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1) ACE field and plasma data propagated to (17,0,0) Re maxmize
Resource ID:spase://VSPO/NumericalData/ACE/MAG_SWEPAM/PT1M
Start:1998-02-05 00:00:00 Observatory:ACE Cadence:1 minute
Stop:2016-09-14 07:52:05 Instrument:ACE Magnetic Field Instrument Resource:NumericalData
This is a family of data sets containing 1-min resolution ACE magnetic field and plasma parameters, in GSE and GSM coordinates, both at the location of the ACE spacecraft and as propagated to the location (17,0,0) Re, GSE. Magnetic field and plasma data are from the ACE MFI and SWEPAM instruments, respectively. Propagation was done by J. Weygand using software provided by D. Weimer. The software determines normal directions to assumed planar phase fronts using a modified minimum variance analysis of 1-min magnetic field data, and propagates data using these normals and the Wind-observed solar wind flow velocity. Magnetic field data consist of three Cartesian components, while plasma data consist of three Cartesian components of the flow velocity vector plus proton density and temperature. Data are current to within about 8 months. Different subdirectories hold data for unique combinations of field vs. plasma parameters, GSE vs. GSM coordinates, and unpropagated vs. propagated data. See the VMO interface for a more detailed breakout.

2) Akebono PWS NPW Data maxmize
Resource ID:spase://VWO/NumericalData/Akebono/PWS/E.NPW.PT2S
Start:1989-02-24 13:32:00 Observatory:Akebono Cadence:2 seconds
Stop:2016-09-14 08:00:15 Instrument:Plasma Wave Observation and Sounder Experiments (PWS) Resource:NumericalData
The Plasma Wave Observation and Sounder Experiment (PWS) observes both natural (NPW) and stimulated (SPW) plasma waves. The frequency range of the NPW system is 20 kHz to 5.12 MHz. These CDF data consist of Electric Field intensities measured by the PWS Recevier 1 (RX1) and Receiver 2 (RX2) units.

3) Apollo 12 Solar Wind Measurements at the Lunar Surface 1-HR Data maxmize
Resource ID:spase://VSPO/NumericalData/Apollo12-LM/SWS/PT1HR
Start:1969-11-19 19:30:00 Observatory:Apollo 12 Lunar Module/ALSEP Cadence:60 minutes
Stop:1976-03-25 08:30:00 Instrument:Solar Wind Spectrometer Resource:NumericalData
This data set contains hourly averaged plasma parameters from the Apollo 12 Solar Wind Spectrometer. Four sets of hourly averaged parameters are computed, using as input data -- (1) all fine-time scale parameters (FTSP), (2) all FTSP computed from spectra with small rms error on curve fitting and thermal speeds less than one-half the bulk velocity, (3) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having only one flow angle that can be directly measured, and (4) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having both flow angles directly measureable. Contained in each of the 4 sets of averages are the proton density, alpha-to-proton ratio, bulk speed, angle of flow, number of spectra, and rms deviations of each average.

4) Apollo 12 Solar Wind Measurements at the Lunar Surface 28-s Data maxmize
Resource ID:spase://VSPO/NumericalData/Apollo12-LM/SWS/PT28S
Start:1969-11-19 18:42:13 Observatory:Apollo 12 Lunar Module/ALSEP Cadence:28 seconds
Stop:1976-03-25 08:35:57 Instrument:Solar Wind Spectrometer Resource:NumericalData
This data set contains the highest time resolution plasma data available (28 sec per spectrum) from the solar wind experiment onboard Apollo 12. Contained in each record are: time, proton density, alpha-to-proton ratio, bulk speed, angle of flow, most probable thermal speed, and various housekeeping and fit parameters relating to the reliability of the calculated plasma parameters. During the local lunar night there is no solar wind signal so there are data gaps of about 15 days each lunation.

5) Apollo 15 Solar Wind Measurements at the Lunar Surface 1-HR Data maxmize
Resource ID:spase://VSPO/NumericalData/Apollo15-LM/SWS/PT1HR
Start:1971-07-31 19:30:00 Observatory:Apollo 15 Lunar Module/ALSEP Cadence:60 minutes
Stop:1972-06-30 17:30:00 Instrument:Solar Wind Spectrometer Resource:NumericalData
This data set contains hourly averaged plasma parameters from the Apollo 15 Solar Wind Spectrometer. Four sets of hourly averaged parameters are computed, using as input data -- (1) all fine-time scale parameters (FTSP), (2) all FTSP computed from spectra with small rms error on curve fitting and thermal speeds less than one-half the bulk velocity, (3) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having only one flow angle that can be directly measured, and (4) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having both flow angles directly measureable. Contained in each of the 4 sets of averages are the proton density, alpha-to-proton ratio, bulk speed, angle of flow, number of spectra, and rms deviations of each average.

6) Apollo 15 Solar Wind Measurements at the Lunar Surface 28-s Data maxmize
Resource ID:spase://VSPO/NumericalData/Apollo15-LM/SWS/PT28S
Start:1971-07-31 19:38:38 Observatory:Apollo 15 Lunar Module/ALSEP Cadence:28 seconds
Stop:1972-06-30 18:14:35 Instrument:Solar Wind Spectrometer Resource:NumericalData
This data set contains the highest time resolution plasma data available (28 sec per spectrum) from the solar wind experiment onboard Apollo 15. Contained in each record are: time, proton density, alpha-to-proton ratio, bulk speed, angle of flow, most probable thermal speed, and various housekeeping and fit parameters relating to the reliability of the calculated plasma parameters. During the local lunar night there is no solar wind signal so there are data gaps of about 15 days each lunation.

7) 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:2016-09-14 08:00:15 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.

8) CRRES Plasma Wave Experiment Survey Dynamic Spectrogram Plots maxmize
Resource ID:spase://VWO/DisplayData/CRRES/PWE/SFR.SA/Survey.DS.PT10H
Start:1990-08-01 17:35:00 Observatory: Cadence:8 seconds
Stop:1991-10-12 00:45:00 Instrument: Resource:DisplayData
This dataset contains one-orbit duration dynamic spectrogram GIF plots of the CRRES/Plasma Wave Experiment Sweep Frequency Receiver and Multichannel Spectrum Analyzer (electric antenna). CRRES was launched on July 25, 1990, into a geosynchronous transfer orbit with perigee altitude of 350 km and an apogee 6.3Re (Earth radii) geocentric. The inclination was 18.2 deg, the orbital period was 9 h and 52 min, and the initial magnetic local time at apogee was 0800 MLT. The plasma wave experiment measures the electromagnetic and/or electrostatic fields detected by three sensors: 1) a 100 m tip-to-tip extendable fine wire long electric dipole antenna (designated WADA for wire antenna deployment assembly), 2) a search coil magnetometer mounted at the end of a 6-m boom, and 3) a 94-m sphere-to-sphere double probe electric antenna (designated SWDA for spherical-double-probe wire deployment assembly) which is part of the EF/LP experiment. The first two sensors are the primary sensors for the plasma wave experiment whereas the third sensor is the primary sensor for EF/LP experiment. Following the antenna extensions, the spacecraft was spun down to approximately 2 rpm. The normal mode of operation for the plasma wave experiment after the antenna extensions has been to have the sweep frequency receiver locked onto the WADA antenna and the multichannel analyzer cycling through all three antennas. The basic CRRES plasma wave experiment instrumentation includes two receivers: 1) a multichannel spectrum analyzer to provide high-time-resolution spectra from 5.6 Hz to 10kHz, and 2) a sweep frequency receiver for high-frequency- resolution spectrum measurements from 100 Hz to 400 kHz. Each plot shows a plasma wave spectrogram for a one orbit (roughly 10 hour) period. The spectrograms cover the frequency range from 5.6 Hz to 400 kHz presented on a logarithmic scale. The data from 5.6-100 Hz are the measurements from the multichannel spectrum analyzer during the portions of its cycling when it is connected to the WADA antenna. Additional marks along the frequency axis indicate the boundaries between bands on the sweep frequency receiver. Band 1 extends from 100 to 800 Hz, Band 2 from 800 to 6.4 kHz, Band 3 from 6.4 to 50 kHz and Band 4 from 50 to 400 kHz. The intensity of the waves are color-coded and are in units of db(V/m/root(Hz)). The red line superimposed on each plot shows the electron cyclotron frequency calculated from the fluxgate magnetometer experiment. The time resolution above 6.4 kHz is one spectrum every 8s. The striations apparent in some emissions are a result of the beating between the spin rate and the sampling rate. Across the top of the figure is "CRRES SFR/SA" for the CRRES Plasma Wave Experiment Sweep Frequency Receiver and Multichannel Spectrum Analyzer, the units of the color scale is provided as well as the color bar with maximum and minimum values. Beneath the time axis is CRRES orbital information: Radial distance in Earth radii, Magnetic Latitude, Magnetic Local Time and L-shell. Along the left edge of the figure is the orbit number followed by the date. Along the right edge of the figure is "The University of Iowa/AFGL", the name of the software package used to create the plots and the date and time in which the plot was created.

9) Callisto Quicklook Solar Spectrogram Plots maxmize
Resource ID:spase://VWO/DisplayData/Callisto/FAS.PT15M
Start:2002-09-07 12:08:00 Observatory: Cadence:
Stop:2016-09-14 08:00:14 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.

10) Cluster 1 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Rumba/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM5 (Rumba) Cadence:0.0000046 seconds
Stop:2016-09-14 08:00:14 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | Bandwidth | Sample Rate | |-----------|--------------| | 9.5 kHz | 27.443 kHz | | 19 kHz | 54.886 kHz | | 77 kHz | 219.544 kHz | +--------------------------+ COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...

11) Cluster 1 WHISPER Natural Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Rumba/WHISPER/PT2S
Start:2000-08-16 12:39:00 Observatory:Cluster FM5 (Rumba) Cadence:2.14 seconds
Stop:2016-09-14 08:00:14 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

12) Cluster 1 WHISPER Active Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Rumba/WHISPER/PT52S
Start:2000-08-16 12:39:00 Observatory:Cluster FM5 (Rumba) Cadence:52 seconds
Stop:2016-09-14 08:00:14 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

13) Cluster 2 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Salsa/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM6 (Salsa) Cadence:0.0000046 seconds
Stop:2016-09-14 08:00:15 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | Bandwidth | Sample Rate | |-----------|--------------| | 9.5 kHz | 27.443 kHz | | 19 kHz | 54.886 kHz | | 77 kHz | 219.544 kHz | +--------------------------+ COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...

14) Cluster 2 WHISPER Natural Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Salsa/WHISPER/PT2S
Start:2000-08-16 12:39:00 Observatory:Cluster FM6 (Salsa) Cadence:2.14 seconds
Stop:2016-09-14 08:00:15 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

15) Cluster 2 WHISPER Active Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Salsa/WHISPER/PT52S
Start:2000-08-16 12:39:00 Observatory:Cluster FM6 (Salsa) Cadence:52 seconds
Stop:2016-09-14 08:00:15 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

16) Cluster 3 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Samba/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM7 (Samba) Cadence:0.0000046 seconds
Stop:2016-09-14 08:00:15 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | Bandwidth | Sample Rate | |-----------|--------------| | 9.5 kHz | 27.443 kHz | | 19 kHz | 54.886 kHz | | 77 kHz | 219.544 kHz | +--------------------------+ COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...

17) Cluster 3 WHISPER Natural Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Samba/WHISPER/PT2S
Start:2000-08-16 12:39:00 Observatory:Cluster FM7 (Samba) Cadence:2.14 seconds
Stop:2016-09-14 08:00:15 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

18) Cluster 3 WHISPER Active Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Samba/WHISPER/PT52S
Start:2000-08-16 12:39:00 Observatory:Cluster FM7 (Samba) Cadence:52 seconds
Stop:2016-09-14 08:00:15 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

19) Cluster 4 Wideband Data Plasma Wave Receiver/High Time Resolution Waveform Data maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Tango/WBD/PT0.0000046S
Start:2001-02-03 05:26:00 Observatory:Cluster FM8 (Tango) Cadence:0.0000046 seconds
Stop:2016-09-14 08:00:15 Instrument:Wide Band Data (WBD) Resource:NumericalData
The following description applies to the Wideband Data (WBD) Plasma Wave Receivers on all four Cluster satellites, each satellite being uniquely identified by its number (1 through 4) or its given name (Rumba, Salsa, Samba, Tango, respectively). High time resolution calibrated waveform data sampled in one of 3 frequency bands in the range 0-577 kHz along one axis using either an electric field antenna or a magnetic search coil sensor. The dataset also includes instrument mode, data quality and the angles required to orient the measurement with respect to the magnetic field and to the GSE coordinate system. The AC electric field data are obtained by using one of the two 88m spin plane electric field antennas of the EFW (Electric Fields and Waves) instrument as a sensor. The AC magnetic field data are obtained by using one of the two search coil magnetometers (one in the spin plane, the other along the spin axis) of the STAFF (Spatio-Temporal Analysis of Field Fluctuations) instrument as a sensor. The WBD data are obtained in one of three filter bandwidth modes: (1) 9.5 kHz, (2) 19 kHz, or (3) 77 kHz. The minimum frequency of each of these three frequency bands can be shifted up (converted) from the default 0 kHz base frequency by 125.454, 250.908 or 501.816 kHz. The time resolution of the data shown in the plots is determined from the WBD instrument mode. The highest time resolution data (generally the 77 kHz bandwidth mode) are sampled at 4.6 microseconds in the time domain (~4.7 milliseconds in the frequency domain using a standard 1024 point FFT). The lowest time resolution data (generally the 9.5 kHz bandwidth mode) are sampled at 36.5 microseconds in the time domain (~37.3 milliseconds in the frequency domain using a standard 1024 point FFT). The availability of these files depends on times of DSN and Panska Ves ground station telemetry downlinks. A list of the status of the WBD instrument on each spacecraft, the telemetry time spans, operating modes and other details are available under Science Data Availability on the University of Iowa Cluster WBD web site at http://www- pw.physics.uiowa.edu/cluster/ and through the documentation section of the Cluster Active Archive (CAA) (http://caa.estec.esa.int/caa). Details on Cluster WBD Interpretation Issues and Caveats can be found at http://www- pw.physics.uiowa.edu/cluster/ by clicking on the links next to the Caution symbol in the listing on the left side of the web site. These documents are also available from the Documentation section of the CAA website. For further details on the Cluster WBD data products see Pickett, J.S., et al., "Cluster Wideband Data Products in the Cluster Active Archive" in _The Cluster Active Archive_, 2010, Springer-Verlag, pp 169-183, and the Cluster WBD User Guide archived at the CAA website in the Documentation section. ... CALIBRATION: ... The procedure used in computing the calibrated Electric Field and Magnetic Field values found in this file can be obtained from the Cluster WBD Calibration Report archived at the CAA website in the Documentation section. Because the calibration was applied in the time domain using simple equations the raw counts actually measured by the WBD instrument can be obtained by using these equations and solving for 'Raw Counts', keeping in mind that this number is an Integer ranging from 0 to 255. Since DC offset is a real number, the resultant when solving for raw counts will need to be converted to the nearest whole number. A sample IDL routine for reverse calibrating to obtain 'Raw Counts' is provided in the WBD Calibration Report archived at the CAA. ... CONVERSION TO FREQUENCY DOMAIN: ... In order to convert the WBD data to the frequency domain via an FFT, the following steps need to be carried out: 1) If Electric Field, first divide calibrated data values by 1000 to get V/m; 2) Apply window of preference, if any (such as Hann, etc.); 3) Divide data values by sqrt(2) to get back to the rms domain; 4) perform FFT (see Bandwidth variable notes for non-continuous modes and/or the WBD User Guide archived at the CAA); 5) divide by the noise bandwidth, which is equal to the sampling frequency divided by the FFT size (see table below for appropriate sampling frequency); 6) multiply by the appropriate constant for the window used, if any. These steps are more fully explained in the WBD Calibration Report archived at the CAA.... +--------------------------+ | Bandwidth | Sample Rate | |-----------|--------------| | 9.5 kHz | 27.443 kHz | | 19 kHz | 54.886 kHz | | 77 kHz | 219.544 kHz | +--------------------------+ COORDINATE SYSTEM USED: ... One axis measurements made in the Antenna Coordinate System, i.e., if electric field measurement, it will either be Ey or Ez, both of which are in the spin plane of the spacecraft, and if magnetic field measurement, it will either be Bx, along the spin axis, or By, in spin plane. The user of WBD data should refer to the WBD User Guide, archived at the CAA, Section 5.4.1 and Figure 5.3 for a description of the three orientation angles provided in these files. Since WBD measurements are made along one axis only, these three angles provide the only means for orienting the WBD measurements with respect to a geocentric coordinate system and to the magnetic field direction ...

20) Cluster 4 WHISPER Natural Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Tango/WHISPER/PT2S
Start:2000-08-16 12:39:00 Observatory:Cluster FM8 (Tango) Cadence:2.14 seconds
Stop:2016-09-14 08:00:15 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

21) Cluster 4 WHISPER Active Electric Power Spectral Density maxmize
Resource ID:spase://VWO/NumericalData/Cluster-Tango/WHISPER/PT52S
Start:2000-08-16 12:39:00 Observatory:Cluster FM8 (Tango) Cadence:52 seconds
Stop:2016-09-14 08:00:15 Instrument:Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Resource:NumericalData
The Waves of HIgh frequency and Sounder for Probing of Electron density by Relaxation (WHISPER) performs the measurement of the electron density on the four satellites of the Cluster project. The two main purposes of the WHISPER experiment are to record the natural waves and to make a diagnostic of the electron density using the sounding technique. The various working modes and the fourier transforms calculated on board provide a good frequency resolution obtained in the bandwidth 2-83 kHz. Onboard data compression by the Digital Wave Processing (DWP) intrument allows a good dynamic and level resolution of the electric signal amplitude.

22) 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.

23) Australian Space Weather Services Culgoora Observatory Spectrograms maxmize
Resource ID:spase://VWO/DisplayData/Culgoora/DS.GIF.PT12H
Start:1992-11-14 20:12:33 Observatory:Culgoora Cadence:
Stop:2016-09-14 08:00:14 Instrument:Culgoora Solar Radiospectrograph Resource:DisplayData
Culgoora and Learmonth Observatories dynamic spectrogram plots display frequency in MHz on the vertical axis and time in UT on the horizontal axis. Each plot spans local daylight hours with time resolution of 3 seconds. The frequency range is 18 - 1800 MHz for Culgoora spectrogams and 25 - 180 MHz for Learmonth spectrograms. The intensity values are color coded and are expressed as relative logarithmic units (0 to 255). The Culgoora spectrograms consist of 4 frequency bands: 18-57, 57-180, 180-570 570 -1800 MHz and Learmonth has 2 bands: 25-75, 75-180 MHz. The two Learmonth bands are each divided into 400 frequency steps. Culgoora spectrograph data is available since November 1992, Learmonth data since June 2000.

24) Dynamics Explorer 1 Plasma Wave Instrument Step Frequency and Low Frequency Correlator Spectrogram Plots maxmize
Resource ID:spase://VWO/DisplayData/DynamicsExplorer1/PWI/SFC.LFC.PT409M
Start:1981-09-16 05:20:00 Observatory:Dynamics Explorer 1 Cadence:
Stop:1984-06-28 23:20:00 Instrument:Dynamics Explorer 1 Plasma Waves Instrument (PWI) Resource:DisplayData
This dataset contains dynamic spectrogram PNG plots of the DE-1/PWI Step Frequency Correlator and Low Frequency Correlator data. Each plot spans one orbital period (6 hours 49 minutes). There are three types of files in this dataset. Those derived from data using: 1) the spin-plane 200m electric antenna (Ex), 2) the spin-axis 8m electric antenna (Ez) and 3) the magnetic antennas (B-H) consisting of a 1.0m^2 loop antenna in the spin plane and a search coil on the spin axis. Each image consists of two panels. The title above each panel indicates the instrument, antenna and frequency range. Each panel is a plot of the power spectral density of received signal (color scale) as a function of operating frequency (in a logarithmic scale on the vertical axis) and time (horizontal axis). Beneath the time labels on the horizontal axis of the spectrograms are ephemeris data: position of the spacecraft in radial distance (Earth radii), McIlwain L-shell, magnetic local time, and geomagnetic latitude. Overlaid on each image are traces of the electron cyclotron frequencies. The file naming convention is: de1_pwi_0000_YYYYMMDD_HHMM_AAA.png where: 0000 - Replace with orbit number YYYYMMDD - Replace with date HHMM - Replace with start time AAA - Replace with antenna string

25) Dynamics Explorer 1 Plasma Wave Instrument Sweep Frequency Receiver-A 2 Hour Dynamic Spectrogram Plots maxmize
Resource ID:spase://VWO/DisplayData/DynamicsExplorer1/PWI/SFR.A.PT2H
Start:1981-09-16 05:20:00 Observatory:Dynamics Explorer 1 Cadence:
Stop:1984-06-28 23:20:00 Instrument:Dynamics Explorer 1 Plasma Waves Instrument (PWI) Resource:DisplayData
This dataset contains two hour duration dynamic spectrogram GIF plots of the DE-1/PWI SFR-A (electric antenna). Each image is a 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 the vertical axis) and time (horizontal axis). At the top center of each plot is a title indicating the University of Iowa, the instrument, and the date. On the upper left is an indication of the receiver used, the upper right is the orbit number. Immediately below the title is a horizontal bar and the label "WB" on the extreme left indicating the time duration when wideband data were acquired. Beneath the time labels on the horizontal axis of the spectrogram are ephemeris data: position of the spacecraft in radial distance (Earth radii), McIlwain L-shell, magnetic local time, and geomagnetic latitude. Overlaid on each image are traces of the electron, hydrogen and oxygen cyclotron frequencies. Running along the left edge of the plot next to the frequency scale is the date represented as two digit year, day of year, hour and minute of the start of the plot.

26) 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 | +-----------------------------------------------------+

27) 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 | +-----------------------------------------------------+

28) Geotail field and plasma data propagated to (17,0,0) Re maxmize
Resource ID:spase://VSPO/NumericalData/Geotail/CPI-MGF-LEP/PT1M
Start:1992-10-09 00:00:00 Observatory:Geotail Cadence:1 minute
Stop:2016-09-14 07:56:51 Instrument:Geotail MGF Resource:NumericalData
This is a family of data sets containing 1-min resolution Geotail magnetic field and plasma parameters, in GSE and GSM coordinates, both at the location of the Geotail spacecraft and as propagated to the location (17,0,0) Re, GSE. Plasma data are from both the CPI and LEP plasma instruments, while field data are from the MGF instrument. Parallel groups of CPI-based and LEP-based data sets are available for the full Geotail mission. Data taken when the spacecraft was inside the Spreiter et al (1966) model bow shock were excluded. Propagation was done by J. Weygand using software provided by D. Weimer. The software determines normal directions to assumed planar phase fronts using a modified minimum variance analysis of 1-min magnetic field data, and propagates data using these normals and the Wind-observed solar wind flow velocity. Magnetic field data consist of three Cartesian components, while plasma data consist of three Cartesian components of the flow velocity vector plus proton density and temperature. Data are current to within about 3 months. Different subdirectories hold data for unique combinations of field vs. plasma parameters, GSE vs. GSM coordinates, CPI-based vs. LEP-based data, and propagated vs. unpropagated data. See the VMO interface for a more detailed breakout.

29) Geotail PWI 24 hour dynamic spectrograms maxmize
Resource ID:spase://VWO/DisplayData/Geotail/PWI/DS.P1D
Start:1992-09-18 00:00:00 Observatory:Geotail Cadence:
Stop:2016-09-14 08:00:14 Instrument:Geotail Plasma Wave Investigation (PWI) Resource:DisplayData
Geotail PWI SFA and MCA dynamic spectrogram plots with frequency in Hz on the vertical axis and time in UT on the horizontal axis. Each file contains one spectrogram from the electric field antennas and one from the magnetic field search coils. The electric field spectrograms span the frequency range 5.62 to 24 Hz (the Multi-Channel Analyzer - MCA instrument) and 24 Hz to 800 kHz (the Sweep Frequency Analyzer - SFA instrument). The intensity values are color coded and are expressed in units of dBV/m/root-Hz. The magnetic field spectrograms also combine the MCA and SFA instruments and span the frequency range 5.62 Hz to 12.5 kHz. The intensity values are color coded and are expressed in units of dB nT/root-Hz. Each plot spans 24 hours. Beneath the time axis of the magnetic field spectrogram are spacecraft GSM coordinates for every 4 hours. Information on the instrument and antenna status is also provided above each spectrogram.

30) Geotail PWI 2 hour dynamic spectrograms maxmize
Resource ID:spase://VWO/DisplayData/Geotail/PWI/DS.PT2H
Start:1992-09-18 00:00:00 Observatory:Geotail Cadence:
Stop:2016-09-14 08:00:14 Instrument:Geotail Plasma Wave Investigation (PWI) Resource:DisplayData
Geotail PWI SFA and MCA dynamic spectrogram plots with frequency in Hz on the vertical axis and time in UT on the horizontal axis. Each file contains one spectrogram from the electric field antennas and one from the magnetic field search coils. The electric field spectrograms span the frequency range 5.62 to 24 Hz (the Multi-Channel Analyzer - MCA instrument) and 24 Hz to 800 kHz (the Sweep Frequency Analyzer - SFA instrument). The intensity values are color coded and are expressed in units of dBV/m/root-Hz. The magnetic field spectrograms also combine the MCA and SFA instruments and span the frequency range 5.62 Hz to 12.5 kHz. The intensity values are color coded and are expressed in units of dB nT/root-Hz. Each plot spans 2 hours. Information on the instrument and antenna status is also provided above each spectrogram.

31) 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.

32) 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.

33) Helios 1 E1 (Rosenbauer) Hourly Plasma Data maxmize
Resource ID:spase://VSPO/NumericalData/Helios1/E1/PT1H
Start:1974-12-12 00:00:00 Observatory:Helios 1 Cadence:1 hour
Stop:1984-12-29 00:00:00 Instrument:Helios 1 E1 Plasma Experiment Resource:NumericalData
These hourly averaged solar wind plasma data from the E1 Plasma Detectors (Rosenbauer) onboard the Helios 1 spacecraft include time, earth-sun-Helios angle, sun-Helios distance (AU), Carrington longitude of Helios, solar-ecliptic latitude, Carrington rotation number, proton bulk speed, temperature, number density, flow angles of ecliptic elevation and azimuth, standard deviations of the plasma parameters, and the number of data points in the hourly averages.

34) Helios 1 E2 Hourly Magnetic Field Data maxmize
Resource ID:spase://VSPO/NumericalData/Helios1/E2/PT1H
Start:1974-12-10 00:00:00 Observatory:Helios 1 Cadence:1 hour
Stop:1976-04-30 00:00:00 Instrument:Fluxgate Magnetometer for Field Fluctuations Resource:NumericalData
This data set contains hour-averaged magnetic field vectors from the Neubauer/Maier experiment on Helios 1. It provides 1-hr average values of the solar ecliptic X, Y, Z components of the magnetic field, in units of centi-gamma. Also available are the number of samples of each component used in the averaging. The location of the spacecraft is specified in terms of ecliptic longitude, heliographic latitude, and radial distance from sun. Data quality flags are also included.

35) Helios 1 E3 Hourly Magnetic Field Data maxmize
Resource ID:spase://VSPO/NumericalData/Helios1/E3/PT1H
Start:1974-12-15 00:00:00 Observatory:Helios 1 Cadence:1 hour
Stop:1978-12-29 00:00:00 Instrument:Fluxgate Magnetometer for Average Fields Resource:NumericalData
This data set contains hour-averaged magnetic field vectors from the Ness/Mariani experiment on Helios 1. Each record contains time, magnetic field intensity and cartesian components in spacecraft-centered solar ecliptic coordinates, standard deviations, numbers of fine-scale points in the average, and an instrument mode indicator. It should be noted that the "average" mode, which was used a minority of the time and involved on-board averaging, may have incorrectly handled range changes caused by occasional significant changes in ambient field intensity. The data set had not been filtered for this effect upon delivery to NSSDC.

36) Helios 1 6-sec magnetic field data maxmize
Resource ID:spase://VSPO/NumericalData/Helios1/E3/PT6.00S
Start:1974-12-15 00:00:00 Observatory:Helios 1 Cadence:6.00 seconds
Stop:1978-12-29 00:00:00 Instrument:Fluxgate Magnetometer for Average Fields Resource:NumericalData
Helios 1 6-sec magnetic field averages from Mariani/Ness experiment

37) Helios 1 Magnetic Field Spectral Density, offline at NSSDC maxmize
Resource ID:spase://VSPO/NumericalData/Helios1/E4/PT8S
Start:1974-12-10 00:00:00 Observatory:Helios 1 Cadence:8 seconds
Stop:1975-09-20 00:00:00 Instrument:Search Coil Magnetometer Resource:NumericalData
This data set contains 8-sec averaged and peak spectral densities of magnetic field component variations in 8 spectral bands with center frequencies logarithmically equispaced between 6.8 Hz and 1470 Hz. Data records also contain time, spacecraft position, spacecraft-sun-Earth angle, spin vector direction, data quality flags, etc.

38) Helios 1 E6 (Kunow) Hourly Particle Fluxes maxmize
Resource ID:spase://VEPO/NumericalData/Helios1/E6/PT1H
Start:1974-12-11 00:00:00 Observatory:Helios 1 Cadence:1 hour
Stop:1983-12-31 00:00:00 Instrument:Cosmic Ray Particles Resource:NumericalData
Data set records contain fluxes of protons in 5 energy ranges (4-13, 13-27, 27-37, 37-51, >51 MeV), alpha particles in 6 energy ranges (2-4, 4-13, 13-27, 27-37, 37-48, >48 MeV/n), and electrons in 2 ranges (0.3-0.8, 0.8-2.0 MeV). The fluxes are averaged over intervals of approximately one hour. Each "data record" (having ending CR and/or LF) spans 4-5 hours and has 10 time-overlapping segments. Each segment has averaging start and stop times plus words for 13 fluxes and words for the statistical uncertainties in the 13 fluxes. However, most words in a given segment have fill values, such that good values for a given flux (species and energy range) and its uncertainty appear only in a minority of the segments. No spacecraft position information is included. Data are from the E6 experiment on Helios 1.

39) Helios 1 E7 (Trainor) Hourly Particle Data maxmize
Resource ID:spase://VSPO/NumericalData/Helios1/E7/PT1H
Start:1974-12-15 00:00:00 Observatory:Helios 1 Cadence:1 hour
Stop:1984-02-12 00:00:00 Instrument:Galactic and Solar Cosmic Rays Resource:NumericalData
This data set contains hourly averaged fluxes of protons measured by the GSFC Galactic and Solar Cosmic Ray experiment on Helios 1. The fixed length ASCII records have been reformatted from the binary format of the originally submitted data set (NSSDC ID 74-097A-08B). Each record contains the date and time in year, month, day, hour, minute, and second. The flux values and statistical errors are included for proton energy ranges of 3.3 - 21.6 MeV, 21.6 - 57 MeV, and above 57 MeV.

40) Helios 1 E7 (Trainor) 30-min fluxes and rates maxmize
Resource ID:spase://VEPO/NumericalData/Helios1/E7/PT30M
Start:1974-12-16 00:00:00 Observatory:Helios 1 Cadence:30 minutes
Stop:1982-12-31 00:00:00 Instrument:Galactic and Solar Cosmic Rays Resource:NumericalData
This data set, created in 2010 by Nand Lal, contains 30-min resolution fluxes and count rates of energetic protons, alpha particles, electrons and X-rays from the E7 experiment (P.I.: J. Trainor, GSFC) flown on the Helios 1 spacecraft. Accompanying each flux and count rate is a statistical uncertainty of the flux or rate. The data are spin-averaged. The data are in 920-character ASCII records and consist of: A. Proton fluxes based on pulse height and rate data in 7 energy windows, 3.40-6.05, 6.05-11.10, 11.10-21.60, 24.52-28.82, 32.00-46.30, 45.30-57.22, 135.2-206.5 MeV. B. Alpha particle fluxes based on pulse heights and count rates in 6 energy windows, 3.20-4.98, 4.98-11.50, 11.50-21.60, 24.51-31.12, 31.12-45.53, 45.53-57.53 MeV/n. C. Combined proton plus alpha particle fluxes based on LET1 and HET count rates in 6 energy windows, 3-6, 6-11, 11-21, 20-30, 32-45, 45-56 MeV/n. D. Alpha particle fluxes based on HET count rates in three energy windows, 20-30, 32-45, 45-57 MeV/n. E. Two count rates primarily due to electrons at 2-4 and 4-8 MeV. F. 21 additional count rates corresponding to individual telescope sensors or sensor combinations. For one sensor, rates at each of several discrimination levels are given). These rates are further discussed in the documentation and in the references provided. A subset of the above parameters (A, B, E) are available with graphical display at the OMNIWeb-Plus interface identified below

41) Helios 1 E8 (Keppler) Hourly Particle Fluxes maxmize
Resource ID:spase://VEPO/NumericalData/Helios1/E8/PT1H
Start:1974-12-10 00:00:00 Observatory:Helios 1 Cadence:1 hour
Stop:1980-12-31 00:00:00 Instrument:Energetic Electron and Proton Detector Resource:NumericalData
Data set records contain hourly count rates of protons and electrons in 16 energy ranges (protons: 15 differential channels between 21 and 677 keV, plus >677 keV; electrons: 15 differential channels between 17 and 835 keV, plus >835 keV), each in 16 22.5 deg azimuthal sectors. Accumulation times for each count rate are also given. No spacecraft position information is included. Data are from the E8 experiment on Helios 1.

42) Helios 1 Hourly Trajectory Data maxmize
Resource ID:spase://VSPO/NumericalData/Helios1/Ephemeris/PT1H
Start:1974-12-10 00:00:00 Observatory:Helios 1 Cadence:1 hour
Stop:1981-09-30 00:00:00 Instrument:Helios 1 Position Resource:NumericalData
This directory includes hourly heliocentric coordinate data for the Helios 1 spacecraft as extracted into the ASCII files HE1TRJyy.asc (yy is the two-digit year) from the merged solar wind magnetic and plasma data set in HELIOS_1/MGD_FREEMAN. All trajectory parameters except solar ecliptic and heliographic inertial coordinates were taken from the original merged dataset. The other parameters were computed and added using the code HELTRJCON in the MGD_FREEMAN directory. Source routines for coordinate conversions in this code were provided by R. Parthasarathy of the Satellite Situation Center at NSSDC. The code READHEL in MGD_FREEMAN was used to read the archived datasets into an intermediate format for input to HELTRJCON. Code HELTRJCN1 was used to correct the solar ecliptic angles as of 6/14/94 (see Note 2 above). HELTRJCON was also corrected as of this date. Data Parameter Description: NY - YEAR OF THE DATA INTERVAL (LAST TWO DIGITS ONLY). ND - DAY OF THE DATA INTERVAL FROM THE FIRST DAY OF THE ABOVE YEAR, JAN. 1= DAY 1. NH - HOUR OF THE DAY OF THE DATA INTERVAL. NCARROT - CARRINGTON ROTATION NUMBER AS SEEN BY AN EARTH BASED OBSERVER AT THE START OF THE DATA INTERVAL. SPAU - SPACECRAFT HELIOCENTRIC DISTANCE IN ASTRONOMICAL UNITS. SECLAT - SOLAR ECLIPTIC LATITUDE IN DEGREES SECLON - SOLAR ECLIPTIC LONGITUDE IN DEGREES HELLAT - SOLAR HELIOGRAPHIC LATITUDE IN DEGREES HELLON - SOLAR HELIOGRAPHIC (CARRINGTON) LONGITUDE IN DEGREES HILLON - SOLAR HELIOGRAPHIC INERTIAL LONGITUDE IN DEGREES WITH RESPECT TO ASCENDING NODE OF SOLAR EQUATOR ON THE ECLIPTIC ESSCSANG - EARTH-SUN-SPACECRAFT SEPARATION ANGLE (IN DEGREES, 0-360). ICODE - DATA CODE: 1 MEANS PLASMA DATA ONLY ARE PRESENT FOR THAT HOURLY INTERVAL; 2 MEANS MAGNETOMETER DATA ONLY; 3 MEANS BOTH PLASMA AND MAGNETOMETER DATA PRESENT. Note 1: The solar ecliptic coordinates are given with respect to true equinox and ecliptic of date. The solar ascending node was located at ecliptic longitude +74.367 degrees as of 1 Jan. 1900 at 1200 UT; this longitude increases by 1.4 degrees/century. Note 2: The solar ecliptic cordinates in this directory before 6/14/94 were calculated incorrectly and have been corrected as of this date. The heliographic angles are from the original source dataset and had no problems.

43) Helios 1 Daily Trajectory Data maxmize
Resource ID:spase://VSPO/NumericalData/Helios1/Ephemeris/PT24H
Start:1974-12-10 00:00:00 Observatory:Helios 1 Cadence:24 hours
Stop:1981-09-30 00:00:00 Instrument:Helios 1 Position Resource:NumericalData
This data set contains orbital parameters for Helios 1: Helios-Sun distance, heliographic longitude from the ascending node, heliographic latitude, ecliptical longitude from the mean equinox, ecliptical longitude from the Earth-Sun line, ecliptical latitude, Helios - Earth distance, and number of rotations of the Sun referred to Helios since launch.

44) Helios 2 E1 (Rosenbauer) Hourly Plasma Data maxmize
Resource ID:spase://VSPO/NumericalData/Helios2/E1/PT1H
Start:1976-01-17 00:00:00 Observatory:Helios 2 Cadence:1 hour
Stop:1980-03-04 00:00:00 Instrument:Helios 2 E1 Plasma Experiment Resource:NumericalData
These hourly averaged solar wind plasma data from the E1 Plasma Detectors (Rosenbauer) onboard the Helios 2 spacecraft include time, earth-sun-Helios angle, sun-Helios distance (AU), Carrington longitude of Helios, solar-ecliptic latitude, Carrington rotation number, proton bulk speed, temperature, number density, flow angles of ecliptic elevation and azimuth, standard deviations of the plasma parameters, and the number of data points in the hourly averages.

45) Helios 2 E2 Hourly Magnetic Field Data maxmize
Resource ID:spase://VSPO/NumericalData/Helios2/E2/PT1H
Start:1976-01-15 00:00:00 Observatory:Helios 2 Cadence:1 hour
Stop:1979-06-27 00:00:00 Instrument:Fluxgate Magnetometer for Field Fluctuations Resource:NumericalData
This data set contains hour-averaged magnetic field vectors from the Neubauer/Maier experiment on Helios 2. It provides 1-hr average values of the solar ecliptic X, Y, Z components of the magnetic field, in units of centi-gamma. Also available are the number of samples of each component used in the averaging. The location of the spacecraft is specified in terms of ecliptic longitude, heliographic latitude, and radial distance from sun. Data quality flags are also included.

46) Helios 2 E3 Hourly Magnetic Field Data maxmize
Resource ID:spase://VSPO/NumericalData/Helios2/E3/PT1H
Start:1976-01-17 00:00:00 Observatory:Helios 2 Cadence:1 hour
Stop:1980-03-08 00:00:00 Instrument:Fluxgate Magnetometer for Average Fields Resource:NumericalData
This data set contains hour-averaged magnetic field vectors from the Ness/Mariani experiment on Helios 2. Each record contains time, magnetic field intensity and cartesian components in spacecraft-centered solar ecliptic coordinates, standard deviations, numbers of fine-scale points in the average, and an instrument mode indicator. It should be noted that the "average" mode, which was used a minority of the time and involved on-board averaging, may have incorrectly handled range changes caused by occasional significant changes in ambient field intensity. The data set had not been filtered for this effect upon delivery to NSSDC.

47) Helios 2 40.5-sec Combined Magnetic Field and Plasma Data maxmize
Resource ID:spase://VSPO/NumericalData/Helios2/E3/PT40.5S
Start:1976-01-17 00:00:00 Observatory:Helios 2 Cadence:40 seconds
Stop:1980-03-08 00:00:00 Instrument:Fluxgate Magnetometer for Average Fields Resource:NumericalData
Helios 2 40-second merged magnetic field and plasma data

48) Helios 2 6-sec magnetic field data maxmize
Resource ID:spase://VSPO/NumericalData/Helios2/E3/PT6.00S
Start:1976-01-17 00:00:00 Observatory:Helios 2 Cadence:6.00 seconds
Stop:1980-03-08 00:00:00 Instrument:Fluxgate Magnetometer for Average Fields Resource:NumericalData
Helios 2 6-sec magnetic field averages from Mariani/Ness experiment

49) Helios 2 Magnetic Field Spectral Density, offline at NSSDC maxmize
Resource ID:spase://VSPO/NumericalData/Helios2/E4/PT8S
Start:1976-01-15 00:00:00 Observatory:Helios 2 Cadence:8 seconds
Stop:1976-11-21 00:00:00 Instrument:Search Coil Magnetometer Resource:NumericalData
This data set contains 8-sec averaged and peak spectral densities of magnetic field component variations in 8 spectral bands with center frequencies logarithmically equispaced between 6.8 Hz and 1470 Hz. Data records also contain time, spacecraft position, spacecraft-sun-Earth angle, spin vector direction, data quality flags, etc.

50) Helios 2 E6 (Kunow) Hourly Particle Fluxes maxmize
Resource ID:spase://VEPO/NumericalData/Helios2/E6/PT1H
Start:1976-01-16 00:00:00 Observatory:Helios 2 Cadence:1 hour
Stop:1980-03-08 00:00:00 Instrument:Cosmic Ray Particles Resource:NumericalData
Data set records contain fluxes of protons in 5 energy ranges (4-13, 13-27, 27-37, 37-51, >51 MeV), alpha particles in 6 energy ranges (2-4, 4-13, 13-27, 27-37, 37-48, >48 MeV/n), and electrons in 2 ranges (0.3-0.8, 0.8-2.0 MeV). The fluxes are averaged over intervals of approximately one hour. Each "data record" (having ending CR and/or LF) spans 4-5 hours and has 10 time-overlapping segments. Each segment has averaging start and stop times plus words for 13 fluxes and words for the statistical uncertainties in the 13 fluxes. However, most words in a given segment have fill values, such that good values for a given flux (species and energy range) and its uncertainty appear only in a minority of the segments. No spacecraft position information is included. Data are from the E6 experiment on Helios 2.

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