PDS_VERSION_ID = PDS3 RECORD_TYPE = "FIXED_LENGTH" RECORD_BYTES = 19 FILE_RECORDS = 6 DATA_SET_ID = "IHW-C-IRSPEC-3-EDR-HALLEY-V2.0" PRODUCT_ID = "IRSP0011" PRODUCT_NAME = "IHW IR SPECTROSCOPY 222002" PRODUCT_CREATION_TIME = 2006-05-12 INSTRUMENT_HOST_NAME = "IHW INFRARED STUDIES NETWORK" INSTRUMENT_HOST_ID = "IRSN" INSTRUMENT_NAME = "IHW INFRARED SPECTROSCOPY DATA" INSTRUMENT_ID = "IRSPEC" TARGET_NAME = "1P/HALLEY 1 (1682 Q1)" START_TIME = 1985-12-14T04:48 STOP_TIME = "UNK" OBSERVATION_TIME = 1985-12-14T04:48 PROCESSING_LEVEL_ID = "3" OBSERVATION_ID = "222002" OBSERVER_FULL_NAME = "HERTER,T/ET AL." DESCRIPTION = " System code: 25009800 Observatory Info Name: NASA KAO (Position at time of observation unknown) Location: NASA-AMES, MOFFETT FIELD, CA Telescope: 0.9-M Instrument: CORNELL U. 7-CHANNEL SPECTROPHOTOMETER Spectral Range: 15.940-17.182 microns Resolution: 0.2 microns Aperture Size: 30 arcseconds Comments from the FITS header: REFERENC Herter, T., Campins, H., Gull, G.E., 1987, Astron. Astrophys. REFERENC 187, 629. REFERENC Herter, T., Gull, G.E., Campins, H. 1986, REFERENC 20th ESLAB Symposium on the Exploration of Halley's Comet, REFERENC ESA SP-250, 2, 117. ADD.OBS. MOSELEY,S/CAMPINS,H/LOEWENSTEIN,R Delta lambda is fairly constant over the entire spectrum. Data form a two-dimensional array in column-major order where row 1 = wavelength in microns, row 2 = flux, row 3 = 1-sigma error Fluxes and errors have been multiplied by ten to the 17th. Flux is in watts per centimeter squared per micron. Data were corrected via cross calibration on Alpha Ori with the moon from August 1985. This version is from original Alpha Ori calibration. " NOTE = " The following erratum was noted by Mikael Aronsson for this file: The spectral resolution is given as 0.2 microns in the [original] FITS header (in the RESOL-SP keyword) even though the wavelength increment ranges from 0.244 to 0.256 microns. The START_TIME listed is actually the OBSERVATION_TIME, i.e., the midpoint of the observation. Exposure times were not reported, so it was not possible to determine the actual starting time of the observation. However, START_TIME is a keyword used to search for data across large sections of the PDS archives, so the midpoint time has been repeated as the START_TIME to prevent these data being lost for want of a more accurate value. " ^TABLE = "IRSP0011.TAB" OBJECT = TABLE INTERCHANGE_FORMAT = "ASCII" ROWS = 6 ROW_BYTES = 19 COLUMNS = 3 OBJECT = COLUMN COLUMN_NUMBER = 1 NAME = "WAVELENGTH" START_BYTE = 1 BYTES = 6 DATA_TYPE = "ASCII_REAL" FORMAT = "F6.3" UNIT = "MICRON" END_OBJECT = COLUMN OBJECT = COLUMN COLUMN_NUMBER = 2 NAME = "FLUX" START_BYTE = 8 BYTES = 5 DATA_TYPE = "ASCII_REAL" FORMAT = "F5.2" UNIT = "WATT/CM^2/MICRON" SCALING_FACTOR = 1.0E-17 END_OBJECT = COLUMN OBJECT = COLUMN COLUMN_NUMBER = 3 NAME = "ERROR" START_BYTE = 14 BYTES = 4 DATA_TYPE = "ASCII_REAL" FORMAT = "F4.2" UNIT = "WATT/CM^2/MICRON" SCALING_FACTOR = 1.0E-17 DESCRIPTION = "1-sigma error in the preceding flux" END_OBJECT = COLUMN END_OBJECT = TABLE END