MGN RSS Bistatic Radar Raw and Calibrated Data
Magellan Bistatic Radar calibrated data archive contains calibrated data from three orbits of S-Band (13 cm wavelength) Magellan bistatic radar data collected with NASA antenna DSS 63 on 5 June 1994 when the specular point crossed Maxwell Montes. The archive has been migrated from the PDS3 standard to PDS4 standard. The original PDS3 archive spans multiple volumes. The directories from these volumes have been merged into the PDS4 bundle and some redundant files excluded. Details of this merge are provided in geo_notes_and_errata.pdf. PDS4 labels and other PDS4 products have also been added. All data products have been given PDS4 labels. Some PDS3 files remain but are not considered part of the PDS4 bundle, such as aareadme.txt in the root directory. The aareadme.txt and voldesc.cat files in the root directory are from the last PDS3 volume. The original BSR Calibrated PDS3 volumes will remain available at the links for the time being.
Magellan Radio Science Calibrated Products that use the PDS4 standard:
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Type |
Description |
PDS4 Collection |
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Binary Spacecraft and Planetary Data Record - The Binary Spacecraft and Planetary (BSP) ephemeris file contains information on the spacecraft trajectory and the motions of the Sun, planets, smaller objects, and barycenters as a function of time. More Information: |
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PRR data collection are the amplitude-calibrated complex time sample. PRR data contains double precision complex time samples, originally from an open loop receiver at a site like a NASA Deep Space Network station. The original integer samples have been converted to double precision complex format; amplitude and/or frequency filtering may have been applied. The header record for this file may provide brief history information. The remainder of the file contains time samples. The file is in the FND format adopted and used by G.L. Tyler's group at Stanford University (the Stanford University Element, or SUE). More Information: |
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PRT data collection are the amplitude- and frequency-calibrated complex time samples. The PRT data have the major sources of Doppler shift and other frequency effects removed. PRT data contains double precision complex time samples, originally from an open loop receiver at a site like a NASA Deep Space Network station. The original integer samples have been converted to double precision complex format; amplitude and/or frequency filtering may have been applied. The header record for this file may provide brief history information. The remainder of the file contains time samples. The file is in the FND format adopted and used by G.L. Tyler's group at Stanford University (the Stanford University Element, or SUE). More Information: |
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This file contains coefficients for a third-order polynomial which, when evaluated, gives the scale factor to be applied to a signal of interest over a range of times. The file has eleven header lines, then an arbitrary number of lines, each listing four coefficients for a cubic equation, valid over a time interval that is specified at the end of the line. The file is used as input to the GAIN program, developed by R.A. Simpson, for adjusting the amplitude of digital samples at Stanford University. More Information: |
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This file contains coefficients for a third-order polynomial which, when evaluated, gives the frequency of a signal of interest over a range of times. The file has eleven header lines, then an arbitrary number of lines, each listing four coefficients for a cubic equation, valid over a time interval that is specified at the end of the line. The file is used as input to the 'steering' process, developed by G.L. Tyler, for adjusting the frequency of digitally sampled data at Stanford University. More Information: |
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This file contains coefficients for a third-order polynomial which, when evaluated, gives the frequency of a signal of interest over a range of times. The file has eleven header lines, then an arbitrary number of lines, each listing four coefficients for a cubic equation, valid over a time interval that is specified at the end of the line. The file is used as input to the 'steering' process, developed by G.L. Tyler, for adjusting the frequency of digitally sampled data at Stanford University. More Information: |
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This file contains calibrated echo spectra from MAGELLAN (MGN) bistatic radar experiments, collected using antennas and 'open loop' receivers at stations of the NASA Deep Space Network (DSN). The processing was carried out at Stanford University. These data have been processed so that the surface echo is approximately centered in the frequency window. The file consists of two ASCII tables. A header table identifies source data from which the file was constructed. The data table includes the actual spectra. More Information: |
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Average S-Band right-circularly polarized (RCP) noise power spectrum from raw data collected at the end of the bistatic radar observations on MAGELLAN orbit 13031 on 5 June 1994. 227 seconds of data were collected with the ground antenna aimed at Venus; these were transformed into 5542 1024-point power spectra which were then summed. Fifteen frequency bins (bins 873-887, centered on about 21500 Hz) contained a spacecraft signal which was removed by linear interpolation between bins 872 and 888. The resulting spectrum was then normalized so that values between about 3000 and 21000 Hz were in the range approximately 0.9-1.1; this result was then multiplied by the weighting factor 5542. 140 seconds of data were collected with the receiver connected to its ambient load. These were transformed into 3427 1024-point power spectra, summed, normalized to the approximate range 0.9-1.1, and then multiplied by the weighting factor 3427. The two weighted power spectra were then added and the sum was divided by 1E9 (an arbitrary choice). The spectrum includes effects of windowing added by the FNDLOOK program, which computes power spectra at Stanford. More Information: |
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This file summarizes observing geometry for MAGELLAN (VEX) bistatic radar (BSR) observations. The results apply to both atmospheric occultations and surface scattering, but more parameters of interest for surface studies have been included. The keywords for start and stop time (above) are Earth Receive Time (ERT). The file comprises two tables. The first table is a single row which identifies the calculation (fingerprints). The second table (with many rows) is the geometry summary itself. At Stanford, file names are of the form ydddHmmC.SRG where y is the one-digit year, ddd is the 3-digit day-of-year, H is a letter denoting the hour (A=00, B=01, ..., X=23), and mm is the 2-digit minute of the first data in the file. C indicates version of the file; C='A' is the first version, 'B' is the second version, etc. This file was produced by Dick Simpson of the VEX Radio Science Team (RST) Stanford University Element (SUE). More Information: |
Magellan Radio Science Raw Products that use the PDS3 standard:
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Type |
Description |
Data Set |
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Radio Science Original Data Records - Original Data Records (ODRs) are raw data generated by the NASA Deep Space Network Radio Science System. The raw data are 8-bit samples of the output from one or more open-loop receivers. More Information: |
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Radio Science Tracking Data File Records - The Tracking Data File (TDF, or sometimes Archival Tracking Data File -- ATDF) is produced by the NASA/JPL Deep Space Network (DSN) Radio Metric Data Conditioning Team for use in determining spacecraft trajectories, gravity fields affecting them, and radio propagation conditions. More Information: |