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ЙрhдлFile Format" leюhелNaming Conventions# №`жл hлFaint Object Camera$ hзл Input Files% &hил# Calibrated Data Files& Lin4hйл2 Processing Steps and Reference Files' Bhкл- ASCII files of Group Parameters( aPhллX-! SCIENCE DATA HEADER) o^hмлTa UNIQUE DATA HEADER* lhнл) STANDARD HEADER DATA HEADER+ z`ол ИhЩлFaint Object Spectrograph, Цhпл Input Files- дh░л + Output Files from Calibration. erf▓h▒лnt@ Processing Steps, Reference Files and Reference/ └h▓лб! SCIENCE DATA HEADER0 ╬h│лPr IMAGE DATA HEADER1 ▄h┤лEd! SCIENCE HEADER LINE2 ъh╡л F" SCIENCE TRAILER LINE3 °h╢л# UNIQUE DATA HEADER4 h╖л) STANDARD HEADER DATA HEADER5 `╕л "hл!High Resolution Spectrograph6 0h╣лй Input Files7 t>h║лFi+ Output Files from Calibration8 filLh╗лte@ Processing Steps, Reference Files and Reference9 Zh╝л ! SCIENCE DATA HEADER: hh╜л UNIQUE DATA HEADER; vh╛ло) STANDARD HEADER DATA HEADER< SД`┐л dП┘РР HH╘ИР┌ПraHH╘ИОТ■ -eshлncHigh Speed Photometer= h└лб Input Files> D$h┴л# Calibrated Data Files? 12h┬л┤! SCIENCE DATA HEADER@ @h├л╡ UNIQUE DATA HEADERA ENh─л╢) STANDARD HEADER DATA HEADERB \`┼л▌ jhл D Wide Field Planetary CameraC xh╞л Input FilesD rЖh╟л+ Output Files from CalibrationE Фh╚л 2 Processing Steps and Reference FilesF вh╔л & Data Quality File ValuesG ░h╩л! SCIENCE DATA HEADERH D╛h╦л# EXTRACTED DATA HEADERI A H╠h╠л) STANDARD HEADER DATA HEADERJ ┌`═л шhлFine Guidance SensorsK UT UTккh╬гIntroductionL ■`╧еra Purpose ( ■ ╨еТZThis Interface Control Document (ICD) provides a definition of the science data interface 4 ■╨еTbetween the Post Observation Data Processing System (PODPS) and the Space Telescope @ ■@╨еA 0Science Data Analysis Software (STSDAS) system. DAX ■`╤еScope h─g ■ ╥еND]This ICD defines and controls the data format of all science files which are produced by the Cs ■╥еPRoutine Science Data Processing system at the Space Telescope Science Institute s ■@╥еEV(ST~ScI). This explicitly includes the contents of the standard science data headers. ЩUR UTккh╙г DProcessing OverviewM и № ╘еVSome understanding of the variety of data which are available to the scientist can be ┤ №@╘еLgleaned from an overview of the processing which takes place at the ST~ScI. ┬ № ╒еFiUThe PODPS system is the portion of the Science Operations Ground System (SOGS) which u╬ №╒еVis responsible for the automatic processing of science and engineering data generated ┌ №╒еUduring an observing session. The PODPS system provides the software to automatically ц №╒еYmanage the receipt, editing, calibration, and archiving of data from the Space Telescope Є №╒е╥X(ST). In addition, PODPS generates certain types of output products from the calibrated d ■ №╒еPdata. The Routine Science Data Processing (RSDP) portion of PODPS performs this st №@╒еautomatic processing. № ╓еes\RSDP controls the routine processing of the data obtained as a result of the execution of a M$ №╓е╘\proposal by the ST. A specification of the data that is expected is supplied by the Science №0 №╓еglWPlanning and Scheduling System (SPSS) for use by RSDP. This is in the form of a subset ╒< №╓еstNof the final Science Mission Schedule (SMS) as reflected in the SPSS proposal H №╓еesYmanagement database. Additionally, SPSS places predicted and definitive Orbit data state T №╓еn Nvectors into the data base management system (DBMS) where RSDP can access it. ` №╓еmaOAdditionally, the Observation Support System (OSS) supplies RSDP with observer scol №╓е╒Vcomments and updates to the final Science Mission Schedule. These updates are used in x №╓еTPODPS to determine if any of the flags and indicators which affect the selection of hidС┘c ТТHH╘ИТ┌Сe HH╘ИРФ■t / e╓е №[calibration reference files and parameters to be used for RSDP calibration have changed as d b@╓е №#a result of real time interaction. lin" ╫еr WBy the time Science Instrument (SI) Science data are received from the ST Data Capture e M.╫еMSXFacility (DCF), RSDP has prepared itself to process the data which will actually arrive y,:╫еctVinstead of the data which was postulated to arrive. The RSDP Data Processing function F╫еMSZedits the SI Science data to insert fill data to take the place of any missing data, then R╫еRS^evaluates the data for acceptable quality. During this data evaluation phase the Data Quality ^@╫еs Ifiles describing the validity of each item of science data are produced. dl ╪еafZOnce the SI Science data is accepted, the Data Processing function converts the data to a x╪еQgeneric format. The RSDP Calibration function then processes it using a standard aД╪еe Xinstrument-specific calibration algorithm. It is important to note that the calibration №Р╪е tWroutines are exactly the same as those provided in the STSDAS environment available to a aЬ@╪еhethe scientists at the ST~ScI. ╡UT UTккh┘г (%Generic Edited Information SetsN s─ ■ ┌еil[For any observation the product of the ST~ScI╒s pipeline is not a single data file, but an Th╨ ■┌еsi]entire set of files called the Generic Edited Information Set (GEIS). At a minimum, for each c▄ ■┌еatZobservation, the RSDP produces a Standard Header Packet file, a Science Data file and its ш ■┌е[corresponding Data Quality file. Engineering data and ancillary information is produced in areЇ ■┌еXthe Unique Data log file for each instrument except for the wide field/planetary camera th ■┌еV(WF/PC). For that instrument, however, a similar ╘Extracted Engineering Data file╒ is ■@┌е produced. $ ■`█еcaStandard Header Packet i3 ■ ▄еhaLMost data in the Standard Header Packet (SHP) are common across the various se? ■▄еTS\instruments, although certain data in the SHP are specific only to certain instruments. The ккK ■▄еEdUSHP contains telemetry data for engineering data as well as data used for spacecraft eW ■▄е iWoperation. The telemetry values include information such as temperature, currents, and Genc ■▄еatUvoltages at various parts of the instrument. The spacecraft operation values include do ■▄еadZinformation such as target name, position and velocity of the telescope, and positions of { ■▄е dXreference objects such as the sun and moon. Instrument-specific information may also be fiЗ ■@▄еmeMrecorded in the SHP, and is described in the individual instrument sections. FЯ ■`▌е, Unique Data Log ╘о ■ ▐еinXThe Unique Data log (UDL) files contain the command values for each instrument, such as et║ ■▐е▄Yexposure parameters, aperture commands, etc. Each instrument╒s UDL file can also contain ╞ ■▐еru\observation-specific data. The contents, structure, and size of UDL files are different for ╥ ■▐еcoVeach of the different instruments, and are described in more detail in the individual ▐ ■▐еatVinstrument sections. The WF/PC has an ╘╘extracted data╒╒ file which contains similiar ъ ■@▐еvo!observation specific parameters. r ■`▀еafScience Data Files lu ■ ре▄[Every instrument pipeline calibration produces a Science Data file containing the observed of ■ре d]image stored as a GEIS file. Usually data are represented as single-precision floating-point ■) ■реreVvalues, however the WF/PC images are usually represented as short integer values. The 5 ■реat^number of Science Data files, the size of these files, and the number of dimensions will vary A ■ре aYacross the instruments and across observing modes of an instrument; these variations are LM ■@реta@described in more detail in the individual instrument sections. se ■`се oData Quality Files ent ■ теZEvery Science Data file has an accompanying Data Quality file to identify bad data values А ■те▐^in the science data. Data Quality files have the same size and dimensions as their associated dУ┘ifФФHH╘ИФ┌УluHH╘ИТЦ■el/liте SZScience Data files. Good pixel values are always marked with a zero value. The Input Data теe YQuality files use the value 1 to denote a Reed-Solomon data-check error and the value 16 F теalZto denote a DCF or PODPS fill. The Output Data Quality files vary across the instruments; ,@теesTthe variations are described in more detail in the individual instruments sections. umEUT UTккhугse!Wide Field Planetary CameraO T ■ фе ■ZDuring PODPS pipeline calibration, several GEIS format data sets are created for the Wide ` ■фе QVField Planetary Camera (WF/PC). They are: the Standard Header Packet, a Science Image l ■феntVfile, and Science Image Data Quality file, an Extracted Engineering Data file, and an x ■феim]Extracted Engineering Data Quality file. Each data file consists of an ASCII header file and Д ■фе^a binary data file. All files from a given observation have the same root file name; the type Р ■@феalWof information contained in each file is distinquished by its extension (see Table 1). es Ю ■ хе dLCALWFP provides routine calibration in both SOGS/PODPS Routine Science Data toк ■хеODJProcessing (RSDP) and IRAF/STSDAS. CALWFP performs a standard sequence of ╢ ■хеvaXprocessing steps on individual WF/PC camera observations designed to remove most of the кк┬ ■хеldUknown instrumental signature. CALWFP does the AtoD fixup, determines and removes the l╬ ■хеse\global bias level, subtracts bias, preflash, dark, and superpurge frames (after appropriate e ┌ ■хеck[scaling), and applies the flat field frame. The Calibrated Science Image Data Quality file cteц ■хе f[flags all pixels flagged in the Science Image Data Quality file and all pixels found to be sisЄ ■хеde[saturated, to have known bad pixels (static mask), and to have been flagged in the DQFs of th■ ■хеamZany of the calibration reference files used in the processing sequence. Histograms of the ■хе T^input data, the data following AtoD correction, and the calibrated output data are generated. ■хе ■YOperation of this program is accomplished via keywords in the header of the input image. " ■@хеva3The output images of CALWFP are listed in Table~2. tio0 ■ цеovZThis task is specific to WF/PC data and requires a large number of keywords obtained from < ■це rWthe WF/PC Science Image Header. The Science Image File and its associated Data Quality supH ■цеteVFile are always required, the Extracted Engineering Data File and its associated Data T ■@цеmaLQuality File are required if the bias level subtraction option is selected. ScnUR UTкк`чгuaInput Files alЖ №`шеbeStandard Header Packet saХ № щеno\The SHP contains telemetry values and spacecraft operation data. This file is not currently anб №ще▌Wused by CALWFP but is part of the standard WF/PC dataset. The SHP files are identified ^inн №@ще f)by the extensions ╘╘.SHH╒╒ and ╘╘.SHD╒╒. d┼ №`ъеenScience Image File х╘ № ые tTThe Science Image file contains the WF/PC image data with the readout from each CCD р №ыеutSdetector in each group. Hence from 1 to 4 groups may be present. The header should ic ь №ыеreWconform to the standard WF/PC header format. Keywords in the header are used to select mag° №ыеnc\the various processing steps and to specify the names of the necessary reference files. The , №ыеneTScience Image file must be an unmodified short integer WF/PC image for the ATODCORR d №ыеsuWand DOSATMAP (see below) steps to be meaningful. Science Image files are identified by St №@ыеet&the extensions ╘╘.D0H╒╒ and ╘╘.D0D╒╒. 4 №`ьеs Science Data Quality File . TC № эеrrUThe Science Data Quality file (DQF) must consist of short integers and have the same O №эеidTdimensions and number of groups as the Science Image file. Each pixel indicates the [ №эеImZquality of the corresponding pixel in the Science Image file. Zero valued pixels indicate g №эеacZ╘╘good╒╒ pixels in the Science Image file and nonzero valued pixels flag various problems s №эеldTor potential problems with their corresponding pixels (see below). The Science Data h №@эеseDQuality file is identified by the extensions ╘╘.Q0H╒╒ and ╘╘.Q0D╒╒. ifdХ┘enЦЦHH╘ИЦ┌ХusHH╘ИФШ■ge,he`юе!Extracted Engineering Data File o яеniXThe Extracted Engineering Data (EED) file contains the two ╘╘engineering╒╒ columns and, H╒#яе №Vfor FULL mode, the 12 columns of overclocked pixels. It has the same number of groups /яеmuXas the Science Image file. It is required when the BLEVCORR option is selected. 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