CCSD3ZF0000100000001NJPL3IF0PDSX00000001 PDS_VERSION_ID = PDS3 RECORD_TYPE = FIXED_LENGTH RECORD_BYTES = 27 FILE_RECORDS = 704 ^TABLE = "G_IMPACT.TAB" DATA_SET_ID = "GO-J-UVS-3-RDR-SL9-G-FRAGMENT-V1.0" SPACECRAFT_NAME = "GALILEO ORBITER" MISSION_PHASE_NAME = "SHOEMAKER-LEVY 9 ENCOUNTER" TARGET_NAME = "JUPITER" OBSERVATION_ID = "SLJNFRAGMG01" NOTE = "UVS observation of impact of G fragment of comet Shoemaker-Levy 9 with Jupiter" START_TIME = 1994-199T07:02:14.445Z STOP_TIME = 1994-199T07:13:21.712Z SPACECRAFT_CLOCK_START_COUNT = "2486477:00:0" SPACECRAFT_CLOCK_STOP_COUNT = "2486487:90:9" PRODUCT_ID = "G_IMPACT.TAB" PRODUCT_CREATION_TIME = 1996-11-08 PRODUCT_NAME = "SL9 G IMPACT DATA" NOTE = "Data numbers recording the impact pass (#19) and average of 52 passes neighboring #19 used to prepare Fig 3 as given in Hord, et al. (1995)" INSTRUMENT_NAME = "ULTRAVIOLET SPECTROMETER" INSTRUMENT_ID = UVS DESCRIPTION = "This file was produced by the Galileo UVS/EUV team at the Laboratory for Atmospheric and Space Physics at the University of Colorado at Boulder. The data contained in the file was generated during the analysis of UVS data from the Shoemaker-Levy 9 comet Fragment G Jupiter impact. This analysis is reported in Geophysical Research Letters, Vol 22, No. 12, pages 1565-1568, June 15, 1995, by C.W. Hord, et al. Figure 3. Times given above are UTC times at the spacecraft. Galileo observed the S-L9 fragment G impact by oscillating the scan platform so that the fields of view of the scan-platform instruments moved to and fro across Jupiter. Each to-and-fro swath lasted 10 2/3 sec and consisted of two 5 1/3 sec passes, labelled even or odd. During the observation the UVS acquired one measurement every 7.6 msec, 4.0/528 sec. For each measurement the counting gate was open for 6.0 msec. Thus each 10 2/3 sec swath contained 1408 6.0 msec samples. The crescent of Jupiter was much smaller than the UVS slit, therefore the wavelength range of the light passing through the exit slit changed slightly as the crescent passed across the instruments field of view. The profiles obtained during each pass do not have flat tops, thus the slope of the profile tops reflect the wavelength dependence of the reflected solar spectrum in the neighborhood of 292 nm. When preparing the average pass profile to compare with the impact flash profile, the profiles from even numbered passes were reversed to allow for this effect." /* Table Description */ OBJECT = TABLE NAME = FRAGMENT_G_IMPACT INTERCHANGE_FORMAT = ASCII COLUMNS = 4 ROWS = 704 ROW_BYTES = 27 OBJECT = COLUMN NAME = PASS_COUNTS DATA_TYPE = ASCII_INTEGER BYTES = 4 START_BYTE = 1 FORMAT = "I4" DESCRIPTION = "The counts recorded during the impact pass. (#19)" END_OBJECT OBJECT = COLUMN NAME = PASS_TRIANGULAR_SMOOTH DATA_TYPE = ASCII_REAL BYTES = 7 START_BYTE = 5 FORMAT = "F7.3" DESCRIPTION = "A triangular smooth of record/column 1 (COUNTS FOR IMPACT PASS) with a full width half maximum of 13 words (0.10 sec)." END_OBJECT OBJECT = COLUMN NAME = AVERAGE_PASS DATA_TYPE = ASCII_REAL BYTES = 7 START_BYTE = 12 FORMAT = "F7.3" DESCRIPTION = "The average of 52 passes neighboring #19 (see SL9_G_PASSES.LABEL file, record/column 7 PASS FLAGS)." END_OBJECT OBJECT = COLUMN NAME = PASS_TRIANGULAR_SMOOTH_AVERAGE DATA_TYPE = ASCII_REAL BYTES = 7 START_BYTE = 19 FORMAT = "F7.3" DESCRIPTION = "A triangular smooth of record/column 3 (AVERAGE OF PASSES), with a full width half maximum of 13 words (0.10 sec)." END_OBJECT END_OBJECT END