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VOYAGER 2 JUP PLASMA WAVE SPECTROMETER RESAMP SPEC 48.0SEC
This data set consists of 48-second calibrated, averaged wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Jovian magnetosphere. For each 48-second interval, a geometric average field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kilo- Hertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of averages is the beginning of the averating interval. Averages are stored in units of volt/meter. During data gaps where complete 48-second intervals are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Gurnett et al. [1979] and a complete instrument description can be found in Scarf and Gurnett [1977].
VOYAGER 2 SATURN PLASMA WAVE SPECTROMETER EDITED SPEC 4.0SEC
This data set consists of 4-second edited, wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Saturnian magnetosphere. For each 4-second interval, a field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kiloHertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of intensities (16 channels) is the time of the beginning of the scan. During data gaps where complete 4-second spectra are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. When one or more channels are missing within a scan, the missing measurements are zero-filled. Data are edited but not calibrated. The data numbers in this data set can be plotted in raw form for event searches and simple trend analysis since they are roughly proportional to the log of the electric field strength. Calibration procedures and tables are provided for use with this data set
Cluster-Salsa Wideband Data (WBD) Plasma Wave Receiver/High Time Resolution Waveform Data
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 Science Archive (CSA) (https://www.cosmos.esa.int/web/csa/documentation). 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 CSA 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 CSA 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 CSA 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 CSA. ... 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 CSA); 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 CSA.... +--------------------------+ 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 CSA, Section 5.4.1
Cluster-Rumba Wideband Data (WBD) Plasma Wave Receiver/High Time Resolution Electric and Magnetic Waveform Data Returned via BM2
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 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 Science Archive (CSA) (https://www.cosmos.esa.int/web/csa/documentation). 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 CSA 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 CSA 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 CSA 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 CSA. ... 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 CSA); 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 CSA.... BURST MODE: ... WBD data can also be obtained in a mode called Burst Mode 2 (BM2), stored onboard, and transmitted to the ground with the data from all the other instruments. This mode has been rarely used throughout the mission only once prior to July 2010 (on March 7, 2001), but more often thereafter to obtain data at low altitude or in the high priority auroral acceleration region, because it results in decreased bandwidth or a higher degree of duty cycling for WBD. NASA's Deep Space Network terminated WBD data acquisition in February 2015 and after that date WBD
Wind Radio/Plasma Wave, (WAVES) Hi-Res Parameters CDF
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
Wind Plasma and Radio Waves (WAVES) Time Domain Sampler (TDS) Dust Impact, Level 3, 1 s Data
Wind WAVES Time Domain Sampler, TDS, Dust Data File References: 1) Bougeret, J.-L., et al., WAVES: The Radio and Plasma Wave Investigation on the Wind Spacecraft, Space Sci. Rev., 71, 231-263, 1995, doi:10.1007/BF00751331. 2) Malaspina, D.M., M. Horanyi, A. Zaslavsky, K. Goetz, L.B. Wilson III, and K. Kersten, Interplanetary and Interstellar Dust observed by the Wind/WAVES Electric Field Instrument, Geophys. Res. Lett., 41, 266-272, 2014, doi:10.1002/2013GL058786. 3) Malaspina, D.M., and L.B. Wilson III, A Database of Interplanetary and Interstellar Dust Detected by the Wind Spacecraft, J. Geophys. Res., 121, 9369-9377, 2016, doi:10.1002/2016JA023209.
DE 1 Plasma Wave Instrument (PWI) Low Frequency Correlator Electric and Magnetic Field Spectral Density
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.
DE 1 Plasma Wave Instrument (PWI) Step Frequency Correlator Electric and Magnetic Field Spectral Density
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.
VG2 J PLASMA WAVE SPECTROMETER DENSITY 1S V1.0
Electron plasma density data set for Jupiter's outer magnetosphere derived from high-resolution wideband measurements of low-frequency radio and plasma waves obtained by Voyagers 1 and 2 during their 1979 flybys. Density data were measured at 1-second intervals.
VOYAGER 2 SAT PLASMA WAVE SPECTROMETER RESAMP SPEC 48.0SEC
This data set consists of 48-second calibrated, averaged wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Saturnian magnetosphere. For each 48-second interval, a geometric average field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kilo- Hertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of averages is the beginning of the averating interval. Averages are stored in units of volt/meter. During data gaps where complete 48-second intervals are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Scarf et al. [1982] and a complete instrument description can be found in Scarf and Gurnett [1977].
VOYAGER 1 SAT PLASMA WAVE SPECTROMETER RESAMP SPEC 48.0SEC
This data set consists of 48-second calibrated, averaged wave electric field intensities from the Voyager 1 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Saturnian magnetosphere. For each 48-second interval, a geometric average field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kilo- Hertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of averages is the beginning of the averating interval. Averages are stored in units of volt/meter. During data gaps where complete 48-second intervals are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Gurnett et al. [1981] and a complete instrument description can be found in Scarf and Gurnett [1977].
VG1 J PLASMA WAVE SPECTROMETER DENSITY 1S V1.0
Electron plasma density data set for Jupiter's outer magnetosphere derived from high-resolution wideband measurements of low-frequency radio and plasma waves obtained by Voyagers 1 and 2 during their 1979 flybys. Density data were measured at 1-second intervals.
VOYAGER 1 SATURN PLASMA WAVE SPECTROMETER EDITED SPEC 4.0SEC
This data set consists of 4-second edited, wave electric field intensities from the Voyager 1 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Saturnian magnetosphere. For each 4-second interval, a field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kiloHertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of intensities (16 channels) is the time of the beginning of the scan. During data gaps where complete 4-second spectra are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. When one or more channels are missing within a scan, the missing measurements are zero-filled. Data are edited but not calibrated. The data numbers in this data set can be plotted in raw form for event searches and simple trend analysis since they are roughly proportional to the log of the electric field strength. Calibration procedures and tables are provided for use with this data set
Polar Plasma Wave Instrument (PWI), High Frequency Waveform Receiver, 16 kHz bandwidth, 6-channel Fields
PWI>Plasma Wave Instrument Reference: Gurnett, D.A., et al., The Polar Plasma Wave Instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995. donald-gurnett@uiowa.edu An FFT on 2048 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series. Coordinate system used: local magnetic field-aligned, a spacecraft centered coordinate system where Z is parallel to the local B-field determined from Polar MFE, X points outward and lies in the plane defined by the Z-axis and the radial vector from the earth to the spacecraft, and Y completes a right-handed system and points eastward. The X- and Z-axes are contained in the north-south plane. Effective bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t. These data come in snapshots of 2048 points per channel, every 128.8 seconds, where the duration of each snapshot is 0.057 seconds. The time for individual samples is their individual epoch time (in CDF TT2000). The unattenuated frequency range for this file type is 20Hz to 16000Hz. The cadence value given here is computed from the inverse of the sampling rate (35712 Hz). For a description of the PWI receivers and the different operational modes see https://space.physics.uiowa.edu/plasma-wave/polar/modes.html
VOYAGER 2 JUP PLASMA WAVE SPECTROMETER EDITED SPEC 4.0SEC
This data set consists of 4-second edited, wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Jovian magnetosphere. For each 4-second interval, a field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kiloHertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of intensities (16 channels) is the time of the beginning of the scan. During data gaps where complete 4-second spectra are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. When one or more channels are missing within a scan, the missing measurements are zero-filled. Data are edited but not calibrated. The data numbers in this data set can be plotted in raw form for event searches and simple trend analysis since they are roughly proportional to the log of the electric field strength. Calibration procedures and tables are provided for use with this data set
VG2 J/S/U/N/SS PLASMA WAVE SPECTROMETER RAW WFRM 60MS V1.0
The Voyager 2 Plasma Wave Spectrometer (PWS) raw full resolution data set consists of electric field waveform samples from the Voyager 2 Plasma Wave Subsystem waveform receiver obtained during the entire mission. Data will continue to be added to the archive on subsequent volumes. The data set encompasses all waveform observations obtained in the cruise mission phases before, between, and after the Jupiter, Saturn, Uranus, and Neptune encounter phases as well as those obtained during the four encounter phases. Data for this data set are acquired from the PWS waveform receiver. Data are presented as time series of 4-bit voltage measurements acquired at the rate of 28,800 samples per second through a 40 Hz to 12 kHz bandpass filter. An automatic gain control is used to keep the signal within the usable range of the 4-bit digitization, however, the gain information is not returned to the ground, hence, there is no direct, absolute calibration. However, a power spectrum analysis returns a spectrum that has accurate relative amplitudes between spectral elements. This data set provides the highest temporal resolution data from the Voyager mission. 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.
VOYAGER 2 JUP PLASMA WAVE SPECTROMETER RESAMP SPEC 48.0SEC
This data set consists of 48-second calibrated, averaged wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Jovian magnetosphere. For each 48-second interval, a geometric average field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kilo- Hertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of averages is the beginning of the averating interval. Averages are stored in units of volt/meter. During data gaps where complete 48-second intervals are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Gurnett et al. [1979] and a complete instrument description can be found in Scarf and Gurnett [1977].
ICE PLASMA WAVE MAGNETIC FIELD MEASUREMENT DATA V1.0
The Plasma Wave Data were submitted to National Space Science Data Center after the Principal Investigator's death (Scarf) by S. Chang of TRW. For the magnetic field data, the time interval submitted was Sept 9 - 14, 1985 was included. That information, as well as an explanation of the reformatted data is detailed.
Polar Plasma Wave Instrument (PWI), High Frequency Waveform Receiver, 16 kHz, Time Domain Fields.
The unattenuated frequency range for this file type is 20Hz to 16000Hz. The cadence value given here is computed from the inverse of the sampling rate (35.71 kHz). For a description of the PWI receivers and the different operational modes see: http://www-pw.physics.uiowa.edu/plasma-wave/istp/polar/modes.html
Polar Plasma Wave Instrument (PWI), Low Frequency Waveform Receiver, ~0.01 sec resolution fields
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.
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