CCSD3ZF0000100000001NJPL3IF0PDS200000001 = SFDU_LABEL RECORD_TYPE = STREAM PRODUCT_CREATION_TIME = 1992-05-13 NOTE = "Data Set information for Phobos CD-ROM." OBJECT = DATASET DATA_SET_ID = "PHB2-M-KRFM-3-PHOTOMETRY-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "PHOBOS 2 MARS KRFM PHOTOMETRY V1.0" EVENT_START_TIME = 1989-03-12T21:36:02.497Z EVENT_STOP_TIME = 1989-003 NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = TABLE DATA_SET_RELEASE_DATE = 1992 PROCESSING_LEVEL_ID = 2 PRODUCER_FULL_NAME = "L. KSANFOMALITY" PRODUCER_INSTITUTION_NAME = "IKI, MOSCOW" SOFTWARE_FLAG = N DETAILED_CATALOG_FLAG = N PROCESSING_START_TIME = 1989 PROCESSING_STOP_TIME = 1989 DATA_SET_DESC = "This data set consists of the set of visual and thermal infrared band photometry of Mars obtained by the KRFM experiment on the Phobos 2 spacecraft. The data are presented as a table of samples for 14 wavelength channels, with successive lines (rows) in the table obtained at 1-second intervals. The 5 infrared channels occur first, followed by 9 visual band channels." CONFIDENCE_LEVEL_NOTE = "N/A" END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = MARS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = "N/A" MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = "N/A" MINIMUM_AVAILABLE_SAMPLING_INT = "N/A" SAMPLING_PARAMETER_UNIT = "N/A" DATA_SET_PARAMETER_NAME = RADIANCE NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = DIMENSIONLESS END_OBJECT = DSPARMINFO OBJECT = SCDATASET INSTRUMENT_HOST_ID = PHB2 INSTRUMENT_ID = KRFM END_OBJECT = SCDATASET OBJECT = DSREFINFO REFERENCE_KEY_ID = "MOROZETAL1991 " OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "DATA SET DESCRIPTION, DERIVATION TECHNIQUE, AND ANALYSIS" JOURNAL_NAME = "Planetary and Space Science" PUBLICATION_DATE = 1991 REFERENCE_DESC = "V. Moroz et al, p. 199-207, vol. 39, 1991" OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "V. I. Moroz" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = DATASET OBJECT = DATASET DATA_SET_ID = "PHB2-M-VSK-EDR-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "PHOBOS 2 MARS VSK-FREGAT EDR V1.0" EVENT_START_TIME = 1989-02-21T12:35:11Z EVENT_STOP_TIME = 1989-03-25T10:42:35Z NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = IMAGE DATA_SET_RELEASE_DATE = 1992 PROCESSING_LEVEL_ID = 2 PRODUCER_FULL_NAME = "B. ZHUKOV" PRODUCER_INSTITUTION_NAME = "IKI, MOSCOW" SOFTWARE_FLAG = N DETAILED_CATALOG_FLAG = N PROCESSING_START_TIME = 1989 PROCESSING_STOP_TIME = 1989 DATA_SET_DESC = "This data set consists of the set of images obtained by the VSK-Fregat experiment on the Phobos 2 spacecraft." CONFIDENCE_LEVEL_NOTE = "No absolute intensity calibration is available for these data." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = MARS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = PIXEL SAMPLING_PARAMETER_RESOLUTION = "N/A" MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = "N/A" SAMPLING_PARAMETER_INTERVAL = "N/A" MINIMUM_AVAILABLE_SAMPLING_INT = "N/A" SAMPLING_PARAMETER_UNIT = "N/A" DATA_SET_PARAMETER_NAME = RADIANCE NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = DIMENSIONLESS END_OBJECT = DSPARMINFO OBJECT = SCDATASET INSTRUMENT_HOST_ID = PHB2 INSTRUMENT_ID = VSK END_OBJECT = SCDATASET OBJECT = DSREFINFO REFERENCE_KEY_ID = "AVANESOVETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "EXPERIMENT DESCRIPTION" JOURNAL_NAME = "Planetary and Space Science" PUBLICATION_DATE = 1991 REFERENCE_DESC = "Avanesov, G.A. et al, p. 281-295, vol. 39, 1991" OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "G. A. AVANESOV" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = DATASET OBJECT = DATASET DATA_SET_ID = "PHB2-M-TS-2-THERM/VIS-IMGEDR-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "PHOBOS 2 MARS TERMOSCAN THERMAL/VISIBLE IMAGING EDR V1.0" EVENT_START_TIME = 1989-02-11T10:55:00Z EVENT_STOP_TIME = 1989-03-26T17:49:50Z NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = IMAGE DATA_SET_RELEASE_DATE = 1992 PROCESSING_LEVEL_ID = 2 PRODUCER_FULL_NAME = "Yuri Gektin" PRODUCER_INSTITUTION_NAME = "Institute for Space Device Engineering" SOFTWARE_FLAG = N DETAILED_CATALOG_FLAG = N PROCESSING_START_TIME = 1989 PROCESSING_STOP_TIME = 1989 DATA_SET_DESC = "In February and March, 1989, the Termoskan instrument on board the Phobos '88 spacecraft of the USSR acquired a limited set of very high resolution simultaneous observations of the reflected solar flux (hereafter referred to as the visible channel) and emitted thermal flux (thermal infrared (IR)) from Mars's equatorial region. These are, so far, the highest spatial resolution thermal data ever obtained for Mars. Four slightly overlapping thermal panoramas (also called scans or swaths) cover a large portion of the equatorial region from 30øS to 6øN latitude. Simultaneous visible panoramas were taken during each of the four observing sessions; due to spacecraft memory limitations, visible channel processing was stopped early relative to the thermal channel for 2 of the sessions (2 and 4). Thus, the visible channel panoramas are shorter than the thermal panoramas for these sessions. The instrument was fixed to the spacecraft with the optical axis pointing in the anti-solar direction. As a consequence, all observations are at approximately zero degrees phase angle and only daytime observations were acquired. Scan lines were acquired approximately going from North to South on the planet at a rate of 1 line per second. In the first session (taken Feb 11, 1989), the periapse altitude of the spacecraft's elliptical orbit was 1150 km and the resolution at nadir was approximately 300 m per pixel. The thermal and visible channel panoramas from this session exhibit longitudinal gaps of varying size between scan lines. Within each scan line (acquired in the North-South direction), however, full resolution and coverage were maintained. In the remaining three sessions (one taken on March 1, 1989 and two on March 26, 1989), the panoramas were acquired from a circular orbit of altitude 6300 km with a resolution at nadir of approximately 1.8 km per pixel. In these panoramas, line and frame scanning correspond; therefore, there are not significant gaps between scan lines and geometrical distortions primarily occur only because of the sphericity of the planet. Each image consists of 384 samples. The number of lines varies depending upon how long the instrument was on in any given panorama. The data is 8 bit data with dn values ranging from 0 to 255 for both the thermal and the visible channels. West is towards the top of each image file and North is to the right. All of the Termoskan data is contained in the 23 files of this data set. These files were delivered by the Institute of Space Devices Engineering (ISDE) (Moscow) to Caltech (Pasadena) in April, 1990 (except for session 1 which was delivered a few months earlier). The only difference between the files included here and those delivered from the Institute of Space Devices is that I have mirror flipped some of the files (resulting files all with the extension img: pan1irr1, pan1irr2, pan1vir1, pan1vir2, pan3irr1, pan3irr2, pan3irr3, pan3irr4, pan4vir1, and pan4vir2) as necessary. This was needed because some, but not all, of the image files were delivered from ISDE with the images appearing as Mars would appear if you saw it in a mirror. Each of the thermal channel files in this data set has 512 samples because in addition to the 384 data pixels per line there are also 126 pixels on one side of the image used for temperature stripes - each stripe representing the dn level for an additional 10 K. The visible channel files each have 384 pixels (except for session 1 which has filler pixels to 512 samples). Each of these files are fragments of larger panoramas. The pixels in the thermal channel files and visible channel files are not aligned (do not correspond to the same location on Mars) in this data set. See confidence level notes for more details and see the edited data set for complete panoramas that have been corrected so as to have the thermal data aligned geometrically with the visible channel data." CONFIDENCE_LEVEL_NOTE = "A given line and sample in the raw thermal files will not correspond to the same location on Mars as the same line and sample in any of the visible channel files. Various quirks within the data and the raw data files that cause misalignment of the thermal and visible images are taken into account in the edited data set (file names ending in ed) but not in this raw data set. These include the following. Part of the misalignment problem is just due to the different raw files being of different length. In addition there are: offsets at the beginning of the scans, probably caused by data lines added to the files on Earth; dropped (missing) data lines in some of the thermal data and in some of the visible data (in most of the raw data no gaps are left to distinguish these missing lines); 2 to 3 pixel offsets in the N-S direction between the thermal and visible channels (caused at the spacecraft), i.e., pixels need to be added to the beginning of each thermal line to make the thermal samples line up with the visible channel samples. In addition to the alignment problems, the following occur in the data: noise in every eighth sample of the thermal channel amounting to a positive 1 or 2 dn increase (probably tied somehow into the calibration that was going on at a similar rate); sporadic single pixel spikes that occur occasionally within the data; occasional partial lines which appear corrupted; occasional whole lines with single dn values that appear to preserve geometry, but have no value as data; depending upon the panorama either the first or last of the 384 sample pixels is corrupted in the thermal channel, leaving at most 383 good samples per line; and two bright West-East lines (affecting the same samples in each line) in visible panorama 1 (possibly caused by reflections off the spacecraft?). The thermal channel appears to be very well calibrated to at least 3 K (Murray, et al. 1991)." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = MARS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = PIXEL SAMPLING_PARAMETER_RESOLUTION = 1 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = 384 SAMPLING_PARAMETER_INTERVAL = 1 MINIMUM_AVAILABLE_SAMPLING_INT = "N/A" SAMPLING_PARAMETER_UNIT = "N/A" DATA_SET_PARAMETER_NAME = DN NOISE_LEVEL = "N/A" DATA_SET_PARAMETER_UNIT = DIMENSIONLESS END_OBJECT = DSPARMINFO OBJECT = SCDATASET INSTRUMENT_HOST_ID = PHB2 INSTRUMENT_ID = TS END_OBJECT = SCDATASET OBJECT = DSREFINFO REFERENCE_KEY_ID = "MURRAYETAL1991" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "DATA SET DESCRIPTION, DERIVATION TECHNIQUE, AND ANALYSIS" JOURNAL_NAME = "PLANETARY AND SPACE SCIENCE" PUBLICATION_DATE = 1991 REFERENCE_DESC = "Preliminary Assessment of Termoskan Observations of Mars, Planetary and Space Science, Vol. 39, 1991, pp. 237-265" OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "BRUCE MURRAY" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = DATASET OBJECT = DATASET DATA_SET_ID = " PHB2-M-TS-1-EDITED-THRM/VIS-IMG-EDR-V1.0" OBJECT = DATASETINFO DATA_SET_NAME = "PHOBOS 2 MARS TERMOSKAN EDITED THERMAL/VIS IMAGING EDR V1.0" EVENT_START_TIME = 1989-02-11T10:55:00Z EVENT_STOP_TIME = 1989-03-26T17:49:50Z NATIVE_START_TIME = "N/A" NATIVE_STOP_TIME = "N/A" DATA_OBJECT_TYPE = IMAGE DATA_SET_RELEASE_DATE = 1992-005 PROCESSING_LEVEL_ID = 2 PRODUCER_FULL_NAME = "BRUCE H. BETTS" PRODUCER_INSTITUTION_NAME = "CALIFORNIA INSTITUTE OF TECHNOLOGY" SOFTWARE_FLAG = N DETAILED_CATALOG_FLAG = N PROCESSING_START_TIME = 1992 PROCESSING_STOP_TIME = 1992 DATA_SET_DESC = "The first part of this description repeats general information from the raw data description and the latter part refers specifically to this data set. See the raw data set template for more description of the raw data. In February and March, 1989, the Termoskan instrument on board the Phobos '88 spacecraft of the USSR acquired a limited set of very high resolution simultaneous observations of the reflected solar flux (hereafter referred to as the visible channel) and emitted thermal flux (thermal infrared (IR)) from Mars's equatorial region. These are, so far, the highest spatial resolution thermal data ever obtained for Mars. Four slightly overlapping thermal panoramas (also called scans or swaths) cover a large portion of the equatorial region from 30øS to 6øN latitude. Simultaneous visible panoramas were taken during each of the four observing sessions; due to spacecraft memory limitations, visible channel processing was stopped early relative to the thermal channel for 2 of the sessions (2 and 4). Thus, the visible channel panoramas are shorter than the thermal panoramas for these sessions. The instrument was fixed to the spacecraft with the optical axis pointing in the anti-solar direction. As a consequence, all observations are at approximately zero degrees phase angle and only daytime observations were acquired. Scan lines were acquired approximately going from North to South on the planet at a rate of 1 line per second. In the first session (taken Feb 11, 1989), the periapse altitude of the spacecraft's elliptical orbit was 1150 km and the resolution at nadir was approximately 300 m per pixel. The thermal and visible channel panoramas from this session exhibit longitudinal gaps of varying size between scan lines. Within each scan line (acquired in the North-South direction), however, full resolution and coverage were maintained. In the remaining three sessions (one taken on March 1, 1989 and two on March 26, 1989), the panoramas were acquired from a circular orbit of altitude 6300 km with a resolution at nadir of approximately 1.8 km per pixel. In these panoramas, line and frame scanning correspond; therefore, there are not significant gaps between scan lines and geometrical distortions primarily occur only because of the sphericity of the planet. The dark West-East bands in observing sessions 3 and 4 are from the shadow of Phobos.\n Each image consists of 384 samples. The number of lines varies depending upon how long the instrument was on in any given panorama. The data is 8 bit data with dn values ranging from 0 to 255 for both the thermal and the visible channels. West is towards the top of each image file and North is to the right. There are three major differences between this data set and the raw data set First, the raw data has been stripped of all non-image samples, leaving 384 samples. Second, all panorama fragments of the raw data files have been recombined so that each of the full length edited files (designated by file names ending with ed) contain one entire panorama (either thermal or visible). Thus, there are 8 full length files corresponding to the 4 Termoskan observing sessions. For ease of display on some systems, each of these full length files has also been chopped into 512 line fragments (with file names ending in f# where # is the fragment number for that panorama). Note that the last fragment file of each panorama may have less than 512 lines depending upon the length of the full length file. Third, data from the visible and thermal channels have been aligned so that a given line and sample in a thermal image should correspond to the same location on Mars as the same line and sample in the corresponding visible channel image. Various actions were required to align the thermal and visible data files. Three factors affected the alignment of lines between the thermal and visible files. First, there were offsets at the beginning of files, probably caused by data lines added on Earth. This initial offset was determined by comparison of surface features near the beginnings of the panoramas. Then, non-data lines were removed from the beginning of the appropriate file. Second, there are dropped (missing) data lines in some of the thermal data and in some of the visible data. In most of the raw data, no extra lines were added to fill these gaps. Comparison of the same surface features in both visible and thermal raw images on either side of the dropped lines was used to determine the number of lines missing. This number of black (dn = 0) lines were inserted to represent the missing lines in the edited files. There were rare occurrences of seemingly superfluous dn = 0 lines in the raw data. These lines were removed. Within the raw data set there are also occasional lines with dn = (a constant value not equal to zero). Most of these lines appeared to preserve geometry, so were left in the edited files. There was also a constant offset between thermal and visible samples (North-South direction). The offset ranged from 2 to 3 samples but appeared to be constant for any given observing session. This offset was corrected for in the edited data by adding either 2 or 3 dn = 0 samples to the beginning of each line in the thermal channel. All thermal files within the edited data set have 388 samples per line, with either 2 or 3 leading dn = 0 samples, 384 data samples, and either 1 or 2 trailing dn = 0 samples. All visible channel files have 384 samples per line. The UT start and stop times given in the full length edited file labels are times at the spacecraft, not earth receive times." CONFIDENCE_LEVEL_NOTE = "The alignment of thermal and visible edited files should be good to within approximately +/- 1 pixel. Lengths of the scans derived from the start and stop times and the 1 line per second scan rate do not always agree with the lengths of the scans, probably due primarily to lines added or subtracted at the beginnings and ends of the 'original' (raw) files. However, the magnitude of the difference in all cases is less than 5 minutes (300) lines and thus an insignificant error for most applications. In addition, the following confidence notes remain from the raw data: noise in every eighth sample of the thermal channel amounting to a positive 1 or 2 dn increase (probably tied somehow into the calibration that was going on at a similar rate); sporadic single pixel spikes that occur occasionally within the data; occasional partial lines which appear corrupted; occasional whole lines with single dn values that appear to preserve geometry, but have no value as data; depending upon the panorama either the first or last of the 384 sample pixels is corrupted in the thermal channel, leaving at most 383 good samples per line; and two bright West-East lines (affecting the same samples in each line) in visible panorama 1 (possibly caused by reflections off the spacecraft?). The thermal channel appears to be very well calibrated to at least 3 K (Murray, et al. 1991)." END_OBJECT = DATASETINFO OBJECT = DATASETTARG TARGET_NAME = MARS END_OBJECT = DATASETTARG OBJECT = DSPARMINFO SAMPLING_PARAMETER_NAME = PIXEL SAMPLING_PARAMETER_RESOLUTION = 1 MINIMUM_SAMPLING_PARAMETER = "N/A" MAXIMUM_SAMPLING_PARAMETER = 384 SAMPLING_PARAMETER_INTERVAL = 1 MINIMUM_AVAILABLE_SAMPLING_INT = "N/A" SAMPLING_PARAMETER_UNIT = "N/A" DATA_SET_PARAMETER_NAME = DN NOISE_LEVEL = UNK DATA_SET_PARAMETER_UNIT = DIMENSIONLESS END_OBJECT = DSPARMINFO OBJECT = SCDATASET INSTRUMENT_HOST_ID = PHB2 INSTRUMENT_ID = TS END_OBJECT = SCDATASET OBJECT = DSREFINFO REFERENCE_KEY_ID = "MURRAYETAL1991" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "DATA SET DESCRIPTION, DERIVATION TECHNIQUE, AND ANALYSIS" JOURNAL_NAME = "PLANETARY AND SPACE SCIENCE" PUBLICATION_DATE = 1991 REFERENCE_DESC = "Preliminary Assessment of Termoskan Observations of Mars, Planetary and Space Science, Vol 39, 1991, pp. 237-265" OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "BRUCE MURRAY" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = DSREFINFO END_OBJECT = DATASET END