scans, simultaneous high-time resolution electric and magnetic frequency spectrum measurements, wave normal and Poynting flux measurements, and wide-band waveform measurements. PWI sampled the environment using three electric dipole antennas with lengths of 215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns of wire and a preamplifier for magnetic-field measurements. The experiment's main electronics consisted of four main elements: 1) a narrow-band sweep frequency receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These elements could be electrically connected to the six antennas in various combinations in flight. Data for this file originate with the spectrum analyzers. The PWI Spectrum Analyzers were designed to provide high time resolution spectrum measurements for resolving wave emissions that are bursty or of a nonlinear nature. The pair consisted of a 20-channel analyzer covering the range from 5.62 Hz to 311 kHz, and a 14-channel analyzer covering the range from 5.62 Hz to 10 kHz. These analyzers have a relatively coarse frequency resolution, with four frequency channels per decade and bandwidths of +/-15 percent up to 10 kHz and +/-7.5 percent for 10 kHz and above. The center frequencies and bandwidths of the 20- and 14-channel analyzers are identical. The 20-channel analyzer was nominally intended for electric field measurements (which extend up to higher frequencies than the magnetic measurements), and the 14-channel analyzer was nominally intended for magnetic field measurements. All channels are sampled simultaneously so that electric-to-magnetic field ratios could be accurately determined. For a detailed description of the Plasma Wave Instrument, the reader is referred to the IEEE Geoscience Electronics reference above. A common acronym for the plasma waves instrument in older documentation is GUM, which stands for for Gurnett Mother. Since this acronym is not easily recognizable by the space physics community and since no official acronym is provided in the instrument paper, the more common short hand 'PWI' is used to refer to the Plasma Wave Instrument in this archive.

26) ISEE1 PWI Sweep Frequency Receiver maxmize
Resource ID:spase://VWO/NumericalData/ISEE1/PWE/SFR.PT32S
Start:1977-10-22 21:40:38 Observatory:ISEE 1 Cadence:32 seconds
Stop:1987-09-26 04:43:49 Instrument:ISEE-1 Plasma wave experiment Resource:NumericalData
'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978. The International Sun-Earth Explorer (ISEE) Program consisted of three satellites intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2 were launched on October 22, 1977 into highly elliptical geocentric orbits. The satellites passed through the magnetosphere and into the magnetosheath during each orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a 'halo orbit' about the the libration point situated about 240 earth radii (Re) upstream between the earth and the sun. Plasma passing this point arrives at the Earth about one hour later where it may cause changes that can be observed by ISEE 1 and ISEE-2. These two spacecraft, separated by a variable distance and with similar instrument complements, were intended to resolve the space-time ambiguity associated with measurements by a single spacecraft on thin boundaries which may be in motion such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S. contributions to the International Magnetospheric Study. ISEE-2 was built and managed by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo orbit' to explore the earth's deep tail region through much of 1983 on its way to an encounter with the comet Giacobini Zinner in September 1985. ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma, and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination of wave characteristics over a broad frequency range, including high-frequency resolution spectrum scans, simultaneous high-time resolution electric and magnetic frequency spectrum measurements, wave normal and Poynting flux measurements, and wide-band waveform measurements. PWI sampled the environment using three electric dipole antennas with lengths of 215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns of wire and a preamplifier for magnetic-field measurements. The experiment's main electronics consisted of four main elements: 1) a narrow-band sweep frequency receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These elements could be electrically connected to the six antennas in various combinations in flight. Data for this file originate with an electric antenna and were measured via the Sweep Frequency Receiver (SFR). The narrow-band sweep frequency receiver was intended to provide very high resolution spectrums with low time resolution for analyzing relatively steady narrow- band emissions such as upper hybrid resonance noise, electron plasma oscillations, and electron cyclotron harmonics. The receiver has 32 frequency steps in each of four bands covering the frequency range from approximately 100 Hz to 400 kHz. The frequency steps are logarithmically spaced with a frequency resolution of about 6.5 percent of the center frequency. The dynamic range of the receiver is 100 dB in the lowest three frequency bands, and 80 dB in the highest. Because the time resolution of the SFR is greater than the typical delay times for waves propagating between the two spacecraft, this receiver is only included on ISEE-1. For a detailed description of the Plasma Wave Instrument, the reader is referred to the IEEE Geoscience Electronics reference above. A common acronym for the plasma waves instrument in older documentation is GUM, which stands for for Gurnett Mother. Since this acronym is not easily recognizable by the space physics community and since no official acronym is provided in the instrument paper, the more common short hand 'PWI' is used to refer to the Plasma Wave Instrument in this archive.

27) ISEE-3 Radio Mapping Experiment Demodulated - 1.5 sec resolution maxmize
Resource ID:spase://VWO/NumericalData/ISEE3/RadioMapping/DEMOD.PT1.5S
Start:1978-08-13 08:31:28 Observatory:ISEE 3 Cadence:1.5 seconds
Stop:1987-01-23 11:13:38 Instrument:ISEE 3 Radio Mapping Experiment Resource:NumericalData
The following is extracted from "User Guide for ISEE-3 Radio Mapping Experiment CD-ROM Data" the original document is available via the Information URL below. The ISEE-3 Radio Mapping Experiment is designed to detect and measure radio bursts from the Sun, the interplanetary medium, and the Earth's magnetosphere, at frequencies from 30 kHz to 2 MHz. It is a collaboration of the Observatory of Paris-Meudon and the Goddard Space Flight Center; the Principal Investigator is Jean-Louis Steinberg. The experiment determines the direction of sources and estimates their apparent angular sizes using two dipole antennas. One dipole, the shorter of the two, is along the spin axis of the satellite, while the second dipole is perpendicular to the spin axis and is therefore carried around by the rotation of the satellite. Each of the monopoles making up the spin-axis dipole can be extended to 7m, whereas each monopole making up the dipole in the spin plane is 45m long. The signal received by the spinning dipole is modulated, being strongest when the dipole is perpendicular to the direction of the source. The phase of the spin modulation provides information on the direction of the source, projected onto the plane in which the dipole is spinning, and the amplitude of the modulation determines the angular size of the source as a function of its elevation above or below the spin plane. The additional information provided by the spin-axis dipole helps determine whether the source is above or below the spin plane, and its elevation. Detailed Description of the Data Acquisition The experiment is designed to make a series of measurements at each frequency (listed in Table 2-1), covering one-half spin. Such a series is called a step. The specifics of the data are described below. In this document, the spin-axis dipole is called the Z-dipole, because the spin axis is labeled the z-axis of the satellite-based coordinate system. The other dipole is called the S-dipole, because it is spinning. ISEE-3 has two spinning dipoles, called U and V. Only the V dipole was used to acquire radio data. Table 2-1. ISEE-3 Radio Mapping Experiment Frequencies +------------------------------------+ | Channel | Receiver Freq. (Khz) | | No. | Broad | Narrow | |===========|=========|==============| | 1 |1980 | 1000 | | 2 |1000 | 466 | | 3 | 513 | 290 | | 4 | 360 | 188 | | 5 | 233 | 145 | | 6 | 160 | 110 | | 7 | 123 | 80 | | 8 | 94 | 66 | | 9 | 72 | 56 | | 10 | 60 | 47 | | 11 | 50 | 36 | | 12 | 41 | 30 | +------------------------------------+ Demodulating the data The direction to the source and the source strength are determined from the spin-modulated S samples and the Z sample by the procedure described in the following section. The linear least-squares solution provides a despun source amplitude A, which is its maximum amplitude, observed when the S dipole is "broadside" to the source, the azimuth angle with respect to the Sun of the source center in the spin plane, and a measure of the modulation of the source due to the changing orientation of the S dipole, called alpha. The standard deviation of the least-squares fit and the uncertainties in the three parameters are also calculated. Comparison of the Z sample and A with the modulation index alpha permits to evaluate the source radius and its elevation from the spin plane. Data file contents There are 3 different sets of data files that are of potential interest to new users - 1.5 sec modulated data, 108 second averages, and 1.5 sec demodulated data. The 1.5 sec modulated data files contain individual data samples, calibrated in units of antenna temperature. The spin modulation has not been removed from these files. The 108 sec average files are simple averages of the 1.5 sec modulated data as a function of frequency. (Note that the average is done in log space, I.e., mean(log(antenna temperature)).) Finally, the 1.5 sec demodulated data file contains the parameters A, alpha, and azimuth. The demodulated data file is the file that most users will want to use. Contents of the ISEE-3 Radio 1.5 sec DEMOD Record +--------------------------------------------------------------------+ | VARIABLE | DIM| # | DESCRIPTION | |==========|====|=======|============================================| |MDATE | | |Julian date of record (YYDDD) | |MHMS | | |Time of midpoint of record in hhmmss | |MSEC | | |Time of midpoint or record in msecs | |NFREQ | | |Frequency channel 1-12 | |ADSP |4 |1 |Despun SB amplitude (or SN for Mode3) | | |2 | |Despun SN amplitude if mode 1 | | |3 | |Log of SB as log TA | | |4 | |Log SN if mode 1, else 0 | |ALPHA |2 |1 |Modulation Index for B(or N if mode3) | | | |2 |Modulation Index for N if mode 1, else 0 | |PHI |2 | |Source longitude(increasing to west of sun) | | | | |for B, N in degrees (-90 - 90) | |Z |4 | |Average Z amplitude - elements as for ADSP | |PHASE |2 | |Phase(volts) for the first input record used| | | | |in group for B, N(or both B for mode 2, both| | | | |N for mode 3) | |PHANG |2 | |Phase sun angle for B,N in radians | |ELEV |2 | |Calculated elevation angle for B,N | |RAD |2 | |Calculated source radius for B,N in degrees | |BW |4 |1 |Background value used for SB in calculating | | | | |ELEV and RAD | | | |2 |Background value used for SN (mode 1) | | | |3 |Background value used for ZB | | | |4 |Background value for ZN if mode 1 | |ST |2 | |Fractional standard deviations of least | | | | |squares fit for B,N | |SIGA |3x2 | |Uncertainties in parameters for least | | | | |squares fit | | | |1x |Uncertainty in mean SB, SN amplitude | | | |2x |Uncertainty in alpha for B,N | | | |3x |Uncertainty in PHI for B, N in degrees | |NSAMP | | |Number of S samples in fit | |IQUAL |2 | |Quality of analysis B, N | |KDATE | | |Julian date of processing | |MODE | | |Data mode | |SPINP | | |Spin period in msec | |GSE |3 | |XYZ coordinates Geocentric solar ecliptic | | | | |in meters | |SPARE |10 | |Spares | +--------------------------------------------------------------------+

28) ISIS-1 Topside Sounder Ionograms maxmize
Resource ID:spase://VWO/NumericalData/ISIS1/SFS/Ionogram.PT29S
Start:1969-01-30 14:50:12 Observatory:ISIS 1 Cadence:24 seconds
Stop:1983-12-30 15:19:33 Instrument:ISIS1 Swept-Frequency Sounder Resource:NumericalData
These ionograms were digitized from the original ISIS-1 7-track analog telemetry tapes using the facilities of the former Data Evaluation Laboratory at the NASA/GSFC. This data restoration project is headed by Dr. R.F. Benson (NASA/GSFC). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.75 km. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution between ionograms is typically 29 seconds.

29) ISIS-2 Topside Sounder Ionograms maxmize
Resource ID:spase://VWO/NumericalData/ISIS2/SFS/Ionogram.PT22S
Start:1969-01-30 14:50:12 Observatory:ISIS 2 Cadence:22 seconds
Stop:1983-12-30 15:19:33 Instrument:ISIS2 Swept-Frequency Sounder Resource:NumericalData
These ionograms were digitized from the original ISIS-2 7-track analog telemetry tapes using the facilities of the former Data Evaluation Laboratory at the NASA/GSFC. This data restoration project is headed by Dr. R.F. Benson (NASA/GSFC). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.75 km. Ionograms with this sample rate are designated as "full" ionograms because they have the full 3.75 km apparent-range resolution. The ionograms used for most analysis, and those available from CDAWeb, were produced by averaging every four samples of the sounder-receiver video amplitude output to yield an average value every 100 microseconds corresponding to an apparent-range resolution of 15 km. These ionogram files are referred to as "average" files with standard resolution. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution between ionograms is typically 14 or 22 seconds depending on the frequency sweep range.

30) 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.

31) 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.

32) 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.

33) 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.

34) 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.

35) 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.

36) STEREO WAVES (SWAVES) PDF Dynamic Spectrogram Plots both Ahead and Behind s/c maxmize
Resource ID:spase://VWO/DisplayData/STEREO/SWAVES/DS.Color.PDF.P1D
Start:2006-10-27 20:24:42 Observatory:STEREO A Cadence:1 minute
Stop:2016-05-19 13:23:47 Instrument:STEREO-A Waves (SWAVES) Resource:DisplayData
This dataset contains 24 hour duration dynamic spectrogram plots from the combined STEREO A and B Waves instrument. The plots are provided in several file formats (PNG, Postscript and PDF) and there are renditions in color and grayscale with and without additional lines of time series data indicating the instrument operating status. These plots all reside within the same directory structure subdivided by year. The "new" subdirectory contain plots at a higher resolution but currently are not available for dates early in the mission. These data consist of output from the SWAVES HFR and LFR receivers. ? the High Frequency Receivers (HFR) - for spectral analysis and direction finding of radio noise generated from a few solar radii (16 MHz) to about half an Astronomical Unit (125 kHz) ? the Low Frequency Receiver (LFR) - for spectral analysis and direction finding from about half an Astronomical Unit (160 kHz) to one AU (2.5 kHz).

37) STEREO WAVES (SWAVES) Radio Intensity Spectra, both Ahead and Behind s/c maxmize
Resource ID:spase://VWO/NumericalData/STEREO/SWAVES/DS.Combined.PT1M
Start:2006-10-27 20:24:42 Observatory:STEREO A Cadence:1 minute
Stop:2016-05-19 13:23:49 Instrument:STEREO-A Waves (SWAVES) Resource:NumericalData
The CDF file contains 1 minute averaged radio intensity data from both the Ahead and Behind s/c. A description of the STEREO/WAVES instrument is provided in: Bougeret, J.L, et al. (2008), S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission, Space Science Reviews, 136, 487-528. The STEREO / WAVES (SWAVES) instruments provide unique and critical observations for all primary science objectives of the STEREO mission, the generation of CMEs, their evolution, and their interaction with Earth's magnetosphere. SWAVES can probe a CME from lift-off to Earth by detecting the coronal and interplanetary (IP) shock of the most powerful CMEs, providing a radial profile through spectral imaging, determining the radial velocity from ~2 RS (from center of sun) to Earth, measuring the density of the volume of the heliosphere between the sun and Earth, and measuring important in situ properties of the IP shock, magnetic cloud, and density compression in the fast solar wind stream that follows. SWAVES measures the fluctuation electric field present on three orthogonal monopole antennas mounted on the back (anti-sunward) surface of the spacecraft. Each monopole antenna unit is a 6 m long Beryllium-Copper (BeCu) ?stacer? spring. The three units deploy from a common baseplate that also accommodates the preamplifier housing. The 6 m length was chosen to put the antenna quarter-wave resonance near the top of the SWAVES HFR2 frequency band. These data consist of output from the SWAVES HFR and LFR receivers. ? the High Frequency Receivers (HFR) - for spectral analysis and direction finding of radio noise generated from a few solar radii (16 MHz) to about half an Astronomical Unit (125 kHz) ? the Low Frequency Receiver (LFR) - for spectral analysis and direction finding from about half an Astronomical Unit (160 kHz) to one AU (2.5 kHz).

38) Ulysses URAP Daily Color Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/Ulysses/URAP/DS.P1D
Start:1990-11-03 19:30:00 Observatory:Ulysses Cadence:128 seconds
Stop:2007-11-26 18:30:00 Instrument:Unified Radio and Plasma Waves (STO/URAP) Resource:DisplayData
from URAP Users Notes: Guide To The Archiving Of Ulysses Radio And Plasma Wave Data by Roger Hess, Robert MacDowall, Denise Lengyel-Frey March 15, 1995 - version 1.0 revised March 24, 1999 - version 1.1 revised June 8, 1999 - version 1.2 These color plots present URAP radio and plasma wave data in a format referred to as dynamic spectra. For the daily plots, the time resolution is 128 seconds, providing high-time resolution across the entire frequency range of the URAP receivers. The 10-day plots use 10-minute resolution data, which permits good detection of bursty wave activity. The 26-day plots use 1-hour resolution data; these plots correspond to the other Ulysses 26-day plot intervals, but the ability to identify wave activity is reduced. The power of the electric or magnetic field is shown in color as a 2-dimensional function of time and frequency. The plots include data from the URAP Radio Astronomy Receivers (RAR), Plasma Frequency Receiver (PFR), and Waveform Analyzer (WFA). Refer to the documentation for the 10-minute average archive data files, as well as Stone et al. (1992), for more general information on these instruments. Here, we describe the choices that were made in generating these plots. 1. Formats - These plots are available in 2 formats: GIF files for viewing with a web browser and Postscript files for high quality printed copies. The resolution of the GIF files is 776 x 600 pixels, a compromise between smaller size for network transfer and larger size for improved resolution. The Postscript files are sized to fit both 8.5x11 inch paper or A4 paper. The daily unzipped (zipped) Postscript files are typically 400-440 kB ( 130-140 KB) in size; the daily GIF files are typically 200-230 kB in size. (The 10-day and 26-day plots are similar in size.) 2. Data units - The data and the associated color bar are plotted in units of decibels, an old radio astronomer unit for describing signal to background ratio on a logarithmic scale. Specifically, Data_in_dB = 10. * log10(total power/background power) The data for electric field observations are in units of microvolts**2 Hz**(-1) as are the calculated background levels. The units for magnetic field observations (the bottom panels on the page) are nT**2 Hz**(-1). The data for the 1-day plots are comparable to the squared values of data in the URAP UFA 10-minute files. Although the ratio (total power-background power)/background power permits one to see weaker events in such plots, it is more sensitive to background determination and enhances the noise seen in the plots. Therefore, it is not used here. 3. Backgrounds - The background levels as a function of frequency for the RAR and WFA are determined from the data for the day, because they vary throughout the mission. The PFR background does not vary significantly with time, so fixed background levels are used. For each of the instruments, the backgrounds vary with the instrument mode, so separate sets of backgrounds are derived for each mode that is present. (Modes are discussed below). The PFR and WFA backgrounds also depend significantly on bit rate. For the RAR the background level selected is the lowest 3% of the data for each frequency; for the PFR and WFA, the background level selected is the lowest 10% of the data for each frequency. The higher number is chosen for the WFA because the data are substantially noisier than the RAR. It should be noted that this type of background subtraction will remove any signal at a given frequency that is constant throughout the day. An example is the quasithermal noise line ("plasma line") in the RAR data, when the density does not vary throughout the day. Note that for 10-day and 26-day plots, in particular, the background determination might result from a few hours of very low intensity data, which will cause all the other data, referenced to that background, to appear enhanced. This is an unfortunate consequence of determining the background levels from intervals of minimum data intensity. 4. Modes and other labels - Each of the instruments has several modes that affect the data display. The telemetry bit rate is also an important parameter. The key modes and the bit rate are shown on the dynamic spectrum as the thickness (or nonexistence) of a line. The RAR Hi and Lo bands are plotted in separate panels because they are commanded separately. For each band, the spin-plane and spin-axis antennas can be either summed or separate. If the RAR Hi or Lo band instrument is in summed mode, then a white line for the appropriate band is present under the RAR plot. Summed mode provides data used for 3-dimensional direction finding at the expense of a higher background level. Because the backgrounds will differ between summed and separate modes, backgrounds are calculated for both modes when they are present. Although the RAR is typically operated in a mode where measurements are made at all 76 frequencies, there are times when only a subset of the frequencies are sampled (called Measure mode). In these cases, the data plotted are interpolated in frequency to give a clearer picture of the events that might be taking place. These intervals are evident from the appearance of the data, which is smoothed in frequency; see Nov. 6, 1990, where the RAR Lo band is in Measure mode for the first 18 hours of the day. This example also shows the RAR hi band in a rarely-used, single frequency mode. If the Measure mode data occupy less than 10% of the day; they are not interpolated, because the events occurring at these times should be clear from the non-Measure mode data, and it is useful to see which frequencies are being sampled. The Jupiter flyby interval (e.g., Feb. 8, 1992) includes examples of short intervals of measure mode. The bit rate significantly affects the PFR and WFA backgrounds. If the science data bit rate is 1024 bps, it is indicated by a thick line, 512 bps is indicated by a thin line, and low ("emergency") bit rates, either 256 or 126 bps, by no line. The PFR operates in one of 3 modes - fast scan, slow scan, or fixed tune (see Stone et al., 1992). These 3 modes have different backgrounds and generate different interferences for the WFA instrument. Fast scan is shown by the white line under the PFR plot, slow scan is in progress if there is no line, and fixed tune is a single frequency mode (evident from the PFR data display), typically used in 1 hour/day intervals. The WFA instruments can sample either the electrical (E) antennas or the (B-field) search coil. For the low band of the WFA B field data (< 8 Hz), either By or Bz data are telemetered. The available parameter is shown by the white line above the B (WFA) plot (present=By, absent=Bz). 5. Interpolation - In addition to the interpolation discussed above for the RAR, the RAR data are interpolated to remove data gaps of 384 seconds or less. We interpolate the RAR data because the events observed in the RAR, such as solar type II and type III radio bursts, are mostly smoothly varying on time scales of a few minutes. Therefore, they are easier to visualize and interpret when data gaps are interpolated. For the events in the PFR and WFA data, predominantly bursty wave events, interpolation is not necessary and not performed. An exception occurs when the data telemetry rate is either 256 or 128 bps; then the WFA data are interpolated in time because they are not sampled every 128 sec. Finally, the RAR Hi band data, for which there are only 12 channels of data, are interpolated to fit a logarithmic frequency scale with 37 equivalent frequencies. 6. Interference and other issues affecting data interpretation - Each of these instruments, like all sensitive wave receivers, is affected by interference from other sources. For the RAR Hi band, an interference signal at 81 kHz is produced by the Ulysses GAS instrument. Depending on the mode in which the GAS instrument is operating, this interference can occur from 0 to 24 hours per day. If an algorithm determines that this interference is present in more than about 10% the RAR data for the day, we remove the 80 kHz data and interpolate from adjacent frequencies. The RAR Hi band also has an enhanced background at 120 kHz (source unknown). Subtraction of this enhanced background can cause artifacts in other events, like type III bursts. See Nov. 30, 1990 as an example. The RAR Lo band has an interference line at 8.75 kHz and odd harmonics caused by the Ulysses traveling wave tube amplifier (TWTA), which is part of the high gain telemetry system. In general, this signal is removed by the background subtraction, sometimes producing artifacts in weak radio events or the thermal noise spectrum at these frequencies The PFR experiences interference from the URAP Sounder; these data are removed from the plots and appear as short data gaps. The background levels of the PFR depend on bit rate, PFR mode, and the cadence of the URAP Fast Envelope Sampler (FES data not presented in these plots); these background variations can affect the appearance of events at the transition from one mode to another. The WFA data are affected by numerous interferences, of which the URAP PFR is the dominant source. WFA "backgrounds" vary significantly depending on whether the PFR is in fast or slow scan mode or fixed tune, so separate backgrounds are calculated for each of these. The URAP Sounder also causes interference; these data are removed from the plots and appear as short data gaps. Spacecraft thruster operations produce a variety of artifacts in the data; since we have no indication of these in our telemetry, they are not flagged on the plots. Examples may be seen on Feb 23, 1995 at 12:00 and on Feb. 25, 1995 at 15:00. An interesting "interference" is seen to disappear on Dec. 17, 1990; this is when the spacecraft nutation was stopped. This is best seen on the 26- day plots. To summarize, there are a variety of artifacts in the wave data that affect interpretation. These can result from corrupted telemetry values (producing bad pixels (most evident in the RAR plots, see March 23, 1993, from 6:00-14:00, or August 16, 1991, a very good example of very bad data quality), interferences (e.g., non-physical, block-like structures sometimes seen in the highest frequencies of the WFA E and B data (see March 14, 1995)), or changes of the instrument mode or the physical medium (e.g., a short interval of data with a very low signal level defines a background for the rest of the day that is not appropriate; see Nov. 4, 1990, when the Ex antenna was deployed). 7. Spacecraft location - At the lower left on the plots, 4 parameters related to the location of Ulysses at the mid-time of the plot are printed: a) the Ulysses-Sun (U-S) distance in AU, b) the heliographic latitude (Hlat_U) of Ulysses in degrees, c) the Ulysses-Sun-Earth (U-S-E) angle in degrees, and d) the Ulysses-Jupiter (U-J) distance in AU. These are among the most relevant parameters for interpreting the URAP data. Additional parameters, as well as a graphic showing the Ulysses location relative to the Sun, Earth, and Jupiter, can be found at the URAP Home Page at Goddard Space Flight Center (see below). 8. For additional information on these plots or on the URAP data, contact the PI of the URAP investigation, Dr. Robert MacDowall, at phone: 1-301-286-2608 fax: 1-301-286-1683 email: robert.macdowall@gsfc.nasa.gov. The URL for the URAP Home Page at Goddard Space Flight Center is http://urap.gsfc.nasa.gov/

39) Spectrograms of Voyager 1 PRA Highband Receiver Jupiter encounter, 48 sec resolution maxmize
Resource ID:spase://VWO/DisplayData/Voyager1/PRA/Jupiter/High.P1D
Start:1979-02-01 00:00:00 Observatory:Voyager 1 Cadence:48 seconds
Stop:1979-04-13 23:59:59 Instrument:Voyager 1 Planetary Radio Astronomy (PRA) experiment Resource:DisplayData
Spectrogram plots in GIF format derived from Voyager 1 Planetary Radio Astronomy (PRA) Highband receiver daily files during Jupiter Encounter (1979-02-01 to 1979-04-13). These plots are available for both polarization channels and in both color and grayscale. The color scale of these plots represent the electric field power spectral density in units of millibels. Across the top of each spectrogram in the spacecraft and instrument name, the name of the binary data file that was used to create this plot, the polarization channel (Left or Right) and the date in the format YYMMDD. The data set provides 48 second resolution highband radio mean power data in units of millibels. The high-band receiver consisted of 128 channels of 200 kHz bandwidth each, with center frequencies spaced at 307.2 kHz intervals from 1.2 MHz to 40.4 MHz. The highband receiver was designed especially for the observation of Jovian decametric radio emissions. The PRA radiometer was usually operated routinely in the so-called POLLO sweeping mode, in which all 198 frequency channels of the high- and low-band receivers together were swept in 6 sec, dwelling at each channel for 25 msec. From one step to the next in the channel switching sequence, the antenna polarization sense was reversed, i.e., was changed from RH to LH or vice versa. Thus the time required for making a measurement of both the RH and LH intensity components at both senses of elliptical polarization at a given frequency was 12 sec. The data consists of successive averages of 4 pairs of RH and LH intensity measurements, each average spanning an interval of 48 sec. The data are calibrated and are given in units of 'millibels' which is 1000 times the log of the received power. Zero millbels corresponds to approximately 1.4 x 10^-21 W m^-2 Hz^-1, however, this value is never seen in practice. The minimum values detected, which includes receiver internal and spacecraft generated noise, are about 2300 to 2400 millibels, or about 3.5 x 10^-19 W m^-2 Hz^-1; even higher values are seen at the very lowest frequencies. Note: The polarization indicated is the received polarization, not necessarily the emitted polarization. Correct interpretation of the received polarization depends on the antenna plane orientation relative to the radio source. A good description of this concept can be found in Leblanc Y., Aubier M. G., Ortega-Molina A., Lecacheux A., 1987, J.Geophys. Res. 92, 15125 and in Wang, L. and Carr, T.D., Recalibration of the Voyager PRA antenna for polarization sense measurement, Astron. Astrophys., 281, 945-954, 1994. and references therein.

40) Voyager 1 PRA Highband Receiver Jupiter encounter, 48 sec resolution maxmize
Resource ID:spase://VWO/NumericalData/Voyager1/PRA/Jupiter/High.PT48S
Start:1979-02-01 00:00:00 Observatory:Voyager 1 Cadence:48 seconds
Stop:1979-04-13 23:59:59 Instrument:Voyager 1 Planetary Radio Astronomy (PRA) experiment Resource:NumericalData
Voyager 1 Planetary Radio Astronomy (PRA) Highband receiver daily files during Jupiter Encounter (1979-02-01 to 1979-04-13). Associated with these binary data are a series of quick-look GIF spectrogram plots created using the binary data. The plots are available for both polarization channels. These binary data were also converted into IDL save sets. The data set provides 48 second resolution highband radio mean power data in units of millibels. The high-band receiver consisted of 128 channels of 200 kHz bandwidth each, with center frequencies spaced at 307.2 kHz intervals from 1.2 MHz to 40.4 MHz. The highband receiver was designed especially for the observation of Jovian decametric radio emissions. The PRA radiometer was usually operated routinely in the so-called POLLO sweeping mode, in which all 198 frequency channels of the high- and low-band receivers together were swept in 6 sec, dwelling at each channel for 25 msec. From one step to the next in the channel switching sequence, the antenna polarization sense was reversed, i.e., was changed from RH to LH or vice versa. Thus the time required for making a measurement of both the RH and LH intensity components at both senses of elliptical polarization at a given frequency was 12 sec. The data consists of successive averages of 4 pairs of RH and LH intensity measurements, each average spanning an interval of 48 sec. The format of these binary data files is as follows: file separation variable year, month, day information millisecond decimal value of the day Integer array (128,2) for 128 left and right channels (NOTE 128 channels for Hi-band; 70 channels for Lo-band) file separation variable There is an IDL program that reads these files into an IDL-format save set. See Information URL for a link to this file. The data are calibrated and are given in units of 'millibels' which is 1000 times the log of the received power. Zero millbels corresponds to approximately 1.4 x 10^-21 W m^-2 Hz^-1, however, this value is never seen in practice. The minimum values detected, which includes receiver internal and spacecraft generated noise, are about 2300 to 2400 millibels, or about 3.5 x 10^-19 W m^-2 Hz^-1; even higher values are seen at the very lowest frequencies. Note: The polarization indicated is the received polarization, not necessarily the emitted polarization. Correct interpretation of the received polarization depends on the antenna plane orientation relative to the radio source. A good description of this concept can be found in Leblanc Y., Aubier M. G., Ortega-Molina A., Lecacheux A., 1987, J.Geophys. Res. 92, 15125 and in Wang, L. and Carr, T.D., Recalibration of the Voyager PRA antenna for polarization sense measurement, Astron. Astrophys., 281, 945-954, 1994. and references therein.

41) Voyager 1 PRA Lowband Receiver Jupiter encounter, 6 sec resolution maxmize
Resource ID:spase://VWO/NumericalData/Voyager1/PRA/Jupiter/Low.PT6S
Start:1979-01-06 00:00:34 Observatory:Voyager 1 Cadence:6 seconds
Stop:1979-04-13 23:59:08 Instrument:Voyager 1 Planetary Radio Astronomy (PRA) experiment Resource:NumericalData
(Description based on material from VG1_PRA_JUP_HRES_DS.CAT) Voyager 1 Radio Astronomy (PRA) data from the Jupiter encounter (1979-01-06 to 1979-04-13). The data set provides 6 second high resolution lowband radio mean power data. The data are provided for 70 instrument channels, covering 1.2 to 1326.0 kHz. This data set (VG1-J-PRA-3-RDR-LOWBAND-6SEC-V1.0) contains data acquired by the Voyager-1 Planetary Radio Astronomy (PRA) instrument during the Jupiter encounter. The bounding time interval set for most Voyager 1 Jupiter PDS data sets is the Voyager project defined 'far encounter' mission phase boundary (1979-02-28 to 1979-03-22). Since, however, the PRA instrument is able to observe planetary phenomenon at much larger ranges than other fields and particles experiments, this boundary is artificial with respect to PRA. Hence, PRA lowband data provided here cover the entire Jupiter Encounter Phase (1979-01-06 to 1979-04-13). Data from beyond the far encounter interval is contained in the cruise data archive which is available from the NSSDC. VG1-J-PRA-3-RDR-LOWBAND-6SEC-V1.0 contains data at the highest time resolution possible during normal operations. The normal mode of PRA operations during the planetary encounters was to sweep through the two radio receiver bands, high band (40.5 to 1.5 MHz in 128 channels spaced 0.3072 MHz apart) and low band (1326.0 to 1.2 kHz in 70 channels spaced 19.2 kHz apart) in a period of 6 seconds. The receivers measured, on alternate samples, the left hand circular and right hand circular (radio definition) power. Measured Parameters =================== The data here are from the low frequency receiver band and are 'packaged' into spacecraft major frame records. Each major frame is 48 seconds long or eight sweeps through the PRA receiver. The data are calibrated and are given in units of 'millibels' which is 1000 times the log of the received power. Zero millbels corresponds to approximately 1.4 x 10^-21 W m^-2 Hz^-1, however, this value is never seen in practice. The minimum values detected, which includes receiver internal and spacecraft generated noise, are about 2300 to 2400 millibels, or about 3.5 x 10^-19 W m^-2 Hz^-1; even higher values are seen at the very lowest frequencies. The data format is ASCII and consists of a time indicator followed by an array containing the eight low band sweeps. Time is spacecraft event time (SCET) which is basically universal time at the spacecraft. Specifically, time is in the form of YYMMDD and seconds into YYMMDD. Both are written as I6. Example: July 1, 1979 at 12 hours SCET would be 790701, 43200. The seconds correspond, to the nearest second, to the start of the sweep (which occurs in PRA high band). The first value in low band (1326.0 kHz) occurs some 3.9 seconds after this time and samples at successively lower frequencies are spaced 0.03 seconds apart. Only one time is given for the entire major frame, thus the start of each sweep is the time given plus 6 times the sweep number minus 1 (i.e., 0 through 7). The data array is dimensioned as 71 X 8 and written as I4 format (i.e. 568I4). The '8' corresponds to the eight PRA sweeps. The lowest 68 of the 70 low band channels (1287.6 to 1.2 kHz) are in positions 2-69. Positions 70-71 should be ignored. Missing or bad data values are set to zero. In position 1 of each sweep is a status word where the 12 least significant bits have used, although not all 12 have meaning for PRA low band. Numbering those bits 0 for least significant to 11 for most significant, the bits that have meaning are as follows: bit 0: 15 dB attenuator in use when equal to 1 1: 30 dB attenuator in use when equal to 1 2: 45 dB attenuator in use when equal to 1 9,10 (together): polarization of first channel sampled (1326.0 kHz) according to the scheme: +---------------------------+ | | |value bit| | | | 10= | | | | 0 | 1 | |value bit 9=| 0 | R | L | | | 1 | L | R | +---------------------------+ Polarization at successively lower frequencies is opposite to the frequency above it, i.e. either a LRLR or an RLRL pattern. Successive 6-second sweeps start on the opposite polarization as the previous sweep as indicated in the status bits. Note that this polarization is the received polarization, not necessarily the emitted polarization. Correct interpretation of the received polarization depends on the antenna plane orientation relative to the radio source. A good description of this concept can be found in Leblanc Y., Aubier M. G., Ortega-Molina A., Lecacheux A., 1987, J.Geophys. Res. 92, 15125 and in Wang, L. and Carr, T.D., Recalibration of the Voyager PRA antenna for polarization sense measurement, Astron. Astrophys., 281, 945-954, 1994. and references therein. Missing or bad data values are set to zero. If the status word is zero, any data in that receiver sweep should be discarded. Data Coverage ============= The data are stored as 4 ASCII tables (.TAB), each accompanied with a PDS label file (.LBL) which describes properties of the data file. Data cover the following time intervals: Volume ID: VGPR_1201 +------------------------------------------------------------------------+ | Filename |Records| Start | Stop | |------------------------------------------------------------------------| | PRA_I.TAB | 35569| 1979-01-06T00:00:34.000Z | 1979-01-30T23:59:47.000Z| | PRA_II.TAB| 39493| 1979-01-31T00:00:35.000Z | 1979-02-25T23:59:47.000Z| |PRA_III.TAB| 41371| 1979-02-26T00:00:35.000Z | 1979-03-22T23:59:56.000Z| | PRA_IV.TAB| 24587| 1979-03-23T00:00:44.000Z | 1979-04-13T23:59:08.000Z| +------------------------------------------------------------------------+ Confidence Level Overview ========================= The accuracy of calibration in the PRA low band is approximately 2 dB, except at frequencies below 100 kHz where it is somewhat worse. Interference from the Voyager power subsystem is a major problem to the PRA instrument, affecting many of the 70 low band channels. This interference manifests itself by abrupt changes in background levels. Some channels, notably 136 and 193 kHz, are almost always affected, whereas, others are only affected for short intervals. Usually, this interference is only a problem when the natural signals are weak. Additional information associated with this data set is available in the following files: +-----------------------------------------------------------------------------------------------------------------------------------+ | file | contents | | http://ppi.pds.nasa.gov/ditdos/download?id=pds://PPI/VGPR_1201/CATALOG/VG1_PRA1_INST.CAT |VG1 PRA instrument description | | http://ppi.pds.nasa.gov/ditdos/download?id=pds://PPI/VGPR_1201/CATALOG/VG1_PRA_JUP_HRES_DS.CAT | data set description | | http://ppi.pds.nasa.gov/ditdos/download?id=pds://PPI/VGPR_1201/CATALOG/PERSON.CAT | personnel information | | http://ppi.pds.nasa.gov/ditdos/download?id=pds://PPI/VGPR_1201/CATALOG/REF.CAT |key reference description | | http://ppi.pds.nasa.gov/ditdos/download?id=pds://PPI/VGPR_1201/DOCUMENT/INSTRUMENT |ASCII and HTML versions of the PRA| | |investigation description paper | +-----------------------------------------------------------------------------------------------------------------------------------+

42) Spectrograms of Voyager 2 PRA Highband Receiver Jupiter encounter, 48 sec resolution maxmize
Resource ID:spase://VWO/DisplayData/Voyager2/PRA/Jupiter/High.P1D
Start:1979-06-01 00:00:34 Observatory:Voyager 2 Cadence:48 seconds
Stop:1979-07-30 23:59:59 Instrument:Voyager 2 Planetary Radio Astronomy (PRA) experiment Resource:DisplayData
Spectrogram plots in GIF format derived from Voyager 2 Planetary Radio Astronomy (PRA) Highband receiver daily files during Jupiter Encounter (1979-06-01 to 1979-07-30). These plots are available for both polarization channels and in both color and grayscale. The color scale of these plots represent the electric field power spectral density in units of millibels. Across the top of each spectrogram in the spacecraft and instrument name, the name of the binary data file that was used to create this plot, the polarization channel (Left or Right) and the date in the format YYMMDD. The data set provides 48 second resolution highband radio mean power data in units of millibels. The high-band receiver consisted of 128 channels of 200 kHz bandwidth each, with center frequencies spaced at 307.2 kHz intervals from 1.2 MHz to 40.4 MHz. The highband receiver was designed especially for the observation of Jovian decametric radio emissions. The PRA radiometer was usually operated routinely in the so-called POLLO sweeping mode, in which all 198 frequency channels of the high- and low-band receivers together were swept in 6 sec, dwelling at each channel for 25 msec. From one step to the next in the channel switching sequence, the antenna polarization sense was reversed, i.e., was changed from RH to LH or vice versa. Thus the time required for making a measurement of both the RH and LH intensity components at both senses of elliptical polarization at a given frequency was 12 sec. The data consists of successive averages of 4 pairs of RH and LH intensity measurements, each average spanning an interval of 48 sec. The data are calibrated and are given in units of 'millibels' which is 1000 times the log of the received power. Zero millbels corresponds to approximately 1.4 x 10^-21 W m^-2 Hz^-1, however, this value is never seen in practice. The minimum values detected, which includes receiver internal and spacecraft generated noise, are about 2300 to 2400 millibels, or about 3.5 x 10^-19 W m^-2 Hz^-1; even higher values are seen at the very lowest frequencies. Note: The polarization indicated is the received polarization, not necessarily the emitted polarization. Correct interpretation of the received polarization depends on the antenna plane orientation relative to the radio source. A good description of this concept can be found in Leblanc Y., Aubier M. G., Ortega-Molina A., Lecacheux A., 1987, J.Geophys. Res. 92, 15125 and in Wang, L. and Carr, T.D., Recalibration of the Voyager PRA antenna for polarization sense measurement, Astron. Astrophys., 281, 945-954, 1994. and references therein.

43) Voyager 2 PRA Highband Receiver Jupiter encounter, 48 sec resolution maxmize
Resource ID:spase://VWO/NumericalData/Voyager2/PRA/Jupiter/High.PT48S
Start:1979-06-01 00:00:34 Observatory:Voyager 2 Cadence:48 seconds
Stop:1979-07-30 23:59:59 Instrument:Voyager 2 Planetary Radio Astronomy (PRA) experiment Resource:NumericalData
Voyager 2 Planetary Radio Astronomy (PRA) Highband receiver daily files during Jupiter Encounter (1979-06-01 to 1979-07-30). Associated with these binary data are a series of quick-look GIF spectrogram plots created using the binary data. The plots are available for both polarization channels. These binary data were also converted into IDL save sets. The data set provides 48 second resolution highband radio mean power data in units of millibels. The high-band receiver consisted of 128 channels of 200 kHz bandwidth each, with center frequencies spaced at 307.2 kHz intervals from 1.2 MHz to 40.4 MHz. The highband receiver was designed especially for the observation of Jovian decametric radio emissions. The PRA radiometer was usually operated routinely in the so-called POLLO sweeping mode, in which all 198 frequency channels of the high- and low-band receivers together were swept in 6 sec, dwelling at each channel for 25 msec. From one step to the next in the channel switching sequence, the antenna polarization sense was reversed, i.e., was changed from RH to LH or vice versa. Thus the time required for making a measurement of both the RH and LH intensity components at both senses of elliptical polarization at a given frequency was 12 sec. The data consists of successive averages of 4 pairs of RH and LH intensity measurements, each average spanning an interval of 48 sec. The format of these binary data files is as follows: file separation variable year, month, day information millisecond decimal value of the day Integer array (128,2) for 128 left and right channels (NOTE 128 channels for Hi-band; 70 channels for Lo-band) file separation variable There is an IDL program that reads these files into an IDL-format save set. See Information URL for a link to this file. The data are calibrated and are given in units of 'millibels' which is 1000 times the log of the received power. Zero millbels corresponds to approximately 1.4 x 10^-21 W m^-2 Hz^-1, however, this value is never seen in practice. The minimum values detected, which includes receiver internal and spacecraft generated noise, are about 2300 to 2400 millibels, or about 3.5 x 10^-19 W m^-2 Hz^-1; even higher values are seen at the very lowest frequencies. Note: The polarization indicated is the received polarization, not necessarily the emitted polarization. Correct interpretation of the received polarization depends on the antenna plane orientation relative to the radio source. A good description of this concept can be found in Leblanc Y., Aubier M. G., Ortega-Molina A., Lecacheux A., 1987, J.Geophys. Res. 92, 15125 and in Wang, L. and Carr, T.D., Recalibration of the Voyager PRA antenna for polarization sense measurement, Astron. Astrophys., 281, 945-954, 1994. and references therein.

44) Voyager 2 PRA Lowband Receiver Jupiter encounter, 6 sec resolution maxmize
Resource ID:spase://VWO/NumericalData/Voyager2/PRA/Jupiter/Low.PT6S
Start:1979-04-25 00:04:00 Observatory:Voyager 2 Cadence:6 seconds
Stop:1979-08-04 23:05:33 Instrument:Voyager 2 Planetary Radio Astronomy (PRA) experiment Resource:NumericalData
(Description based on material from VG2_PRA_JUP_HRES_DS.CAT) Voyager 2 Radio Astronomy (PRA) data from the Jupiter encounter (1979-04-25 to 1979-08-04). The data set provides 6 second high resolution lowband radio mean power data. The data are provided for 70 instrument channels, covering 1.2 to 1326.0 kHz. This data set (VG2-J-PRA-3-RDR-LOWBAND-6SEC-V1.0) contains data acquired by the Voyager-2 Planetary Radio Astronomy (PRA) instrument during the Jupiter encounter. The bounding time interval set for most Voyager 2 Jupiter PDS data sets is the Voyager project defined 'far encounter' mission phase boundary (1979-07-02 to 1979-08-03). Since, however, the PRA instrument is able to observe planetary phenomenon at much larger ranges than other fields and particles experiments, this boundary is artificial with respect to PRA. Hence, PRA lowband data provided here cover the entire Jupiter Encounter Phase (1979-04-25 to 1979-08-04). Data from beyond the far encounter interval is contained in the cruise data archive which is available from the NSSDC. VG2-J-PRA-3-RDR-LOWBAND-6SEC-V1.0 contains data at the highest time resolution possible during normal operations. The normal mode of PRA operations during the planetary encounters was to sweep through the two radio receiver bands, high band (40.5 to 1.5 MHz in 128 channels spaced 0.3072 MHz apart) and low band (1326.0 to 1.2 kHz in 70 channels spaced 19.2 kHz apart) in a period of 6 seconds. The receivers measured, on alternate samples, the left hand circular and right hand circular (radio definition) power. Measured Parameters =================== The data here are from the low frequency receiver band and are 'packaged' into spacecraft major frame records. Each major frame is 48 seconds long or eight sweeps through the PRA receiver. The data are calibrated and are given in units of 'millibels' which is 1000 times the log of the received power. Zero millbels corresponds to approximately 1.4 x 10^-21 W m^-2 Hz^-1, however, this value is never seen in practice. The minimum values detected, which includes receiver internal and spacecraft generated noise, are about 2300 to 2400 millibels, or about 3.5 x 10^-19 W m^-2 Hz^-1; even higher values are seen at the very lowest frequencies. The data format is ASCII and consists of a time indicator followed by an array containing the eight low band sweeps. Time is spacecraft event time (SCET) which is basically universal time at the spacecraft. Specifically, time is in the form of YYMMDD and seconds into YYMMDD. Both are written as I6. Example: July 1, 1979 at 12 hours SCET would be 790701, 43200. The seconds correspond, to the nearest second, to the start of the sweep (which occurs in PRA high band). The first value in low band (1326.0 kHz) occurs some 3.9 seconds after this time and samples at successively lower frequencies are spaced 0.03 seconds apart. Only one time is given for the entire major frame, thus the start of each sweep is the time given plus 6 times the sweep number minus 1 (i.e., 0 through 7). The data array is dimensioned as 71 X 8 and written as I4 format (i.e. 568I4). The '8' corresponds to the eight PRA sweeps. The lowest 68 of the 70 low band channels (1287.6 to 1.2 kHz) are in positions 2-69. Positions 70-71 should be ignored. Missing or bad data values are set to zero. In position 1 of each sweep is a status word where the 12 least significant bits have used, although not all 12 have meaning for PRA low band. Numbering those bits 0 for least significant to 11 for most significant, the bits that have meaning are as follows: bit 0: 15 dB attenuator in use when equal to 1 1: 30 dB attenuator in use when equal to 1 2: 45 dB attenuator in use when equal to 1 9,10 (together): polarization of first channel sampled (1326.0 kHz) according to the scheme: +---------------------------+ | | |value bit| | | | 10= | | | | 0 | 1 | |value bit 9=| 0 | R | L | | | 1 | L | R | +---------------------------+ Polarization at successively lower frequencies is opposite to the frequency above it, i.e. either a LRLR or an RLRL pattern. Successive 6-second sweeps start on the opposite polarization as the previous sweep as indicated in the status bits. Note that this polarization is the received polarization, not necessarily the emitted polarization. Correct interpretation of the received polarization depends on the antenna plane orientation relative to the radio source. A good description of this concept can be found in Leblanc Y., Aubier M. G., Ortega-Molina A., Lecacheux A., 1987, J.Geophys. Res. 92, 15125 and in Wang, L. and Carr, T.D., Recalibration of the Voyager PRA antenna for polarization sense measurement, Astron. Astrophys., 281, 945-954, 1994. and references therein. Missing or bad data values are set to zero. If the status word is zero, any data in that receiver sweep should be discarded. Data Coverage ============= The data are stored as 4 ASCII tables (.TAB), each accompanied with a PDS label file (.LBL) which describes properties of the data file. Data cover the following time intervals: Volume ID: VGPR_1201 +------------------------------------------------------------------------+ | Filename |Records| Start | Stop | |------------------------------------------------------------------------| | PRA_I.TAB | 32707| 1979-04-25T00:00:04.000Z |1979-05-28T23:59:14.000Z | | PRA_II.TAB| 34207| 1979-05-29T00:00:02.000Z |1979-06-23T23:59:59.000Z | |PRA_III.TAB| 31652| 1979-06-24T00:00:47.000Z |1979-07-12T23:59:58.000Z | | PRA_IV.TAB| 34416| 1979-07-13T00:00:46.000Z |1979-08-04T23:05:33.000Z | +------------------------------------------------------------------------+ Confidence Level Overview ========================= The accuracy of calibration in the PRA low band is approximately 2 dB, except at frequencies below 100 kHz where it is somewhat worse. Interference from the Voyager power subsystem is a major problem to the PRA instrument, affecting many of the 70 low band channels. This interference manifests itself by abrupt changes in background levels. Some channels, notably 136 and 193 kHz, are almost always affected, whereas, others are only affected for short intervals. Usually, this interference is only a problem when the natural signals are weak. Additional information associated with this data set is available in the following files: +-----------------------------------------------------------------------------------------------------------------------------------+ | file | contents | |------------------------------------------------------------------------------------------------|----------------------------------| |http://ppi.pds.nasa.gov/ditdos/download?id=pds://PPI/VGPR_1201/CATALOG/VG2_PRA_INST.CAT | VG1 PRA instrument description | |http://ppi.pds.nasa.gov/ditdos/download?id=pds://PPI/VGPR_1201/CATALOG/VG2_PRA_JUP_HRES_DS.CAT | data set description | |http://ppi.pds.nasa.gov/ditdos/download?id=pds://PPI/VGPR_1201/CATALOG/PERSON.CAT |personnel information | |http://ppi.pds.nasa.gov/ditdos/download?id=pds://PPI/VGPR_1201/CATALOG/REF.CAT |key reference description | |http://ppi.pds.nasa.gov/ditdos/download?id=pds://PPI/VGPR_1201/DOCUMENT/INSTRUMENT |ASCII and HTML versions of the PRA| | |investigation description paper | +-----------------------------------------------------------------------------------------------------------------------------------+

45) Wind Radio/Plasma Wave, (WAVES) Hi-Res Parameters CDF maxmize
Resource ID:spase://VWO/NumericalData/Wind/WAVES/DS.PT1M
Start:1994-11-11 16:00:00 Observatory:Wind Cadence:1 minute
Stop:2016-05-19 13:23:48 Instrument:Plasma and Radio Waves (WAVES) Resource:NumericalData
Wind Waves RAD2, RAD1, and TNR data in CDF format. RAD1 RAD1 is the low frequency radio astronomy receiver. It sweeps over the range of 20 to 1040 kHz with as many as 256 channels. However, some of the time the number of channels is restricted to 16 or 32 so that direction of arrival and polarization information can be obtained. RAD2 RAD2 is the high frequency radio astronomy receiver. It sweeps over the range of 1.075 to 13.825 MHz with as many as 256 channels. However, some of the time the number of channels is restricted to 16 or 32 so that direction of arrival and polarization information can be obtained. TNR The thermal noise receiver (TNR) is designed to actively track the solar wind plasma frequency. TNR consists of 5 overlapping bands. Each band covers 2 octaves, with the next band beginning at the mid point of the lower band. The overall frequency range is 4 - 256 kHz. Usually the tnr is operated in a mode where the first, third and fifth bands are sampled, but occassionally the instrument is driven by neural network software which tries to pick the one band containing the plasma frequency. For more information: The Radio and Plasma Wave Investigation on the Wind Spacecraft, Sp.Sci.Rev.,Vol 71, pg, 231-263,1995

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