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LineH║╘Ж┌ЕЙАRЗИDouble LineQ╘З▌ИЖ╘╘И▌ЗЖ╘HЖ╘ Й┌ЖЛАRККSingle LineQ╘К▌Й╘RHZ┤Л┌ЙМАQ TableFootnoteE╕╛GX-RЯb^иМ┌ЛАQE╕╛PoE╕╛Poй┌ TableFootnotedН┘ООHH╘ИО┌Н┘HH╘ИС■,K║`Щб #UT UTкк`ЬгKeyword Definitions ∙v=UR UTккhЭгABSHFILE L № ЮеSi]Absolute Sensitivity Files (ABS): The absolute sensitivity scale files contain data that are X №Юе\used to perform HRS absolute flux calibration. These files are used in conjunction with the d №ЮеZHRS wavelength net files that specify the wavelength net (grid) used for interpolation of p №Юе^absolute sensitivity scale values. Absolute sensitivity files contain two groups of data that | №ЮеWcorrespond to the large and small apertures of the HRS. Because the HRS wavelength net И №Юе]files contain the wavelength net corresponding to these sensitivity values it is not assumed FФ №ЮеЯb^that the spacing between wavelength values is uniform. Data in the absolute sensitivity files а №@Юеare stored in REAL*4 format. ║UP UTккhЯгACCPDATE ╔ ·`ае$proposal acceptance date (yyyyddd): UTуUN UTккhбгorADC_CORR! Є ° веZapplication of dispersion constants: Convert the sample positions on the photocathode to ■ °веonUwavelengths by applying the dispersion constants using tables ccr5, ccr6, and ccr7 . °веUcontaining spectral order, dispersion, and thermal constants. This routine computes °ве (`spectral orders and wavelengths. For first order gratings, the spectral order is set to 1. For se" °@веntLechelle gratings the spectral order is computed by the following formula: sm0 °`глhe&order = NINT( numerator/ denominator) > °`дл"numerator = b*A*sin((C-carpos)/B) L °`елes+denominator = ydef-a-d*A(sin((C-carpos)/B) Z °`жл tWhere: bh °`злvaNINT is the nearest integer, sv °`илfiA,B,C are in table ccr5, rД °`йл fa,b,d are in table ccr5, Т °`кл ·&carpos is the carrousel position, and а ° ллUN1ydef is the Y-deflection adjusted for the proper м °@ллis aperture s║ ° млe 2And: The wavelengths are computed by solving the ╞ °млth3dispersion relation for wavelength using Newton╒s ccr╥ °мл.8iterative method. The dispersion relation is described n,▐ °@млanby the following equation: °ь °`нлsp3s = a0 + (a1*m*w) + (a2*m*m*w) + (a3*m) + (a4*w) + ngs· °`олer(a5*m*m*2) + (a6*m*w*w) °`плllWhere: t °`░л im is the spectral order, $ °`▒лw is the wavelength, I2 °`▓лom.a0,a1,.. are the dispersion coefficients, and @ °`│л °s is the sample position. N °`┤л(((calguide) hUL UTккh╡г tAFFILIAT" w Ў ╢еNI^observer organization or affiliation: Obtained directly from the cover page of the proposal Г Ў@╢еleform: Т °dР┘rrСС °HH╘ИС┌РflHH╘ИОУ■*is`╖лGO = general observer, ave`╕лedAR = archival researcher, $`╣лon%IDT = investigation definition team, s2`║лм"IS = interdisciplinary scientist, @`╗лscSCI = ST Science staff, anN`╝л eESA = european space agency, p\`╜л) 2MOC = mission operation contractor. (qpersonnel) uUT UTккh╛г ( ALIASi # °Д ■ ┐еWhXsynonym for target name: (i=1..2) In addition to the catalog name, a target should be elР ■┐еZassigned at most two ╒common names╒, or aliases. These might include the Bayer (Greek-Ь ■┐еWletter) designation or Flamsteed number with the standard three-letter constellation ervи ■┐е aVabbreviation (eg, ZETA-CAP, 22VUL), the Bright Star Catalog number (eg, HR5270), or ┤ ■┐еLother names, if they exist (eg, CYG-X1, BARNARDS-STAR, PROXIMA-CEN). Star └ ■┐е[clusters, nebulae, galaxies, and clusters of galaxies should be assigned commonly used ╠ ■┐е aDnames (eg, HYADES, OMEGA-CEN, CRAB-NEBULA, ABELL63, COMA-CLUSTER) on╪ ■@┐еCor Messier numbers (eg, M13, M31, M67). (PROP_INST--SEC_5.TEX;1) = ЄUR UTккh└гanANGLESEP$ № ┴еan[target angular separation in arcsec. user input if qextpf=t. computed from target position UT №┴еSiZ(qtara2, qtadc2) and computed target position (qexcra, qexcdc) if qextpf=a. together with №┴еouXthe position angle this field specifies offset data from the referenced target position ht% №@┴е H(qtara2,qtadc2) in polar coordinates (1 x 10e-3 precision). [qexposure] t?UP UTккh┬гe-ANG_SIDE% N · ├еY(0.,360.) angle between sides of scan parallelogram clockwise angle, about the beginning ,Z ·├е┐]of the first scan, from the direction of the first scan to the side of the scan parallogram. f ·@├е, "(1x10e-04 precision). [qexposure] АUN UTккh─гe ANNPARRA& П ° ┼е\par. shift in position, non-solar sys target: the magnitude of the parallactic shift in the Ы °@┼еerEposition of the non-solar system target at the time of observation. кй °`╞л[qobservation.annparra] ta├UL UTккh╟гatAPERAREA' ╥ Ў ╚еf=`aperature area: Area of the aperture used, in square arc seconds. This keyword is filled by it▐ Ў@╚еc)Ccalibration software only when the target is an extended source. thi°UJ UTккh╔гofAPEROBJ ( Ї ╩еet_si object aperture id: SI object aperture and coordinate system id; specifies the aperture and xpo Ї╩екк\coordinate system of the instrument to be used for the observation of the target. It is the ra Ї╩е aZaperture id concatenated with the aperture coordinate system id. These ids are defined in + Ї@╩еofDST_ICD_26 part III. WFPC: W//[WF|PC]//aperture//summode, where: ex9 Ї`╦лкк aperture: ALL (for ALL or ANY); G Ї`╠лft4ND (for ALL-ND); U Ї`═лe 1,2,3,4; fc Ї`╬лhisummode: S (for mode= 2x2); erq Ї`╧л1WFLOOD: if mode=UVFLOOD;[qobservation.coord_id] кdТ┘n.УУккHH╘ИУ┌ТHH╘ИСХ■er'se UT UTккh╨гecAPEROFFX) ■ ╤еit^x component of offset of object in aperture (arcsec): X component of the offset of the target $ ■╤еAP^from the center of the aperture. If coord_typ = SIAS, then units are pixels; if coord_typ = 0 ■@╤еe "SICS, then units are arc-seconds. JUR UTккh╥гm APEROFFY* Y № ╙еhe^y component of offset of object in aperture (arcsec): Y component of the offset of the target e №╙еe ]from the center of the aperture. If coord_typ = SIAS, then units are lines; if coord_typ = Cq №@╙еde"SICS, then units are arc-seconds. ЛUP UTккh╘гLLAPERSKY + Ъ · ╒е4NYsi sky aperture id: SI sky aperture and coordinate system id: specifies the aperture and ж ·╒еYcoordinate system of the instrument to be used for the sky background light observations ▓ ·╒е_in conjunction with the observation of the target. It is the aperture id concatenated with the UT╛ ·@╒еAPLaperture coordinate system id. These ids are defined in ST_ICD_26 part III. (a╪UN UTккh╓гt APERTOBJ, ч °`╫еaperture in use - object data: theUL UTккh╪гd_APERTSKY- Ў`┘е aperture in use - sky data: ╤*UJ UTккh┌гniAPERTURE. 9 Ї`█е╥)name of the aperture used for this file: SUH UTккh▄гt APERTURE/ b Є`▌еcoaperture name: fse|UF UTккh▐г №APERTYPE0 Л Ё`▀еof:SIDS/SIAS/SICS ... aperture coordinate system type where Щ Ё`рл №7SIDS = si detector system, a coordinate system derived UTз Ё слSK4from si readouts in the science or engineering data ky│ Ё@слdistream; m ┴ Ё тлap8SIAS = si aperture system, a coordinate system based on i═ Ё@тлedthe he█ Ё`улghaperture or fov of the si; ╒щ Ё флon9SICS = si corrected system which in general differs from cї Ё@флhethe · Ё`хлap2sias by removal of distortions and scale changes. Ё`цлII[qexposure.coord_type] AP+UD UTккhчг APER_k 1 p: ю`шеje(TYPE=C*15 instrument aperture: (k=1..4) TUB UTккhщг┘APER_ID 2 c ь`ъе╤The entrance aperture id: Eq ь`ыл█ A-14.3 o ь`ьлd A-20.5-PAIR dФ┘ ХХapHH╘ИХ┌Ф №HH╘ИУЧ■/S&CS`элdiA-30.25-PAIR whe`юлрA-40.1-PAIR $`ял c B-10.5 y2`Ёл Ё B-20.3 с@`ёлou B-31.0 cN`ЄлngB-4 \`єлdiC-11.0-PAIR j`ЇлSIC-20.25x2.0 x`їл C-32.0-BAR oЖ`ЎлтC-40.7x2.0-BAR Ф`ўлtuERRerror(tguide 7.0-11) нUT UTккh°г =APER_POS3 ╝ ■`∙еraaperture used: ї Ё╓UR UTккh·гthARGPERIG4 х №`√еre*argument of perigee (revolutions/second): UP UTккh№г[qASA_FILE5 ·`¤еккarea scan analog is present: (UN UTккh■г=CASD_FILE6 7 °` еarea scan digital is present: QUL UTккhгъASK_FILE7 ` Ў`еanalog sky science is present: ьzUJ UTккhгA-AST_FILE8 Й Ї`е analog star science is present: apгUH UTккhг┌ATODCORR9 ▓ Є еTDo A-to-D correction: YES, NO, DONE: Replace each pixel with the appropriate value ю╛ ЄеR Yfrom the AtoD correction lookup table. The name of the lookup table must be provided in 1╩ ЄеЄRthe keyword ATODFILE. The AtoD table may consist of multiple lookup tables. The ╓ ЄеZlookup table whose temperature is closest to the value of the input science image header т Є@еUT)keyword WBA3PCTM is selected. (calguide) №UF UTккhг uATODFILE: Ё еERXA-to-D Lookup Tables Files (A2D): The A-to-D lookup table files are used to correct the [q Ёе ·\image data for a pattern introduced by the Analog to Digital converter electronics. This is # Ёеn Wdone by replacing the short integer pixel values obtained from the WF/PC with floating sci/ Ё@е ьYpoint values that remove the systematic degradation introduced by this hardware problem. pIUD UTккhг┌ATODSAT ; X ю` е+number of "AtoD saturated" pixels (DQF=8): ce rUB UTккh гe BACCORR < Б ь еYbackground subtraction correction: Subtract dark-count images. The dark-count reference dЦ┘woЧЧtaHH╘ИЧ┌Ц HH╘ИХЩ■=*seеosafile multiplied by the exposure time is subtracted from the input science file. The dark-count tеUF`file is a full-frame image (512 x 1024 or 1024 x 1024), so if the science file is smaller than l @еarUfull frame, only the appropriate section of the dark-count file is used. (calguide) e9UT UTккhг cBACHFILE= H ■ е ЁXBackground (Dark Count) Files (BAC): The background files contain data used to subtract wT ■ е ЁZdark count from FOC science images. It is used for the background calibration. Background ` ■ еUD[data files contain one group of data. Every background data file has the same format as an 8):l ■ е Vimage. It is either a 1024 sample by 1024 line image for use with normal pixel format x ■ еThWimages, or a 512 sample by 1024 line image for use with zoom pixel format images. Each HД ■ еZpixel in the background data file is a single-precision real (REAL*4) count rate value in Р ■@ еsucounts per second. frкUR UTккhгceBACHFILE> ╣ № еVBackground Files (BAC): FOS background reference files contain the default background ┼ №е lUdata used during background subtraction (spectroscopy ground software mode) for both i╤ №@е eobject and sky spectra. FIыUP UTккhгBAC_CORR? · · еFiRbackground subtraction: Subtract the background from sky and object spectra. The ·еFObobserved background is first repaired; bad points (i.e., points at which the data is flagges as ·еro^lost or garbled in the telemetry process) are filled by linearly interpolating between "good ·е24[neighbors". Next, the background is smoothed with a median, followed by two iterations of a 5* ·еli`a mean filter before subtraction. Filter widths are contained in table ccs3. If no background un6 ·е[was taken, a default reference background, bachfile, is used. No smoothing is done to the кURB ·@еBA_reference file background, if used. This is a spectroscopy mode calibration step. (calguide) the\UN UTккhгd BADPIXEL@ k °`еri)number of "generic bad" pixels (DQF=32): uЕUL UTккhгfoBCK_CORRA Ф Ў еctUbackground removal: Subtract the background counts from the raw counts of the diode dа Ўеtr\array. This routine subtracts the background by one of four methods. The first applicable iм ЎеbaZmethod is used. (1) Subtract sky spectra (header keyword BINID of 5 or 6). For this case ╕ Ўе pWthe background is smoothed by a median filter followed by a mean filter. (2) Subtract rs"─ ЎеroYinterorder from main diode array. (header keyword BINID of 3 or 4). For this case, the a╨ ЎеbtYbackground is smoothed by a median filter followed by a mean filter. (3) Use background ▄ ЎеauWdiodes from separate substep bins with header keyword BINID between 8 through 15. The @ш Ўеle^diodes to use are selected on the basis of the value of BINID. (4) Use all background diodes Ї Ў@е2from the same bins as gross spectrum. (calguide) UJ UTккhгULBDEXPFLGB Ї`е Ўbus director expander flag: em7UH UTккhгe BIASCORRC F Є еntZDo bias correction: YES, NO, DONE: Subtract the bias image reference file from the input R Єеe Zscience image. The names of the bias image and its DQF must be provided in the keywords ^ Є@е o"BIASFILE and BIASDFIL. (calguide) xUF UTккhгndBIASEVEND dШ┘n ЩЩs"HH╘ИЩ┌ШfrHH╘ИЧЫ■ o( 4 еtBTYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI UNITS= Bias level from EED е fXextended register Information garnered from columns 3-14 of the extracted engineering ea е bY(.x0h) file. Note that the BIASEVEN value should be the mean of columns 3,5,7,9..., and o,еIDSthe BIASODD value should be the mean of columns 4,6,8,10,...---i.e., the overscan ect8@еUJJcolumns are 180 degrees out of phase from the science image. (opr.21796) QUT UTккhгккBIASFILEE ` ■ еZBias Files (BAS): The structure in the electronic bias is removed by subtracting the bias l ■е]reference file (with its accompanying data quality file). The most notable component of this ox ■еTstructure is a 0.6 DN even/odd column pattern. The BIASDFIL is the name of the bias Д ■@е#frame reference data quality file. ╘ЮUR UTккhгBINID F н №`еЫbinid: o╟UP UTккh г BINIDi G R╓ ·`!еFIbin id of substep i where: fф ·`"л 0 = no data, dЄ ·`#л1 = star small aperture, 3 ·`$лed2 = star large aperture, ·`%лil3 = upper interorder, ·`&лth4 = lower interorder, * ·`'л5 = sky small aperture, va8 ·`(лme6 = sky large aperture, .-F ·`)лan 7 = dark cur `UN UTккh*гar BITPIX H uo °`+еhebits per data value: 7ЙUL UTккh,гBLEVCORRI Ш Ў -еXDo bias level correction: YES, NO, DONE: Determine the global bias level from the mean bд Ў-е_of the extended register pixels in the extracted engineering data file (.x0h) and subtracted s o░ Ў-еVfrom each pixel in the input science image. Only pixels not flagged in the extracted ╝ Ў-еXengineering DQF (.q1h) are included in the averaging. The names of these files must be ╚ Ў@-еUPл3i = internal, ╟ °`?лFie = external. ╒ °`@лitset if qextyp_type = cal. O Ёу °`Aлpr[qexposure.calibr_typ] e e¤UL UTккhBг p CAMERA R Ў CеpuXcamera in use: WF (wide-field), PC (planetary): This indicates which of the two cameras un ЎCеn Qwas used to obtain the scientific data. The possible values are ╒WIDE-FIELD╒ and T$ Ў@CеHT ╒PLANETARY╒.[qexposure.camera] >UJ UTккhDгЫCAMMODE S M Ї EеRcoronographic apodizer mask: INBEAM, NOTUSED: In the FOC/288 configuration, the Y ЇEеfoVOCC Mode uses the f/96 camera with the compact Cassegrain assembly and an apodizing e ЇEеURZmask. The 0.4-arcsec occulting finger is used to produce a Lyot-type coronagraph. The q ЇEеUTS0.8-arcsec occulting finger is not available in this Operating Mode. (PROP_INST--h<} Ї@Eе SEC_8_2.TEX) =ЧUH UTккhFгra CARPOS T ж Є`Gе>carrousel position: °└UF UTккhHгe CCG2 U ╒ °╧ Ё IеseYpaired pulse correction: Paired-pulse correction table. Deadtime constants are used to B█ ЁIе ]correct for the non-linear channel response of each diode. These constants are not expected hч ЁIе Ў]to change during the lifetime of the FOS. Analysis of prelaunch data indicate that the same aє Ё@IеC:constants can be used for both FOS detectors. (calguide) UD UTккhJг ЇCCP0 V е ю KеodVAperture Areas Relation: A CDBS table containing the names and areas of all the HSP╒s ( юKе96Xapertures and are used by the HSP calibration. Each entry contains an aperture name and . 4 юKеcc[an aperture area, which is used to convert HSP count rates into count rates per square arc-sec@ юKе=Xsecond. This information is loaded only from the Project Data Base Tape. See ICD-47 for =L ю@Kеrafurther information. fUB UTккhLгouCCP1 W °u ь Mеe WHigh Voltage Factor Relation: A CDBS table containing the coefficients and base values ablБ ьMеnt]used in computing the high voltage detector characteristic for the HSP calibration. Each set .dЬ┘ hЭЭtoHH╘ИЭ┌Ь FHH╘ИЫЯ■ha,saMеIVof base values and coefficients corresponds to a particular HSP detector high voltage Mе^setting (command value), and data type. In each set there are a base value, a reference time, @MеK>a reference temperature, and sixteen polynomial coefficients. 9UT UTккhNгreCCP2 X 4 юH ■ OеanWGain Factor Relation: A CDBS table containing the coefficients and base values used in secT ■Oе=\computing the gain detector characteristic for HSP calibration. Each set of base values and ю` ■OеfuZcoefficients corresponds to a particular HSP detector and a gain setting (command value). l ■OеCD[In each set there are a base value, a reference time, a reference temperature, and sixteen ng x ■@Oеetpolynomial coefficients. eТUR UTккhPгEaCCP3 Y б № QеSPre Amp Relation: A CDBS table containing the coefficients and base values used in н №QеYcomputing the pre-amplifier detector characteristic for the HSP calibration. The PRE AMP a╣ №Qеh adetector characteristic is the contribution to the digital count rate or analog current from the v┼ №QеtiVelectronics. Each set of base values and coefficients corresponds to a particular HSP ╤ №QеreZdetector and data type. In each set there are a base value, a reference time, a reference ▌ №@Qеva2temperature, and sixteen polynomial coefficients. ўUP UTккhRгacCCP4 Z HSP · Sе sVEfficiency Relation: A CDBS table containing the coefficients and base values used in ·SеgaTcomputing the efficiency (relative sensitivity) detector characteristic for the HSP a ·SеreVcalibration. Each set of base values and coefficients corresponds to a particular HSP * ·SеCC_aperture and detector. In each set there are point and extended base values, a reference time, bas6 ·@Sе>a reference temperature, and sixteen polynomial coefficients. PUN UTккhTгHSCCP5 [ . T_ ° UеVDark Count Relation: A CDBS table containing the coefficients and base values used in k °Uе t]computing the dark count characteristic for the HSP calibration. Each set of base values and aw °Uе №Scoefficients corresponds to a particular HSP dark aperture, a high voltage setting encГ °Uеe X(command value), and data type. In each set there are a base value, a reference time, a acП °@Uе · UTккh╩г tDATA_FMTО w ш`╦еhe*data format: byte, word, lwrd, alog, all: dи┘Oйй!raHH╘Ий┌иisHH╘Изл■ty# ° UT UTккh╠гfiDATA_SRCП ■`═е#data source: star, sky, area scan: ode2UR UTккh╬г cDATA_TYPР A №`╧еtsdata type: digital, analog: Ў[UP UTккh╨гthDATE С soj ·`╤еUJ'date this file was written (dd/mm/yy): ДUN UTккh╥гe DATE-OBSТ У ° ╙еDAaUT date of start of observation (dd/mm/yy): Note that this is not necessarily the start of the AЯ °╙еYexposure. For example, the WFPC observation starts on a major frame pulse, while the л °@╙е vVexposure actually starts 16.4 seconds later following a memory erase. See EXPSTART. ┼UL UTккh╘г tDCFOBSN У ╘ Ў`╒еDADCF observation number in SHP: daюUJ UTккh╓гy:DDTHFILEФ ¤ Ї ╫е\Disabled Diode Files (DDT): The disabled diode files contain a disabled diode table for use Ї@╫ейPin the standard case reduction when the Unique Data Log (UDL) is not available. #UH UTккh╪гUTDEADTIMEХ 2 Є`┘е ■3accumulator close time (units of 7.8125 microsec): odeLUF UTккh┌г cDEADTIMEЦ [ Ё █еtsaCorrect dead time. This switch applies only to digital data; if the data is analog, this switch g Ё@█еddJhas no effect. The following equation is used to correct for dead time: u Ё`▄лrvx = y/(1-y*t) Г Ё`▌л iWhere: ssС Ё`▐л tx is the true count rate, Я Ё`▀лpl"y is the observed count rate, and н Ё`рлe,t is the dead time. (calguide) Vex╟UD UTккhсгar DEADTM Ч ╓ ю теa _deadtime: Deadtime used in calculating pair-pulse correction for digital data, in seconds. tioт ю@теda[This keyword is filled by the calibration software only for digital data files. (calhsp) abl№UB UTккhугtaDEA_TEMPШ ь`фе(DEA temperature of the object detector: r%U@ UTккhхгUnDECAPER1Щ 4 ъ`цеle#declination of the aperture (deg): NU> UTккhчг ■DECAPER1Ъ ] ш`ше 7#declination of the aperture (deg): г cwU< UTккhщг ЁDEC_APERЫ dк┘ppлл"atHH╘Ил┌кitHH╘Ийн■he#wi`ъеed#declination of the aperture (deg): !UT UTккhыг-yDEC_APERЬ 0 ■`ьеss#declination of the aperture (deg): ounJUR UTккhэгDEC_APERЭ Y №`юеra#declination of the aperture (deg): e dsUP UTккhягe)DEC_MOONЮ В ·`ЁеЧ8declination of moon in geocentric J2000.0 coordinates. cuР ·`ёлco[qobservation.declmoon] кUN UTккhЄг юDEC_REF Я ╣ ° єеfiOdeclination of the reference target position. This is in heliocentric J2000.0. UT┼ °@єеTE[qobservation.ref_obj_dec] (DE▀UL UTккhЇгheDEC_SUN а ю Ў`їех7declination of sun in geocentric J2000.0 coordinates. the№ Ў`Ўл [qobservation.declsun] APEUJ UTккhўгDEC_TARGб % Ї °еurWDeclination of the target. The epoch and equinox of the target position is J2000. For 1 Ї°еUmoving target, the epoch of the target position is the predicted start time for the = Ї@°еdeHobservation. (Fixed - Heliocentric J2000, moving - Geocentric J2000.) ■K Ї`∙лde[qobservation.dec_target] eUH UTккh·гкк DEC_V1 в Pt Є √е\declination of v1 axis of space telescope in geocentric J2000.0 coordinates. The v1 axis is А Є√еioYthe optical axis of the space telescope (more or less the ╒roll╒ axis). The epoch of the nМ Є@√еЄUposition of the v1-axis is the predicted start of observation.[qobsevation.declnv1] жUF UTккh№гntDEFAULTSг ╡ Ё`¤еTE0default values used in reformatting these data: he╧UD UTккh■г ЎDEFDDTBLд ▐ ю` еunUDL disabled diode table used: s. °UB UTккhгЎDELAY е at ь`еUJ2delay between integrations (in 1/1.024 microsec): !U@ UTккhгhe DELTAS ж o0 ъ`еthdelta sample position: 00.JU> UTккhгDELTA_X з Y ш`е o(x increment for map (deflection units): arsU< UTккhг ЇDELTA_Y и В ц`еix(y increment for map (deflection units): icdм┘[qнн#] HH╘Ин┌м PHH╘Илп■is)ac UT UTккhгceDETECTOBй ■ еax]detector in use (0-5) - object data: This holds the number of the detector that was used for a$ ■ е tZdata from the object during this observation. It is one of the five image dissector tubes 0 ■ е Y(numbered from 1 to 5), including the two CsTe photocathodes, the two bialkali cathodes, n< ■@ еUDand the photomultiplier tube. ▐ юJ ■` лUD0:none dX ■`л. 1:POL ккf ■`ле2:UV1 t ■` лy 3:VIS nteВ ■`л244:UV2 ): Р ■`лhe5:PMT[qexposure.detectob] кUR UTккhг pDETECTORк ╣ № еDEXFOS: detector in use: amber, blue HRS: detector in use (1-2): WFPC: the ccd number of ┼ №@е the data ▀UP UTккhгenDETECTSKл ю · е_detector in use (0-5) - sky data: This holds the number of the possible detector that was used H· ·е[for data from the sky (or background) during this observation. It is one of the five image us ·еatVdissector tubes (numbered from 1 to 5), including the two CsTe photocathodes, the two ·еinZbialkali cathodes, and the photomultiplier tube. When MODE is SCP or ARS, this field will ·@еin2contain the null value (-1).[qexposure.detectsk] 8UN UTккhгDET_CHR м G ° еie[retrieve detector characteristics: Retrieve detector characteristics. This keyword is not леS °@еRcurrently used, and it is not updated to COMPLETE by the calibration. (calguide) mUL UTккhгobDET_TEMPн | Ў еSdetector temperature of the object detector: Determined from the telemetered items ): И Ў@еmbгstDQIHFILE╝ Ъ · ?е t]Data Quality Initialization Files (QIN): The HRS data quality initialization files contain a uж ·?еUF\priori information concerning the effect of the HRS╒s diode arrays on the quality of output E:▓ ·?еgg\data values. Data quality initialization data files contain a single group of data with 512 nv╛ ·@?еh >entries corresponding to the 512 diodes of each HRS detector. ╪UN UTккh@гDQI_CORR╜ ч ° Aеedata quality initialization: Apply data quality initialization using the reference file, dqihfile. xє °Aеgu\This routine performs the data quality initialization by flagging each data value with the DQ °Aеavalues in the data quality initialization file. The file contains a data quality value for each l °Aе=cdiode. If the data quality value of the data is larger than the data qualify initialization file °@Aеut[value for the diode, it is left unchanged. Quality values are never decreased. (calguide) liz1UL UTккhBг TDSK_FILE╛ @ Ў`Cе f digital sky science is present: UFZUJ UTккhDгonDST_FILE┐ i Ї`Eеs !digital star science is present: uГUH UTккhFг?DWELL_LN└ Т Є Gеit]( 1-99) dwell points per line for scan pointing mode; set if this is a dwell scan, otherwise oЮ Є@Gе 5'equal to zero. [qexposure.dwells_line] кк╕UF UTккhHгDWELL_TM┴ ╟ Ё`Iеli???? iсUD UTккhJгda ECBDX3 ┬ iЁ ю`Kеe eccentricity cubed times 3: ° UB UTккhLгThECBDX4D3├ ь`Mеtyeccentricity cubed times 4/3: 3U@ UTккhNгthECCENTRY─ B ъ`Oеn 5Eccentricity of the orbit[wiephemeris.eccentricity] s\U> UTккhPгluECCENTX2┼ k ш`Qеdi?2 times the eccentricity of the orbit. [wiephemeris.two_x_ecc] ta d▓┘ °││&e HH╘И│┌▓d.HH╘И▒╡■gu)iz UT UTккhRг TECH_CORR╞ ■ Sе fbcorrection for echelle ripple: If one of the echelle gratings is used, divide the flux value by $ ■Sеpr\the normalized grating efficiency to remove the echelle ripple using tables ccr9 and ccra, e 0 ■Sеmo]which contain echelle ripple constants. This routine performs the echelle ripple removal by l< ■@SеUT>dividing the flux by the following echelle ripple function: J ■`TлX3ripple = gnorm sinc(a*x+b)^^2 X ■`UлimWhere: UBf ■`VлEC gnorm = cos(A+B+C)/cos(A+B-C+e) ect ■`Wлim.x = [pi]*m*cos(A+B+C)*sin(A+e/2)/sin(A+C+e/2) В ■`XлEcAnd: Р ■`Yлie e is arctan ( (samp-280.0)/f ), ккЮ ■`Zлm is the spectral order, м ■`[лci*samp is the photocathode sample position, ║ ■`\л┘!A is (r0 - carpos)*2*pi/65536.0, ╚ ■`]л6r0, B, C, f are grating parameters in table ccra, and ╓ ■`^лUT5a and b are coefficients from table ccr9. (calguide) oЁUR UTккh_гleEPCHTIME╟ № `еatWEpoch time of orbital parameters; given in the form of the number of seconds since 1/1/cie №@`еec85.[wiephemeris.epoch_time] %UP UTккhaгEPLONGPM╚ 4 · bеe Uplanetographic coordinate system parameters: epoch of longitude of prime meridian of S@ ·@bе f=planetary target. seconds from 1980.[qtargets.epo_prim_mer] TZUN UTккhcгrmEQNX_SUN╔ i °`dеimequinox of the sun: ГUL UTккheгcoEQRADTRG╩ Т Ў fеOTplanetographic coordinate system parameters: equatorial radius of planetary target. ■Ю Ў@fеe [qobservation.equ_radius] ╕UJ UTккhgгZEQUINOX ╦ ╟ Ї hе ■XTYPE=C*7 equinox of the celestial coordinate system: eyyyy.f ... specifies the epoch of -╙ Їhе6.^equinox of the input coordinate system for target position data e = j or b, yyyy = year, f is ▀ Ї@hеcoa fraction of yyyy. c∙UH UTккhiгUR ERRCNT ╠ e Є jе №[number of segments containing errors: Science data is divided for telemetry purposes into s s Єjе\lines and frames. A line is a maximum of 965 16-bit words of science data, and a frame is b ЄjеicQa collection of one or more lines. For transmission purposes, a line of data is , Єjеy Vaccommodated in a packet, which in turn is divided into from 1..16 segments (each of 8 Є@jеimwhich has 64 16-bit words.) TRUF UTккhkгDTERR_CORR═ a Ё lеet[propagated error computation: Compute the propagated error at each point in the spectrum. @fm Ёlеn.]The photon statistical errors in the original data are carried through the reductions. The ey Ёlе s^errors are scaled at each calibration step. Thus, the standard errors have the same units as d┤┘e ╡╡' fHH╘И╡┌┤onHH╘И│╖■╠( Є@lеnuTthe calibrated data. This step is a spectroscopy mode calibration step. (calguide) to!UT UTккhmгjESQDX5D2╬ 0 ■`nе a.Eccentricity of the orbit squared times 5/2. > ■`oл Є[wiephemeris.ecc_sqd_x_fh] n oXUR UTккhpгs.EXPACKET╧ g № qеe WThe expected number of source packets for an observation for the SI science instrument o fs №qе (_data. This value is used to determine whether data collected by data partitioning has all been a Ё №qеprYcollected. The estimate includes science data, unique definition log, and science header fЛ №@qеn. packets. Щ №`rлrs[qobservation.expected_pkt] ie│UP UTккhsгuc EXPEND ╨ Ё┬ · tеerNexposure end time (Modified Julian Date): WFPC: EXPEND = EXPSTART + EXPTIME ╬ ·@tеK(cgwcex) FOS: EXPEND = FPKTTME (1 readout), LPKTTIME (multiple readouts) ┤шUN UTккhuгEXPFLAG ╤ ў ° vеUExposure interruption indicator: NORMAL - EXPTIME was successfully calculated from a °vеdeUtelemetry information, is equal to the predicted exposure time, and the value of °vе JNSHUTA17 is less than or equal to 1. EXPFLAG is also set to NORMAL when °vеZEXPTIME was successfully calculated and the predicted exposure time was not available. ' °vеT INTERRUPTED - EXPTIME was successfully calculated from telemetry information, is ti3 °vеXequal to the predicted exposure time, and the value of NSHUTA17 is greater than 1. l? °vеadRINCOMPLETE - EXPTIME was successfully calculated from telemetry information and K °vеs[is not equal to the predicted exposure time. (Invariably the case in Rapid-Read mode FOS XPEW °vеPTKobservations. ETS-E) EXTENDED - EXPTIME was successfully calculated from IMEc °vеs)[telemetry information and is greater than the predicted exposure time. UNCERTAIN - The : o °vеwaTShutter Log Overflow flag (WWLOGOF) was set, which indicates that not all shutter l { °vеxpTopen/close times are available. EXPTIME was calculated from the shutter open/ close o З °vеsoNtimes that are available. INDETERMINATE - EXPTIME could not be successfully У °vеexWcalculated from the telemetry and the predicted exposure time was not available. ullЯ °vе RPREDICTED - EXPTIME could not be successfully calculated from the telemetry and л °@vеe 0EXPTIME was set to the predicted exposure time. v┼UL UTккhwг EEXPFLAG ╥ ╘ Ў`xе f!Exposure interruption indicator: °юUJ UTккhyгisEXPFLAG ╙ ¤ Ї`zеre!Exposure interruption indicator: pUH UTккh{гPEEXPFLAG ╘ & Є`|е. !Exposure interruption indicator: c@UF UTккh}гd EXPFLAG ╒ O Ё`~еme!Exposure interruption indicator: aiUD UTккhгpoEXPOSURE╓ x ю`Ае °exposure time (seconds): od╢┘ ╖╖(noHH╘И╖┌╢xpHH╘И╡╣■wa.ul UT UTккhБгteEXPOSURE╫ ■ ВеsoUexposure time per pixel (seconds): As opposed to the misleading EXPTIME which gives $ ■Веul\the total time the accumlation of photons took even though that time includes independent 0 ■@ВеD 4pixels (nxsteps) and the sum of all groups. (ETS-D) thJUR UTккhГг °EXPSTART╪ Y № ДеtoWexposure start time (Modified Julian Date): WFPC: Calculated as follows: EXPSTART = !Exe №Деn 9UTC0 + (CLKRATE * T) + (CLKDRFTR * T**2)/2 + DELAY T = q №Де iG(WEXPTMHI*2**16 + WEXPOTIM) - SPCLINCN where: SPCLINCL = spacecraft `|} №@ДеerLticks since UTC0 DELAY = 16.4 seconds if non-NSCC-1 controlled exposure ExЛ №`Елn 6(generally means, the NSCC-1 didn╒t have take over to Щ №`Жлsudeal with loss of PCS lock.) з №`Зл.= 16.5 seconds if NSCC-1 controlled exposure ╡ №`Ил7(rather than WFPC micro-processor controlled.) (ETS-f) кк├ №`Йл4FOS: EXPSTART = FPKTTIME - (EXPTIME + EXPDEADTM) on╤ №`Клo where: adi▀ № ЛлivEXPDEADTM= (DEADTIME*7.8125E-oы №Ллml)6)*INTS*[NXSTEPS*OVERSCAN*YSTEPS*SLICES] ў №Ллnt;*NPAT*NREAD*NMCLEARS NOTE: EXPSTART only gives the start gr №ЛлUR3time of the FIRST group of data in the final PODPS Wex №@Лл(Mproduct.(ETS-f) ))UP UTккhМгd EXPTIME ┘ 8 · НеQexposure duration (seconds)--calculated: WFPC: If the WFPC exposure was a DARK D ·НеI*MFRAME, the exposure time code in WEXPORTH is used to obtain EXPTIME from the ДP ·НеUTRWFPC Exposure Time Table. Otherwise, the exposure time code in WEXPOCMD is used \ ·Не, Vto obtain EXPTIME from that table. In addition, if the number of shutter closures h ·НеO(NSHUTA17) was greater than 1, the WFOCTIME values are used to calculate the n Wt ·@Неr -amount of time that the shutter was closed: OВ ·`ОлKT(EXPTIME = EXPTIME - shutter_closed_time Р · Плdi9When EXPFLAG is set to PREDICTED, EXPTIME was set to the Ь ·ПлNT9predicted exposure time. FOS: EXPTIME reflects the Nи ·Пл 2total accumulator open time (livetime): EXPTIME= ┤ ·@Плth5(LIVETIME*7.8125E-6)*INTS*[NXSTEPS*OVERSCAN*YSTEPS* ┬ ·`Рл(SLICES]*NPAT*NREAD*NMCLEARS EX╨ · Сл8Misleading exposure time: This gives the total time the FP▄ ·Слos4accumlation of photons took even though that time urш ·СлPO5includes independent pixels (nxsteps) and separate НЇ ·Слe 5spectra (ysteps) and is the sum of ALL groups. See O ·@СлEXPOSURE.(ETS-f) UN UTккhТг tEXP_CORR┌ ) ° Уеbe\division by exposure time: Convert to count rates. This routine converts the input data to es5 °Уеcu\count rates by dividing by the exposure times. The exposure time is computed for each bin ОA °УеPTLas 0.05*NCOADD*INTPER, where NCOADD is the number of coadds to the bin and CTM °Уеt ^INTPER is the integration period in 0.05 second intervals. If either value contains fill, no Y °@Уеl Uexposure time can be computed and the entire bin is flagged as unusable. (calguide) IsUL UTккhФгCAEXTNCT_V█ В Ў`ХеSLextinction in V: Cd╕┘ea╣╣)isHH╘И╣┌╕HH╘И╖╗■k (ho UT UTккhЦг ·EX_EFFIC▄ ■ Чеde]scaled extended source cathode efficiency: Extended source sensitivity relative to that of L$ ■Че ·^the reference aperture, unitless. This keyword is filled by the calibration software only 0 ■@Че t'when the target is an extended source. e cJUR UTккhШгdaE_B_V ▌ Y №`Щеt E(B-V): disUP UTккhЪгsuFAINT ▐ exВ ·`Ыеpu,lower threshold for star presence (counts): .0ЬUN UTккhЬгheFCHNL ▀ heл ° Эе t@first channel: ACTUAL FLAGS AND INDICATORS COMMON (FOS keyword: ri╖ °ЭеiLNCHNLS). The first channel to be processed: 0,2,4,...,510 or -1 for error. e ├ °@Эеf[qexposure.fchnl] ▌UL UTккhЮг. FDMEANANр ь Ў ЯеEXHFirst derivative coefficient for mean anomaly in revolutions per second° Ў@Яе[wiephemeris.fd_mean_anom] ИUJ UTккhагFGSLOCK с ! Ї беQstatus of FGS lock (FINE, COARSE, GYROS, UNKNOWN): Keyword source is the field t- Ї@беdeJqbs_obset.scenario_acq which is translated into simpler terms. (cgalok) GUH UTккhвгreFGWA_ID т V Є`геwoThe disperser id: alid Є`дл oDisperserDisperser ID 'whr Є`елn G130HH13 ce.А Є`жлШG190HH19 ▌О Є`злЩG270HH27 diЬ Є`илsuG400HH40 exк Є`йлpuG570HH57 hol╕ Є`клe G780HH78 ЬUN╞ Є`ллFCG160LL15 л °╘ Є`млfiG650LL65 ACTт Є`нлCAPRISMPRI FOSЁ Є`олMIRRORCAM NC■ Є`плha&or ERR for error.[qexposure.fgwa_id] UF UTккh░г °FILLCNT у ' Ё ▒е] Ynumber of segments containing fill: Science data is divided for telemetry purposes into m3 Ё▒еol\lines and frames. A line is a maximum of 965 16-bit words of science data, and a frame is FG? Ё▒еQa collection of one or more lines. For transmission purposes, a line of data is sK Ё▒еVaccommodated in a packet, which in turn is divided into from 1..16 segments (each of W Ё@▒еrewhich has 64 16-bit words.) гqUD UTккh▓гr FILTER1 ф А ю │еer`first filter number (0-48): This holds the number of the first filter used. Possible values are d║┘╗╗*40HH╘И╗┌║57HH╘И╣╜■ Є'│е15M0 to 48 (0 meaning the clear filter and 1-48 meaning one of the 48 filters). Є@│еMI[qexposure.filter1] -UT UTккh┤гorFILTER2 х < ■ ╡еUTWsecond filter number (0-48): This holds the number of the second filter used. Possible ienH ■╡е f\values are are 0 to 48 (0 meaning the clear filter and 1-48 meaning one of the 48 filters). 5 T ■@╡еie[qexposure.filter2] inUR UTккh╢г▒FILTNAMiц } №`╖еlifilter name: (i=1..2) ЧUP UTккh╕г dFILTNAMiч ж ·`╣еmmfilter name: (i=1..4) └UN UTккh║гdeFINCODE ш ╧ ° ╗еf Xobservation termination code: ZFINCOD: a status code giving the reason for the dump of ю█ °@╗еfiKthe HRS Unique Data Log. Thse codes are given in Section 3.8.3 of SE-01: sibщ °`╝л&101: Observation Processing initiated ў °`╜л"102: Observation pattern complete °`╛л 103: Under-exposure termination °`┐л 4104: Over-exposure termination 1-! °`└лth105: Bad-data termination / °`┴лre106: Observation time-out IUL UTккh┬г FL1HFILEщ X Ў`├еr first flat-field header file: rUJ UTккh─г fFL2HFILEъ Б Ї ┼еVFlat Field Files (FLT): FOS flat field reference files contain diode and photocathode Н Ї@┼е ■Xsensitivity data used to reduce flat-field spectra (spectroscopy ground software mode). ╖зUH UTккh╞г (FLATCORRы ╢ Є ╟еNA\Do flat field correction: YES, NO, DONE: Correct the input science image for variations in ┬ Є╟еrv]gain among pixels by applying a flat-field image. The input science image is multiplied by ╬ Є╟еU]the flat-field image. The names of the flat field image and its DQF must be provided in the O┌ Є@╟еin+keywords FLATFILE and FLATDFIL. (calguide) atiЇUF UTккh╚гe FLATDFILь Ё`╔еxp&name of the flat field reference DQF: UD UTккh╩гreFLATFILEэ , ю ╦еthZFlat Field Reference Files (FLT): The variations in sensitivity between pixels in the CCD 8 ю╦е Xdetectors are corrected by applying a flat field reference file. This file contains the ЇD ю╦еFl_normalized inverse sensitivity (gain) for each pixel in the detector. It is made from internal @┼P ю╦еdaZflat lamp exposures, the combination of streaked earth flats or processed observations of \ ю╦е `astronomical sources. The image is multiplied by the flat field file after correcting for bias, r h ю╦е ЄZpreflash, superpurge, and dark. The FLATDFIL is the name of the flat field reference data t ю@╦еquality file. d╝┘me╜╜+agHH╘И╜┌╝ tHH╘И╗┐■E *AT UT UTккh╠гtiFLATNTRGю ■ ═е \planetographic coordinate system parameters: flattening of planetary target, the difference $ ■@═еthKbetween the equatorial and polar radius divided by the equatorial radius. els2 ■`╬л[qobservation.flattening] LUR UTккh╧гOFLT_CORRя [ № ╨еs `flat-fielding: Remove diode-to-diode sensitivity variations and fine structure by multiplying thg №╨еma`by the flat field response. The object spectra and sky spectra (if obtained) are flat-fielded. las №╨еsedThis process requires the use of the flat field response file, fl1file. A second flat field file, a №╨еr ]fl2file, is required for paired aperture or spectropolarimetry observations. This step is a lЛ №@╨е d0spectroscopy mode calibration step. (calguide) еUP UTккh╤гFLX_CORRЁ ┤ · ╥е_flux scale generation: Convert the object spectra to absolute flux units. The object spectra гti└ ·╥е ■\are converted to flux units by multiplying by the inverse sensitivity vector. This routine t╠ ·╥е ■_requires the inverse sensitivity file iv1file. A second inverse sensitivity file, iv2file, is 2 ■╪ ·╥е[qZrequired for paired- aperture or spectropolarimetry observations. This calibration step ф ·╥е-t[converts the count rates to units of ergs/cm^^2/sec/Angstrom. This step is a spectroscopy theЁ ·@╥еse"mode calibration step. (calguide) UN UTккh╙гe FLX_CORRё ° ╘еse_flux scale generation: Calculate the absolute flux by dividing the flux by the absolute flux le,% °╘е╨Ycoefficients using the absolute flux file, abshfile, and corresponding wavelength file, e1 °╘е[nethfile. This routine converts the input flux to absolute flux units by dividing it by a = °╘е_sensitivity stored in absfil (sensitivities) and netfil (wavelengths for the sensitivities). гtiI °╘е ■_Quadtratic interpolation is used within the sensitivity file to compute sensitivities for the ╠ ·U °@╘еreinput wavelengths. (calguide) oUL UTккh╒гcoFPKTTIMEЄ ~ Ў ╓еleVthe time of the first packet: Each packet contains ancillary information including a К Ў╓еbr]spacecraft time code value. This value contains the spacecraft time of transmission of the Ц Ў@╓еec╒Line Start╒ signal. ░UJ UTккh╫гibFP_SPLITє ┐ Ї`╪екк)fp-split (NO, TWO, FOUR, DSTWO, DSFOUR): e┘UH UTккh┘гatF_RATIO Ї ш Є ┌еbyRfocal ratio: Set to 48 if the optic relay (OPTCRLY) is ╒F48╒; set to 288 if the Ї Є┌е fYcoronographic apodizer mask (CAMMODE) is in the beam; otherwise the focal ratio is set u Є@┌еinto 96. (OPR.20224) flUF UTккh█гng GCOUNT ї °) Ё`▄еsenumber of groups: CUD UTккh▌гtiGEOCORR Ў R ю ▐еe Zgeometric correction: Geometric correction. A raw FOC image is slightly distorted (about ^ ю▐еpuW2%) by the optics and the detector. The distortions are comparable in magnitude. The ккj ю▐е\optical distortion was computed by ray tracing, and the detector distortion is measured by atv ю▐е ЎYtaking flat-field images and observing the positions of reseau marks that are uniformly tВ ю▐е ^spaced on the photocathode. A geometric correction reference file includes both optical and d╛┘WO┐┐,ккHH╘И┐┌╛HH╘И╜┴■ti(y ▐е; bdetector distortion. It consists of two sets of positions: a uniform grid of reference positions ▐еraT(i.e., on the sky) and where those positions would be observed in a raw FOC image. ї ▐е▄^Removing the distortion involves determining the location in the input (distorted) image of ,▐е c]each pixel in the output (undistorted) image, and then interpolating the DN (in counts) for s8@▐е TXthat location. Bilinear interpolation is used for both the position and DN. (calguide) onQUT UTккh▀гayGEODEFV ў ` ■`реti*geo DN value for areas outside sci image: zUR UTккhсгagGEOHFILE° Й № те rYGeometric Distortion Files (GEO): The geometric distortion correction data files contain rХ №теreWdata used to correct FOC science images for the geometric distortion caused by the FOC б №теYoptics and the Photon Detector Assembly (PDA). It is used for the geometric calibration. н №теioYThe geometric distortion correction data files consist of the distorted and undistorted, ╣ №теn Tsample and line coordinate values (REAL*4) of a grid of reference points on the FOC ┼ №@те tdetector screen. l▀UP UTккhугe GMF_CORR∙ ю ·`феiscale reference background: eaUN UTккhхгtpGOODMAX · °`цеin$maximum value of the "good" pixels: 1UL UTккhчгthGOODMIN √ @ Ў`шеon$minimum value of the "good" pixels: (ZUJ UTккhщгUTGPIXELS № i Ї`ъе!number of "good" pixels (DQF=0): sГUH UTккhыг: GRAPHTAB¤ Т Є`ье Ethe HST graph table: See PHOTMODE and related photometry keywords. iмUF UTккhэгn GRATING ■ ╗ Ё`юетEgrating, echelle or mirror in use: GRATING -- grating/echelle mode: i╔ Ё`ялOC#Spectral ElementGratingDetector the╫ Ё`ЁлssG140MG-1Digicon 1 or х Ё`ёлbrG160MG-2Digicon 2 еioє Ё`ЄлstG200MG-3Digicon 2 les Ё`єлstG270MG-4Digicon 2 ╣ № Ё`ЇлsaG140LG-5Digicon 1 val Ё`їлgrECH-AE-ADigicon 1 th+ Ё`ЎлECH-BE-BDigicon 2 . l9 Ё`ўлe SAFE1SAFDigicon 1 G Ё`°лfeSAFE2SAFDigicon 2 UTU Ё`∙лMAMIRROR-N1MN1Digicon 1 c Ё`·л tMIRROR-A1MA1Digicon 1 q Ё`√лMIMIRROR-N2MN2Digicon 2 Ё`№л tMIRROR-A2MA2Digicon 2 d└┘┴┴-f HH╘И┴┌└HH╘И┐├■ 'HS`¤лeeNDF OD`■лom5(NDF = NOT DEFINED, ERR = ERROR) [qexposure.grating] Ё/UT UTккh гgrGRNDMODE > ■`еRAground software mode: odeL ■`ляLED-FLAT-FIELD-MAP (IMAGE) Z ■`лTIME-RESOLVED(PERIOD) Dh ■`лTIME-TAGGED(TAG) G-v ■`л ЁRAPID-READOUT(RAPID) G-Д ■ л Ё0TARGET ACQUISITION(ACQ,ACQ/BINARY,ACQ/PEAK,ACQ/Р ■@лL FIRMWARE) Ю ■`лSPECTROSCOPY(no polarizer) 1м ■`лЎ4SPECTROPOLARIMETRY(with polarizer) (tguide 7.0-10) SA╞UR UTккhг 1 GROUPS ╒ №` еSAimage is in group format: яUP UTккh г1 HEADER ■ ·`е tscience header line exists: ЁUN UTккhгMIHEL_CORR ' ° еXconversion to heliocentric wavelengths: Convert wavelengths to heliocentric coordinate 3 °@ еQsystem. This routine corrects for the Earth╒s motion around the Sun. (calguide) MUL UTккhгHIGHVOLT \ Ў еEDZscaled high voltage factor: Scaling factor relative to the reference volatge, unitless, h Ў@еmo3calculated by the calibration software (calhsp). AGEВUJ UTккhгHOFFi OLС Ї`е ■"horizontal offset bin i+1: i=1..6 лUH UTккhгHSTHORB ║ Є`е ■-half the duration of the ST orbit (seconds): I╘UF UTккhгHVPSM у Ё`е ■9high voltage power supply output of the object detector: ¤UD UTккhгOLIAC_CORR ю е7.Yincidence angle correction: Adjust the zero-point of the wavelength scale for the large юе1]science aperture and the two spectral lamp apertures using table CCR8 containing incidence O$ юе_angle coefficients. This routine adjusts the wavelenght array for the difference in incidence 0 юе[angle of apertures LSA, SC1 and SC2 from the SSA. Table CCR8 is searched for the correct кк< юе `grating, spectral order, aperture, and carrousel position to obtain two coefficients, A and B. olH юе Ў\Interpolation of the coefficients (in carrousel position) is used if an exact match is not HOT ю@е\found. These coefficients are then used to compute an offset using the following formula: b ю`л dw = w + (A+B*s)/m p ю`лUFWhere: ~ ю`лw is the wavelength, id┬┘th├├.UDHH╘И├┌┬ юHH╘И┴┼■on&us`лf "A and B are coefficients in ccr8, `л1+s is the photocathode sample position, and ap$`лe m is the spectral order. O2`л(calguide) iciKUT UTккhг aIMAGETYP Z ■` еhe;image type: DARK/BIAS/INTFLAT/KSPOTS/EXTERNAL/EARTH-CALIB: erttUR UTккh!г SINFOB A.Г №`"еrc"deflection pairs/substep pattern: ЭUP UTккh#г sINFOC aм ·`$еus,largest repeat code in the substep pattern: B╞UN UTккh%гINSTRUME ╒ °`&еieinstrument in use: itу °`'л eFGS: Fine Guidance System ё °`(лd.FOC: Faint Object Camera e °`)лanFOS: Faint Object Spectrograph la: °`*л*HRS: Goddard High Resolution Spectrograph ° +л8HSP: High Speed Photometer WFPC: Wide Field/Planetary ' °@+лCamera AUL UTккh,г INTOBS P Ў`-е*expected number of intermediate readouts: jUJ UTккh.гd INTS ieny Ї`/еnumber of integrations: toУUH UTккh0гitINT_TIME в Є`1еm /time of integration (in 1/1.024 microseconds): lgu╝UF UTккh2гккITFCORR ╦ Ё 3е\intensity transfer function correction: Apply format-dependent photometric correction. The IN╫ Ё3еcreference files used in this step are called ITF files for historical reasons. They are not full-еusу Ё3еod[frame; there is one such file for each format. The format-dependent correction is applied entя Ё3е\by multiplying the image from the previous step (i.e., the dark-count subtracted image) by √ Ё@3е Fthis file. (calguide) la:UD UTккh4гITFHFILE $ ю 5еct]Intensity Transfer Function Files (ITF): The Intensity Transfer Function (ITF) files contain 0 ю5еraWdata used to correct FOC science images for spatial nonuniformities that depend on the iat< ю5еUT[image format. It is used for the format-dependent photometric correction. An ITF data file гitH ю5е ЄWhas the same form as an FOC image. The lengths of the axes are the same or larger than ITT ю5е[those of the image to be calibrated. Each entry is a REAL*4 scaling factor that is used to rec` ю5еUmultiply the corresponding pixel DN count in the FOC science data file that is to be al ю@5еt corrected. d─┘su┼┼/t.HH╘И┼┌─isHH╘И├╟■pl(he UT UTккh6гreIV1HFILE ■`7еub'first inverse sensitivity header file: th2UR UTккh8гe)IV2HFILE A № 9е ^Inverse Sensitivity Files (IVS): FOS inverse sensitivity reference files contain data used to M №@9еtaSconvert object data to an absolute flux scale (spectroscopy ground software mode). ormgUP UTккh:гon IXDEFi v ·`;еe initial x deflection i: i=1..5 -deРUN UTккh<гc IYDEFi IЯ °`=е юinitial y deflection i: i=1..5 rm ╣UL UTккh>гhe KSPOTS ╚ Ў ?еorWStatus of Kelsall spot lamps: ON, OFF: Determined by PODPS on the basis of the packet a R╘ Ў?еTformat code of the observation: KSPOTS=OFF unless the packet format code=╒24╒x or tр Ў@?еa ╒2C╒x. (cgwsdh) a·UJ UTккh@гt KXDEPLOY Ї Aе┘TCOSTAR deployed for FOC (T or F) The logical DEPLOY keywords are to be set to True ЇAе╟Wonly if the COSTAR arm for that SI has been deployed. There are two conditions under se ! ЇAе fZwhich this keyword should be set to False. Before the servicing mission, a database flag - ЇAе s[will have to be set to instruct PODPS not to extract the COSTAR mirror positions from the an 9 ЇAеe [SHP (the telemetry positions will still correspond to HSP data), set the DEPLOY keywords еe E ЇAеti[to False and set the mirror position keywords to a default value (99999). Once COSTAR is n iQ ЇAеUT]installed in HST, the database flag will be set to indicate that the COSTAR SHP entries are m] ЇAеheQvalid. PODPS should then populate the DEPLOY keywords based on the SHP position Ti ЇAеacZtelemetry values. If any of the telemetered values for a given SI are the default value u ЇAеZ(99999), then the DEPLOY keyword for that SI should be set to false. This will allow for Б Ї@Aе?the possibility of deploying some COSTAR arms and not others. TheЫUH UTккhBгonKXBFOCUS к Є`CеwhCOSTAR M1 Focus Position (mm) ─UF UTккhDгe KXBXTILT ╙ Ё`Eеg 'COSTAR FOC M1 X-tilt Position (arcsec) toэUD UTккhFгt KXBYTILT № ю`Gеti'COSTAR FOC M1 Y-tilt Position (arcsec) (tUB UTккhHгtiKYDEPLOY % ь IеatTCOSTAR deployed for FOS (T or F) The logical DEPLOY keywords are to be set to True ti1 ьIеefWonly if the COSTAR arm for that SI has been deployed. There are two conditions under ase= ьIеtoZwhich this keyword should be set to False. Before the servicing mission, a database flag I ьIеY [will have to be set to instruct PODPS not to extract the COSTAR mirror positions from the lemU ьIеa [SHP (the telemetry positions will still correspond to HSP data), set the DEPLOY keywords at a ьIеto[to False and set the mirror position keywords to a default value (99999). Once COSTAR is rmsm ьIеhe]installed in HST, the database flag will be set to indicate that the COSTAR SHP entries are Ty ьIеTIQvalid. PODPS should then populate the DEPLOY keywords based on the SHP position кd╞┘╟╟01 HH╘И╟┌╞UTHH╘И┼╔■I'COIеFOZtelemetry values. If any of the telemetered values for a given SI are the default value IеfoZ(99999), then the DEPLOY keyword for that SI should be set to false. This will allow for @Iеd ?the possibility of deploying some COSTAR arms and not others. I ь9UT UTккhJгwiKYBFOCUS H ■`KеS COSTAR M1 Focus Position (mm) bUR UTккhLгheKYBXTILT q №`Mе t'COSTAR FOS M1 X-tilt Position (arcsec) toЛUP UTккhNгe KYBYTILT Ъ ·`OеI'COSTAR FOS M1 Y-tilt Position (arcsec) n k┤UN UTккhPгltKZDEPLOY ├ ° QеmsTCOSTAR deployed for HRS (T or F) The logical DEPLOY keywords are to be set to True t ╧ °QеriWonly if the COSTAR arm for that SI has been deployed. There are two conditions under d o█ °Qе кZwhich this keyword should be set to False. Before the servicing mission, a database flag ч °Qе[will have to be set to instruct PODPS not to extract the COSTAR mirror positions from the lemє °Qеa [SHP (the telemetry positions will still correspond to HSP data), set the DEPLOY keywords at °Qеto[to False and set the mirror position keywords to a default value (99999). Once COSTAR is rms °Qе]installed in HST, the database flag will be set to indicate that the COSTAR SHP entries are T °QеTIQvalid. PODPS should then populate the DEPLOY keywords based on the SHP position к# °Qе Ztelemetry values. If any of the telemetered values for a given SI are the default value / °QеZ(99999), then the DEPLOY keyword for that SI should be set to false. This will allow for ; °@Qе?the possibility of deploying some COSTAR arms and not others. TheUUL UTккhRгonKZBFOCUS d Ў`SеwhCOSTAR M1 Focus Position (mm) ~UJ UTккhTгe KZBXTILT Н Ї`Uеg 'COSTAR HRS M1 X-tilt Position (arcsec) toзUH UTккhVгt KZBYTILT ! ╢ Є`Wеti'COSTAR HRS M1 Y-tilt Position (arcsec) (t╨UF UTккhXгtiLEDCOLOR " ▀ Ё YеatLLED color (a color, blank , NONE or ERROR): If at least one telemetry item roы ЁYеs U(XC1LEDSL, XC2LEDSL) is NOT fill, then the FOC LED selection table will be searched ў ЁYеwiUto determine the significance of the telemetered value or values. If the telemetry D ЁYеpuXmeasurements are above a threshold count, then LEDMODE is ON , else it is OFF. If both s. ЁYеemTtelemetry measurements are valid, then both must agree on whether LEDMODE is ON or n Ё@Yе fCOFF. If they disagree, an error condition is generated.(cp2jld) @Q5UD UTккhZгitLEDMODE # D ю [еndOled calibration status: ACTIVE, NOTUSED: calibration LED mode: ACTIVE,NOTUSED. M1 P ю@[е) [qexposure.ledmode] KZjUB UTккh\гLINE $ 'COy ь`]е Pline positions: tod╚┘ ╔╔1COHH╘И╔┌╚c)HH╘И╟╦■ Ё! UT UTккh^гr LINEBEG % ■`_еI+line number (1st line: wrt source format): Y2UR UTккh`гC2LINEBEG & A №`aеLE+line number (1st line: wrt source format): [UP UTккhbгmiLINENUM ' j ·`cеtePEP proposal line number: ДUN UTккhdгLINEOFF ( У °`eеveQline offset (0.0-1023.75): Line offset, mnemonic = XCCCUVRO.[qexposure.lineoff] YнUL UTккhfгasLINEPFM ) ╝ Ў gе Ilines per frame (64, 128, 256, 512, or 1024): Number of lines per frameg╚ Ў@gеdi[qexposure.linepfm] p2тUJ UTккhhгккLINES * ODё Ї`iеnumber of lines in a group: usUH UTккhjг cLIVETIME + Є`kеD.2accumulator open time (units of 7.8125 microsec): 4UF UTккhlгLI LOCATE , ьC Ё`mеli%do a locate after the spiral search: ]UD UTккhnгLONGPMER - l ю oе┌Vplanetographic coordinate system parameters: longitude of prime meridian of planetary x ю@oе ■ target. [qtargets.long_prim_me] lТUB UTккhpгrmLPKTTIME . б ь qеBEUthe time of the last packet: Each packet contains ancillary information including a кн ьqе ^spacecraft time code value. This value contains the spacecraft time of the start of the DMA ╣ ь@qе oH(Direct Memory Access) transfer that produced the data for the packet. Y╙U@ UTккhrгasMAG_B / т ъ`sе expected B Magnitude: №U> UTккhtг02MAG_R 0 li ш`uе Ўexpected R Magnitude: %U< UTккhvгUJMAG_U 1 кк4 ц`wе Їexpected U Magnitude: NU: UTккhxгupMAG_V 2 кк] ф`yе expected V Magnitude: wU8 UTккhzг t MAP 3 d╩┘l╦╦2 ЁHH╘И╦┌╩r HH╘И╔═■LO( `{еo-dwell points at which to image the aperture: r!UT UTккh|гimMAP_CORR 4 0 ■ }еYmapping function: Perform the photocathode mapping function using tables ccr1 and ccr2 < ■}е oWcontaining the photocathode line mapping and sample parameters. This routine computes qH ■@}еtiRthe mapping function for each of the substep bins using the following formulae: V ■`~л(D"SAMPLE(bin) = x0 + b*XD + c*XD^^2 d ■`лfoDELTAS(bin) = e U@r ■`АлMALINE(bin) = L0 + A*YD А ■`Бл BWhere: : О ■`Вл025SAMPLE -- is the sample position of the first diode, uЬ ■`Глv2DELTAS-- is the spacing between sample positions, к ■`ДлUT,LINE -- is the line position of the diodes, ╕ ■`Елtu&XD -- is the X-deflection minus 2048, ╞ ■`Жл&YD -- is the Y-deflection minus 2048, ╘ ■ Зл6s0, b, c and e are coefficients in ccr2, interpolated р ■@Злfor oю ■`Илwhthe given Y-deflection, and UT№ ■`ЙлMA'L0, and A -- are coefficients in ccr1. fu ■`Клhe(calguide) ma$UR UTккhЛгngMAP_NUM 5 3 №`Меmosaic map number: theMUP UTккhНгMASKCORR 6 \ · Оеs TDo mask correction: YES, NO, DONE: Include the static bad pixel mask in the output bh ·ОеloWDQF. The name of the static bad pixel mask must be provided in the keyword MASKFILE. лfot ·@ОеU@5This file is in the same format as a DQF. (calguide) ОUN UTккhПг: MASKFILE 7 Э ° Ре tUStatic Bad Pixel Mask Files (MSK): The static mask files (formerly known as the data eй °РеioYquality masks) contain flags for those pixels which always contain degraded values. This u╡ °Реef\mask is routinely incorporated into the data quality file generated in the RSDP pipeline by З┴ °Ре e]calwfp. The static mask file is a short integer (INTEGER*2) image file of of four (4) groups i═ °РеanWwith the same dimensions as the WF/PC science image. The image contains values of zero (c┘ °РеUT\(0) in all pixels, except for those with known static defects. Defective pixels are flagged MAх °@Реwith the value four (4). c UL UTккhСгE: MAXCLK 8 t Ў`Теk maximum clock count: (UJ UTккhУг T MAXGSS 9 7 Ї ФеasSmaximum substep patterns/observation: read from the value telemetered in the HRS thC Ї@Фе D"Unique Data Log (UDL): ZMAXGSS. ]UH UTккhХг °MAXWAVE : l Є`Це Mmaximum wavelength: tad╠┘th══3РHH╘И═┌╠ fHH╘И╦╧■de&es UT UTккhЧгMAXWAVE ; ■`Шеormaximum wavelength: li2UR UTккhЩгinMDF_CORR < A № ЪеZmedian filter of background spectra: Use a median filter on the background. This routine M №Ъеbperforms a median filter of the background with a user-specified (i.e., specified in the table) Y №ЪеР]filter width. The edge points are filled with the value of the closest position that can be ee №@ЪеРfiltered. (calguide) uUP UTккhЫгккMEANANOM = О ·`Ье)mean anomaly. [wiephemeris.mean_anomaly] киUN UTккhЭг 9 MERGED > ╖ °`Юеsu*number of merged spectra in this pattern: ╤UL UTккhЯгinMER_CORR ? р Ў аеUnZmerging of substep bins: Merge the substep bins. This routine merges the spectral data. ь ЎаеtaWUnmerged output data is just a copy of the input data. Both the input and output data ° Ўае_arrays are 2-dimensional arrays treated as 1-dimensional arrays by this routine. The input is imu ЎаеUR[treated as 1-dimensional to make copying faster (2-dimensional copying takes longer) and se Ўае t\the output array is treated as 1-dimensional because this routine computes its dimensions. wi Ў@аеd (calguide) ied6UJ UTккhбг №METER @ РE Ї`веe 4observation terminated by exposure meter? (Y or N): po_UH UTккhггMINWAVE A n Є`деalmaximum wavelength: ЫИUF UTккhег MINWAVE B Ч Ё`же. maximum wavelength: al▒UD UTккhзгЭMIR_REVR C └ ю`иеЮis the image mirror reversed: ┌UB UTккhйгULMNF_CORR D щ ь ке ЎVmean filter of background spectra: Use a mean filter on the background. This routine ї ьке `performs a mean filter of the background with a user-specified (i.e., specified in the table) ut ьке]filter width. The edge points are filled with the value of the closest position that can be ь@ке Ўfiltered. (calguide) e'U@ UTккhлгl MODE E ng 6 ъ меnaKinstrument mode SCP, SSP, ARS: instrument mode for hsp: SCP = single color ateB ъме bSphotometry, SSP = star/sky photometry, ARS = area scan, DUM = a dump; wfpc: FULL = 6UJN ъмеMEUfull-resolution (800X800), AREA = area-integration (400x400); fos: modes specify how oZ ъме]the data should be calibrated: target acquisition, spectroscopy, rapid-readout, time-tagged, f ъ@ме. Ztime-resolved, spectropolarimetry. hrs: direct readout, accumulation, target acquisition t ъ`нл: [qexposure.mode] Ld╬┘ Ў╧╧4roHH╘И╧┌╬ tHH╘И═╤■к*pe UT UTккhогteMODHFILE F ■ пеecXReseau Mark Model Files (MOD): A reseau mark model data file contains from one to fifty s $ ■пеe Vmodels of reseau marks. A reseau mark model is a small image file containing a reseau 0 ■пеl [mark in the center and just a few background pixels around the edge. It is used during the SC< ■пеteWreseau calibration. Each group of a reseau mark model file has the form of a miniature p; H ■пе ъ\rectangular image, i.e., a reseau mark model which is used to determine the actual location ciT ■@пе9of each reseau mark listed in the reseau reference file. ,nUR UTккh░гidModified G } № ▒еVUniversal Time is defined as time since 00:00 17-Nov-1858, in 100-nanosecond units. Й №▒еWThis is the Smithsonian base date & time for the astronomical calendar. The Modified roХ №▒е┌WJulian Date (MJD) is defined as time since 00:00 17-Nov-1858, in units of days and MOб №@▒еfractions of a day. (cgamjd) ╗UP UTккh▓гeaMOD_CORR H ╩ · │еomSground software mode dependent reductions: Perform ground software mode-dependent a s╓ ·│еntWreductions for time-resolved, spectropolarimetry, and rapid-readout observations. The arт ·│еis]following processing steps are performed in addition to the standard case and spectroscopy ю ·│еof_mode calibration steps. Rapid-Readout: The total and its statistical error for each frame are to · ·│еalZcalculated. Time-Resolved: The average of all slices (bins) and the differences from the ·│еidUaverage for each slice (bin) of the last frame of time-resolved data are computed. N ·│еnaQSpectropolarimetry: The spectropolarimetry reductions require the Wollaston and r ·│еca^Waveplate parameter table, ccs4, and the retardation reference file, rethfile. On an initial * ·│еniapass, the reference data is read. On all calls to the special processing routine, the flux and O6 ·│еYerrors are saved for use on the last call---in which the processing is done. The Stokes tB ·│е│Zparameters, linear and circular polarization, and the polarization angle (theta) for FOS N ·│е│]polarimetry data are computed. Interference is corrected using the coefficients in ccs4 and oZ ·│е│Ytheta is changed to sky coordinates by adding PANGAPER. If you are truly interested in ff ·@│е/how this works, talk to Rich Allen. (calguide) ragАUN UTккh┤гinMOONANGL I П ° ╡е ·Qangle between moon and V1 axis (deg): Computed as: moonangle = cosd(declmoon) * dЫ °╡еNWcosd(declnv1) * cosd(rtasmoon - rtascnv1) + (sind(declmoon) * sind(declnv1)) moonangle Wolз °@╡е= acosd (moonangle)(cgaang) ta┴UL UTккh╢г r MTFLAG J e╨ Ў`╖еle2moving target flag; t = this is a moving target. ▐ Ў`╕лd.[qobservation.mt_flag] ial°UJ UTккh╣гe,MT_LVi_k K Ї ║еQmoving target information: Proposer comments on moving targets (i=1..3, k=1..5). Ї@║е UTккh╫гNPDECTRG Z S ш ╪еit\planetographic coordinate system parameters: declination of north pole of planetary target. h _ ш@╪еtw[qobservation.north_dec] syU< UTккh┘гanNPRATRG [ d╥┘. ╙╙6teHH╘И╙┌╥olHH╘И╤╒■rr%in`┌еh &north pole right ascension of target: !UT UTккh█гNREAD \ th0 ■`▄еDa%number of readouts per memory clear: eJUR UTккh▌г. NSHUTA17 ] Y №`▐еFO!Number of AP17 shutter B closes: tsUP UTккh▀гofNXSTEPS ^ В · ре Dnumber of x steps: ACTUAL FLAGS AND INDICATORS COMMON (FOS keyword: UTО ·@реELENXSTEPS). The number of xsteps per ystep: 1,...,32 or -1 for error. кЬ ·`сл [qexposure.nxsteps] to╢UN UTккhтгpeOBSERVTN _ ┼ °`уеliobservation number (base 36): ▀UL UTккhфгttOBSET_ID ` ю Ў хе╫[observation set id: The observation set id, these are numbered sequentially throughout the ati· Ўхеf Dproposal. A base 36 number which allows for 1295 observation sets. U< Ў@хеNP[qobservation.obset_id] UJ UTккhцг. OBSINT a / Ї`чеintermediate readout number: IUH UTккhшгOBSMODE b X Є`щеobservation mode: rigf Є ълrg%╒DIRECT READOUT╒ if proposed mode is hr Є@ълDa╒RAPID╒,╒ENGINEERING╒, memА Є`ылUT╒PULSE-HEIGHT╒, ╒THRESHOLD╒; №О Є ьлNu#╒ACCUMULATION╒ if proposed mode is UTЪ Є@ьлEP╒ACCUM╒,╒OSCAN╒,╒WSCAN╒, и Є`элs: ╒PHOTOSCAN╒; N╢ Є юлN )╒TARGET ACQUISITION╒ if proposed mode is P┬ Є@юлxs╒ACQ╒,╒IMAGE╒,╒DEFCAL╒, r ╨ Є`ял ·╒ACQ/PEAKUP╒. (tguide 7.0-12) ъUF UTккhЁгкк OBSRPT c V∙ Ё`ёеobservation repeat number: (baUD UTккhЄгккOBSSTRTT d " ю єе[predicted obs. start time (seconds since 01/01/1985) OBSSTRTT is the predicted start time out. юєеQPSTRTIME (which comes from the relation qobservation) converted to sogs_seconds Ў: юєе[qV(seconds since 01-jan-1980 00:00:00.00) less the number of seconds between 1980 and F ю@єеbe1985 (157852800). (cecosp) MOD`UB UTккhЇгOFFS_TAB e o ь`їе Є.GIMP offsets (post-pipeline processing only): d╘┘ID╒╒7 ЄHH╘И╒┌╘╒THH╘И╙╫■AT&f UT UTккhЎгUTOFF_CORR f ■`ўеANPerform GIMP correction: э2UR UTккh°г NOPFORMAT g A №`∙еIS%output product format specification: [UP UTккh·гMA OPMODE h j ·`√е ·proposed operation mode: -ДUN UTккh№гЁOPTCRLY i У ° ¤еёVoptical relay: F48,F96,F288. These are the three possible magnifications in which the Я °@¤еs.%camera operates. [qexposure.optcrly] ╣UL UTккh■гedOPTELTn j ╚ Ў еєXThis specifies which filter or optical element was used on (F48,F96) wheel n: 0,...,11. ю╘ Ў@ е(s(wheel n=1..4) janюUJ UTккhг lORIENTAT k ¤ Ї`е19$the orientation of the image (deg): 78UH UTккhгODOUTDTYPE l & Є е UOutput image datatype: REAL, LONG, SHORT: Select the data type of the output (.c0h) ┘2 ЄеNimage. The allowed options are REAL, SHORT, and LONG corresponding to single-> ЄеAT_precision real, short integer, and long integer pixels. The data is scaled with the keywords UTJ Є@еRMFWSCALE and WZERO if the SHORT or LONG option is selected. (calguide) dUF UTккhгOPOVERSCAN m s Ё еprBoverscan number: ACTUAL FLAGS AND INDICATORS COMMON (FOS keyword: Ё@еcaAOVERSCAN). The overscan number: 1,2,3,4,...,256 or -1 for error. iЩUD UTккhгPARALLAX n и ю еxp_expected parallax of target: (0.,1000.)... target parallax in arcsec (1 x 10e-3 precision) the lte┤ юеnt^change in direction of a celestrial object which results from the change from heliocentric to └ ю@е Egeocentric coordinate systems. (default = zero). [qtargets.parallax] T┌UB UTккhгTYPAR_CORR o щ ь` еut#parallax correction used (T or F): SelU@ UTккh гofPASS_DIR p ъ`еpolarization pass direction: s,U> UTккhг aPA_APER q ; ш е ЄUposition angle of aperture used with target (deg): This value is computed before the sG ш еywZobservation, rather than spacecraft measured. This is the angle from North, towards East, S ш еккUof the +Y-axis of the Science Instrument Corrected System (SICS) coordinates for the O_ ш еwoXaperture designated by APEROBJ. The direction of North is taken at the target even when ik ш еShe target is not centered in the FOV. For FOC, the zoomed FOV have the SICS Y-axis et w ш е (Zaligned with the direction of increasing pixel. In the group data, the Y-axis (for the CD Г ш еm Vmatrix and ORIENTAT) is always the direction of increasing line. For these zoomed FOC d╓┘ T╫╫8PAHH╘И╫┌╓paHH╘И╒┘■UT) е \apertures, that can be identified as those with a Z in the fourth caharcter in APEROBJ, the еtiVvalue of PA_APER will be 90 degrees larger than the ORIENTAT value in the group data. еrvYFor FOS, in the right-handed XY coordinate system of the detector, this is the angle one , еheTrotates the image clockwize in order for North to coincide with +Y. The FOS APEROBJ 8 еtuOvalues that end in "BAR" have a PA_APER value 90 degrees larger than ORIENTAT. iD@ е[qobservation.aper_angle] ]UT UTккhгC, PA_REF r l ■ еisVpos. angle of target from ref. object (deg): Reference target is that used for target x ■@еorKacquisition. (Not yet supported. Always zero.) [qobservation.position_ang] inТUR UTккhг tPA_V3 s C б № е┘\position angle of v3 axis of ST (deg): This is the angle from North, towards East, of the Y-н №еWaxis of the vehicle coordinate system. The direction of North is taken at the V1-axis. the╣ №еinYPosition angles measured from North at different right ascensions, such as at the target R┼ №еe Uposition for PA_APER or the aperture reference position for ORIENTAT, will include a t╤ №@еisWsmall correction for the difference in the direction of North. [qobservation.psanglv3] oinыUP UTккhгFO PCOUNT t · ·`еvanumber of group parameters: PAUN UTккhгrePDTYPEi u # °`еLData type of the group parameter number i. This is a required FITS keyword. ■=UL UTккhгpoPEP_EXPO v L Ў`еt ,PEP exposure identifier including sequence: t fUJ UTккhгorPEQUINOX w u Ї`е A`8л1!= ( INTEGRAL P(LAM)*LAM*DLAM ) / L`9лUV( INTEGRAL P(LAM)*DLAM ) 3Z`:лd and: h`;л u!= ( INTEGRAL P(LAM)*DLAM/LAM ) / Tv`<лge( INTEGRAL P(LAM)*DLAM ) LД`=л3([Koornneef et al. (1986), Horne (1988)] bsЭUT UTккh>г ·PHOTTAB м ■`?е. 0name of the photometry keyword reference table: PL╞UR UTккh@гPHOTZPT А ╒ № AеvoVST magnitude zero point: PHOTZPT is the zero-point of the ST magnitude system. The ST с №Aе FHmagnitude is STMAG = -2.5 * LOG_10( FLAM ) + 21.10, thus constant STMAG э №AеTcorresponds to constant FLAM, and the zero-point is PHOTZPT = -21.10. This value is ∙ №Aе Schosen so that Vega has an ST magnitude of zero for the Johnson V passband. If the pa №Aе dZabsolute calibration of Vega changes, this value may also change slightly. [Koornneef et №@Aеal. (1986), Horne (1988)] +UP UTккhBг1 PKTFMT Б P: ·`Cе packet format code: WFPC: LH ·`DлType of Exposure WF PC hV ·`Eл= ---------------- ----- ----- Td ·`FлgeEXTERNAL ╒60╒X ╒61╒X Mr ·`Gл=w/PREFLASH ╒62╒X ╒63╒X 198А ·`Hлbsw/PURGE ╒64╒X ╒65╒X PHО ·`Iлw/PURGE & PREFLASH ╒66╒X ╒67╒X tryЬ ·`Jл t+EXTERNAL ╒68╒X ╒69╒X with Serial Clocks On ╒ №к ·`KлST-w/PREFLASH ╒6A╒X ╒6B╒X with Serial Clocks On t╕ ·`Lлde*w/PURGE ╒6C╒X ╒6D╒X with Serial Clocks On ╞ ·`Mл5 5w/PURGE & PREFLASH ╒6E╒X ╒6F╒X with Serial Clocks On ╘ ·`NлesBIAS ╒20╒X ╒28╒X Lт ·`OлoiDARK ╒21╒X ╒29╒X .Ё ·`PлINTFLAT ╒22╒X ╒2A╒X ch■ ·`QлhaEXTFLAT ╒23╒X ╒2B╒X er ·`RлV KSPOT ╒24╒X ╒2C╒X ·`Sл dUVFLOOD ╒25╒X ╒2D╒X o( ·`TлisDARK w/CLOCKS=ON ╒26╒X ╒2E╒X .6 ·`Uл №PREFLASH ╒27╒X ╒2F╒X 1PUN UTккhVг] PKTTIME В _ ° Wе P]time from the packet ancillary data: Each packet contains ancillary information including a Ck °WеE^spacecraft time code value. This value contains the spacecraft time associated with the SHP w °@Wе62:(standard header packet) which contains ancilliary data. d▄┘SH▌▌;HH╘И▌┌▄ wHH╘И█▀■ST*EF UT UTккhXгitPLY_CORR Г ■`YеL,polynomial smoothing of background spectra: n 2UR UTккhZг5 PODPSFF Д A №`[еit+0=(no podps fill), 1=(podps fill present): S ╒[UP UTккh\г POLANG Е Aj ·`]е ·'initial angular position of polarizer: ■ ·ДUN UTккh^гEXPOLAR_ID Ж У °`_еRpolarizer id: ╒2б °``лSA:polarizer A; X п °`aлB:polarizer B; LO╜ °`bл .C:no polarizer; №╦ °`cл2FE:error. ккхUL UTккhdг POSTNSTX З Ї Ў eеm [position of space telescope x axis (km): X-axis coordinate of the space telescope position Ўeеft[in orbit at the predicted start time of observation. The coordinates are in the geocentric Ўeеd ]J2000.0 inertial coordinate system. This is a right-handed coordinate system centered in the ▌ ЎeеYearth, with the X-axis pointing towards the vernal equinox for the year 2000, the Z-axis к$ Ўeе Zpointing towards the north celestial pole for the year 2000, and the Y-axis orthogonal to 0 Ў@eе №both. [qobservation.postnstx] JUJ UTккhfг pPOSTNSTY И Y Ї gеPO[position of space telescope y axis (km): Y-axis coordinate of the space telescope position гEXe Їgе °[in orbit at the predicted start time of observation. The coordinates are in the geocentric лq ЇgеLO]J2000.0 inertial coordinate system. This is a right-handed coordinate system centered in the } Їgе ЎYearth, with the X-axis pointing towards the vernal equinox for the year 2000, the Z-axis eЙ ЇgеZpointing towards the north celestial pole for the year 2000, and the Y-axis orthogonal to Х Ї@gеicboth. [qobservation.postnsty] пUH UTккhhгatPOSTNSTZ Й ╛ Є iеoo[position of space telescope z axis (km): Z-axis coordinate of the space telescope position th╩ Єiеor[in orbit at the predicted start time of observation. The coordinates are in the geocentric or ╓ Єiе t]J2000.0 inertial coordinate system. This is a right-handed coordinate system centered in the pт Єiе ЇYearth, with the X-axis pointing towards the vernal equinox for the year 2000, the Z-axis eю ЄiеEXZpointing towards the north celestial pole for the year 2000, and the Y-axis orthogonal to · Є@iеicboth. [qobservation.postnstz] UF UTккhjгatPPC_CORR К # Ё kеooKTYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI paired pulse correction: Correct the poi/ ЁkеveWraw count rates for saturation in the detector electronics using table coccg2r, which rth; Ёkеr acontains the paired-pulse correction table. On the first call, the paired pulse parameters are HG Ё@kеPO7read from table ccg2. The following equation is used: copU Ё`lлxi x = y/(1-yt) c Ё`mлe Where: thq Ё`nлorx -- is the true count rate, r Ё`oлio!y -- is the observed count rate, nd▐┘0.▀▀<syHH╘И▀┌▐inHH╘И▌с■i(ea`pлis,t = q0 if y is less than or equal to F, and ea`qл e.t = q0 + q1 * (y - F) if y is greater than F. $`rлr )q0, q1, and F are coefficients in ccg2r. 2`sлic0This is a standard calibration step. (calguide) atKUT UTккhtг ЁPRECISN Л Z ■`uеEN0number of diodes used to map (HIGH=1,NORMAL=2): cttUR UTккhvгPREFCORR М Г № wеraVDo preflash correction: YES, NO, DONE: If the value in keyword PREFTIME is less than П №wеpuYzero, the preflash image reference file is scaled and subtracted from the input science kЫ №wе\image. The preflash image is multiplied by the preflash lamp exposure time (obtained from mз №wе ЁVthe keyword PREFTIME in the input science image header and expressed in seconds) and │ №wеTthen subtracted from the input science image. If the keyword PREFTIME = 0, the CTE ┐ №wеZfixup is applied. The names of the preflash or CTE image and its DQF must be provided in ╦ №@wе0the keywords PREFFILE and PREFDFIL. (calguide) r хUP UTккhxгPREFDFIL Н Ї ·`yеci$name of the preflash reference DQF: ThUN UTккhzгalPREFFILE О ° {еUTXPreflash Files (PRF): The WF/PC Preflash Reference File and its associated data quality MA) °{екк[file are used to remove the signal introduced by the preflash lamp. This signal is removed val5 °{еTI_by subtracting this reference file. The reference file is scaled by the preflash exposure time racA °{е s]to allow for variations in the requested preflash exposure. The subtraction of the reference oM °{еed_file corrects for the uneven illumination pattern of the preflash image. Since the preflash is ed Y °{е №^obtained by illuminating the backside of the shutter with an internal lamp, the difference in e °{е`reflectivity of the two shutter blades requires reference files specific to each shutter blade. n q °@{еFThe PREFDFIL is the name of the preflash reference data quality file. ЛUL UTккh|г ·PREFTIME П Ъ Ў`}еla$Predicted preflash time in seconds: al┤UJ UTккh~г °PRE_AMP Р ├ Ї еPRZscaled tube pre-amp contribution: Pre-amplifier noise, in counts/seconds. Calculated by ╧ Ї@е r%the calibration software. (calhsp) lщUH UTккhАгnaPROC_TYP С ° Є БеTIRlevel of reprocessing (NORMAL, MINOR, MAJOR): If the keyword is set to MINOR the ЄБе °Uproprietary date in DADS will not be changed and the data will not be automatically a ЄБеen[distributed to the Guest Observers (GOs). If the keyword is set to MAJOR the proprietary mag ЄБеasTdate in DADS will be reset as if this were new data the data will be automatically h ( Є@Беth.distributed to the GO as if it were new data. BUF UTккhВгtePRODTYPE Т Q Ё`Геspoutput product medium type: n kUD UTккhДгPROGRMID У z ю ЕеprZA base 36 program id assigned by the pm software to a proposal that has been accepted. (1-dр┘dsсс= °HH╘Ис┌рPRHH╘И▀у■am$r @Ееec46,655 possible ids) Ї!UT UTккhЖгthPROPOSID Ф 0 ■`Зе lPEP proposal identifier: TJUR UTккhИгPR_INV_F Х Y №`ЙеOR&first name of principal investigator: sUP UTккhКг ЄPR_INV_L Ц В ·`Ле i%last name of principal investigator: aЬUN UTккhМгatPR_INV_M Ч л °`Неri*middle initial of principal investigator: ┼UL UTккhОгMA PSIZEi Ш t╘ Ў`ПеZnumber of bits allowed for the group parameter number i. This is a required FITS keyword. юUJ UTккhРгБPSTPTIME Щ ¤ Ї`СеitJyyyy.ddd:hh:mm:ss ... Predicted date and time of end of execution where: Ї`Тлm yyyy is year, Ї`УлRMddd is day of year, Е' Ї`Флoghh is hour, d 5 Ї`Хл tmm is minutes, haC Ї`Цл1-,ss is seconds.[qobservation.pred_stop_tm] с]UH UTккhЧгPSTRTIME Ъ l Є`ШеLyyyy.ddd:hh:mm:ss ... Predicted date and time of start of execution where: blz Є`Щлккyyyy is year, И Є`Ълddd is day of year, iЦ Є`ЫлUThh is hour, PRд Є`Ьлmm is minutes, st ▓ Є`Элin,ss is seconds.[qobservation.pred_strt_tm] ╠UF UTккhЮг iPTSRCFLG Ы █ Ё`ЯеP/E...HSP point source flag. щ Ё`алP = Point (default), lў Ё`блst&E = Extended.[qexposure.pt_src_flg] UD UTккhвгП PTYPEi Ь ю геheZName of the group parameter number i. This is a required FITS keyword. See the definition , ю@геСfor that group parameter name. cteFUB UTккhдг ePT_EFFIC Э U ь ее[scaled point source cathode efficiency: Point source sensitivity relative to that of the is a ьее_reference aperture, unitless. This keyword is filled by the calibration software only when ]UHm ь@ееPSthe target is a point source. dт┘daуу>f HH╘Иу┌тЩHH╘Исх■dd*ay UT UTккhжгPURGCORR Ю ■ зеSDo purge correction: YES, NO, DONE: The names of the superpurge image and its DQF red$ ■зеUTRmust be provided in the keywords PURGFILE and PURGDFIL. The scaling is obtained 0 ■@зеP 4from the keywords DARKTIME and PURGTIME. (calguide) .JUR UTккhиг_fPURGDFIL Я Y №`йе Ь!name of the purge reference DQF: hsUP UTккhкгnuPURGFILE а В · леywTSuperpurge Files (SPG): The WF/PC superpurge reference file and its associated data UTО ·леFFXquality file are used in the superpurge calibration procedure. The superpurge procedure tiЪ ·леhaYremoves residual images of highly overexposed sources. However, it creates a non-uniform ж ·леftYresidual image over the entire detector which decays with time. The level of this global ┘▓ ·леYresidual image in a readout depends upon both the time since the purge was performed and ╛ ·леUTZthe time since the last erase prior to the readout. The superpurge reference file must be ╩ ·леpe[scaled and subtracted from all images obtained after a superpurge in which the residual is and╓ ·@леliVstill significant. The PURGDFIL is the name of the purge reference data quality file. ЁUN UTккhмгиPURGTIME б ° нейWTime since last SuperPurge (seconds): The time of the observation, which was dredged л °неil_from qobservation, is used to establish the search limit. 24 hours are subtracted from the lit °не t]current observation time, and a join of qolink and qesiparm is queried to determine if any e# °неig]purge observations were taken within the previous 24 hours. If one is found, the number of e/ °неet`seconds is calculated. If none are found, the limit of 24 hours (172800 seconds) is written re; °@не b$into the keyword PURGTIME. (cgwprg) rmUUL UTккhогPXFORMT в d Ў`пеer?format of the image: NORMAL, ZOOM: (pixel size) pixel format: ╩ ·r Ў`░лsc4NORMAL: 512 samples, 512 lines 0.022x0.022 arcsec^2 upА Ў`▒л Ё3ZOOM: 512 samples, 1024 lines 0.044x0.022 arcsec^2 nt.ЪUJ UTккh▓гhePXLCORR г й Ї │еqu[split zoom-format pixels: Correct for zoom mode. If the image was taken in zoom mode, the rge╡ Ї│еti_next step is to split the data values along the first image axis (the sample direction). For es┴ Ї│е l[example, suppose the first three digital number values (DN) in the image are A, B, C. The nd ═ Ї│еndWfirst six DN values of the dezoomed image would be A/2, A/2, B/2, B/2, C/2, C/2. The ta┘ Ї│еreZlength of the first axis (NAXIS1) is doubled, and the length of the second axis (NAXIS2) х Ї@│еndremains unchanged. (calguide) UH UTккh┤гteRAD_VEL д Є ╡е kb(-300,000.,+300,000.)... radial velocity of a star the velocity of a star along the line of sight Є╡еM:[of an observer. it is calculated directly from the doppler shift in the lines of the stars 022& Є@╡е spectrum.[qtargets.radial_vel] 02@UF UTккh╢г2 RASCASCN е O Ё ╖еPXTright ascension of ascending node (revolutions): The right ascension of the line of t[ Ё╖е i]intersection of the orbital plane and the equatorial plane in the direction of the ascending tg Ё╖еsaXnode. A parameter of the flight software model of the HST orbit. See Appendix D of "HST mbs Ё@╖еth?Flight Software Examination for PCS" [wiephemeris.rt_asc_node] luedф┘A/хх? CHH╘Их┌фleHH╘Иуч■, 'e UT UTккh╕гonRA_APER ж ■ ╣еnd\right ascension of the aperture (deg): The right ascension of the reference position of the 0,$ ■╣е rXaperture used for the group data. For WFPC group data, the aperture is indicated by the M:0 ■╣еitYvalue of the group keyword DETECTOR. For other SIs the aperture is that indicated by the ╡< ■@╣е(standard header packet keyword APEROBJ. RAVUR UTккh║гRA_APER1 з e № ╗еsc\right ascension of the aperture (deg): The right ascension of the reference position of the tiq №@╗еpl+aperture specified in the APER_ID keyword. ofЛUP UTккh╝г ЁRA_APER1 и Ъ · ╜еr \right ascension of the aperture (deg): The right ascension of the reference position of the Flж ·@╜еin,aperture specified in the APERTURE keyword. └UN UTккh╛гRA_MOON й ╧ ° ┐е CYright ascension of moon in geocentric J2000.0 coordinates. The epoch is at the predicted T█ °@┐еRA/start of observation. [qobservation.rtasmoon] ofїUL UTккh└г): RA_REF к n Ў ┴еnc]right ascension of the reference target position. This is in heliocentric J2000.0. Reference , Ў┴еndYtarget is that used for target acquisition. (Not yet supported. Always same as RA_TARG.) e Ў@┴еin[qobservation.ref_obj_ra] @╣6UJ UTккh┬гde RA_SUN л dE Ї ├еUT^right ascension of sun in geocentric J2000.0 coordinates. The epoch is the predicted start of Q Ї@├еe %observation. [qobservation.rtascsun] kUH UTккh─г sRA_TARG м z Є ┼еof]Right Ascension of the target. The equinox of the target position is J2000. The epoch of the :Ж Є┼еon^target position is the predicted start time for the observation. (Fixed - Heliocentric J2000, Т Є@┼екк UTккhгerSCAN_ANG ┼ Г ш е °Y(0.,360.) position angle of scan line. When SCAN_COR (qexsco) is equal to c, this is the odъ┘ыыBatHH╘Иы┌ъctHH╘Ищэ■le)r еou_counterclockwise angle, about the beginning of the first scan, from north at the target to the le:е):Wdirection of the first scan. When SCAN_COR is equal to v, this is the counterclockwise кк е Zangle from the positive v3-axis to the direction of the first scan. (1 x 10e-4 precision) ,@е[qalignment.scan_angle] UDEUT UTккhгSASCAN_COR ╞ T ■ еsa`c/v...flag to indicate the scan coordinate frame of reference c = celestial frame (ra-dec), v = кк` ■@е Ovehicle (v2v3). Used to determine meaning of SCAN_ANG. [qalignment.scan_coord] SAzUR UTккhгSCAN_LEN ╟ Й № еsaYscan length ( 0.,3600.) in arcseconds. The length of one continuous scan or the distance iХ №@е lSbetween the first and last dwell point of the first line. [qalignment.scan_length] пUP UTккhгSCAN_RAT ╚ ╛ · е]scan rate ... the commanded constant rate of the line scan (slew of the ST optical axis from i╩ ·@еe >point a to b on the celestial sphere). [qalignment.scan_rate] фUN UTккh г):SCAN_TYP ╔ є ° еn Zc/d/n ... continuous/dwell... scan type where c = a series of linear scans alternating in ° еto^direction and offset from one another by a small angle separation (a linear scan is a slew of ° екк]the ST optical axis from point a to b on the celestial sphere at a constant commanded rate); o ° еle^d = like continuous with a specified number of dwell points per line and time to wait at each # °@ еnt8dwell point; n = not applicable. [qalignment.scan_type] =UL UTккhг lSCAN_WID ╩ L Ў еhe_scan width (0.,3600.) in arcseconds. The separation from the first to the last scan line along dweX ЎеrsSthe direction ANG_SIDE from the first scan line. Always zero when NO_LINES is one. d Ў@е. [qalignment.scan_width] e ~UJ UTккh гslSCIDATA ╦ Н Ї`е ·3science data present (T/F) (actual not predicted): e).зUH UTккhгra SCIDMP ╠ к╢ Є е Wintermediate data dump (-1 = nodump): Number of substep patterms between intermediate ine┬ Є@еng7data dumps (-1 for no intermediate dumps) SE-01p3-267 not▄UF UTккhгle SCLAMP ═ lы Ё`еewspectral calibration lamp: STUD UTккhг pSDECORR ╬ ю еe Wspectrograph de correction: Apply spectrographic detector efficiency correction. This d n юеntbcorrection is only applied to spectrographic images. It includes both the flat-field correction , юеULXand a conversion from counts to flux density. It is applied after geometric correction T8 юе tVbecause the absolute sensitivity depends on wavelength, and a major function of the D юеin[geometric correction for spectrographic images is to align the spectrum with the axes and UTP юеATZset the dispersion. The correction is applied by multiplying by a spectrogaphic detector \ юеMP_efficiency reference file. The use of an order-selecting filter can change the location of a etwh юеne]given wavelength on the photocathode, so there are several reference files; the appropriate t юе laone is selected based on the filters used. These files are full-frame (1024 x 1024), so only a А ю@еraRsubset will be used if the science image is smaller than 1024 x 1024. (calguide) dь┘nlээCapHH╘Иэ┌ьflHH╘Иыя■an&nv UT UTккhг tSDEHFILE ╧ ■ еerWSpectrographic Detector Efficiency Files (SDE): The spectrographic detector efficiency n w$ ■еaj^data files are used for the spectrographic DE calibration step. A spectrographic DE data file 0 ■е wXhas the same form as an FOC image. It always has dimensions 1024 samples by 1024 lines. y < ■еpeZEach entry is a REAL*4 scaling factor that is used to multiply the corresponding pixel DN H ■е c\count in the FOC science data file that is to be corrected. All images to be corrected will reT ■@еreJfind their proper position inside the chosen spectrographic DE data file. nUR UTккhгThSDMA3SQ ╨ } № е02S3 * (SDMEANAN**2). A value precomputed for the flight software. A parameter of the lleЙ №е. Oflight software model of the HST orbit. See Appendix D of "HST Flight Software ╘Х №@е*Examination for PCS" [wiephemeris.3sdma2] пUP UTккhгUTSDMEANAN ╤ ╛ · еW2nd derivative coef for mean anomly (revs/sec/sec): A parameter of the flight software ef╩ ·еTmodel of the HST orbit. See Appendix D of "HST Flight Software Examination for PCS" og╓ ·@еe [wiephemeris.sd_mean_anom] saЁUN UTккhгimSEMILREC ╥ ° е s\Semi-latus rectum in meters: An orbital element related to the semi-major axis. It half the ed °еorawidth of the ellipse at one of its foci. It is equal to the semi-major axis times the difference d °е c]of one minus the square of the eccentricity. A parameter of the flight software model of the i# °еURGHST orbit. See Appendix D of "HST Flight Software Examination for PCS" A v/ °@еor[wiephemeris.semilat_rect] eteIUL UTккhгSEQLINE ╙ X Ў`еl %PEP line number of defined sequence: TrUJ UTккhгSEQNAME ╘ Б Ї` еfoPEP define/use sequence name: ЫUH UTккh!гSDSERIALS ╒ к Є "е2nWserial clocks: ON, OFF: Determined by PODPS on the basis of the packet format code of ╩ ·╢ Є@"еmoTthe observation. Serial clocks are on if the packet format code = ╒68╒x. (cgwsdh) ·╨UF UTккh#г[wSGESTAR ╓ ▀ Ё $еUTAthe fgs id (f1, f2, f3) concatenated with the subdominant gs id. ы Ё@$еta[qobservation.subdominant] -maUD UTккh%гthSHTMODE ╫ ю`&е t4shutter mode: INBEAM, NOTUSED:[qexposure.shtmode] -m.UB UTккh'гe SHUTTER ╪ = ь`(еof1Shutter in place during preflash: A, B, UNKNOWN: tWU@ UTккh)гof SIMPLE ┘ tf ъ`*е%image conforms to the fits standard: АU> UTккh+гamSINEINCL ┌ dю┘erяяDULHH╘Ия┌ю ЎHH╘Иэё■ed%nc ,еYSine of the orbit inclination angle: A parameter of the flight software model of the HST D,е ЄCorbit. See Appendix D of "HST Flight Software Examination for PCS" ba @,еfo[wiephemeris.sin_orb_incl] @"9UT UTккh-гtiSKY_CORR █ H ■ .еck`sky subtraction: Subtract the sky from the object spectrum. If the sky was observed, the flat-fgT ■.еcoVfielded sky spectrum is smoothed with a median filter once and a mean filter twice---` ■.е%^except in known regions of emission lines. The spectrum is then scaled by the aperture size, l ■.еe Wand shifted so that the wavelength scales of the object and sky are matched. The sky WU@x ■.еSIWspectrum is then subtracted from the object spectra. This routine requires table ccs3 гamД ■.е`containing the filter widths, the aperture size table, ccs0, the emission line position table, Р ■.еZccs2, and the sky shift table, ccs5. This step is a spectroscopy mode calibration step. Ь ■@.еof(calguide) f t╢UR UTккh/г SLICES ▄ .┼ №`0е "number of time slices: nat▀UP UTккh1гSMMMODE ▌ ю ·`2е_oDspectrographic mirror mechanism: INBEAM,NOTUSED. [qexposure.smmode] skUN UTккh3гbtSOFTERRS ▐ °`4еru'number of "soft error" pixels (DQF=1): T ■1UL UTккh5гfiSOPNTIME ▀ @ Ў`6еh 0First shutter open time (Modified Julian Date): ■ZUJ UTккh7гexSPCLINCN р i Ї 8еliXspacecraft clock at UTC0: Value of the counter which is keeping count of the number of sou Ї8еgt\0.125 second ticks of the spacecraft clock. This value is as input from the ground. It is sБ Ї8е o]updated only after spacecraft safings and/or when the difference in spacecraft time from a Н Ї@8еre:POCC time ╘obtained from White Sands╒ is 10msec.(ETS-a) зUH UTккh9гcc SPEC_i с ╢ Є`:е. spectral element i: (i=1..4) e╨UF UTккh;г SPORDER т ▀ Ё`<е tspectral order: ∙UD UTккh=г №SP_TYPE у ю`>еlispectral type: кк"UB UTккh?г SRCHSIZE ф 1 ь`@еra(width of spiral-search in dwell points: xpKU@ UTккhAгUNSS_APER х Z ъ`Bе °1Planned (expected) entrance aperture id: APER_ID FtU> UTккhCгккSS_CAMMO ц Г ш`Dе>Planned (expected) coronographic apodizer mask: CAMMODE (cf). dЁ┘ ЇёёEecHH╘Иё┌ЁcoHH╘Ияє■ o Ї UT UTккhEг0.SS_CAMRA ч ■`Fеt /Planned (expected) camera in use: CAMERA (cf). t i2UR UTккhGг8 SS_DET ш nA №`Hеft3Planned (expected) detector in use: DETECTOR (cf). e f[UP UTккhIгSS_DETOB щ j ·`Jе W3Planned (expected) object detector: DETECTOB (cf). SPДUN UTккhKгSS_DETSK ъ У °`Lе(i0Planned (expected) sky detector: DETECTSK (cf). нUL UTккhMгtrSS_FCHNL ы ╝ Ў`NеSP.Planned (expected) first channel: FCHNL (cf). ╓UJ UTккhOг?SS_FGWA ь х Ї`Pе@/Planned (expected) disperser id: FGWA_ID (cf). KU@ UH UTккhQгSSSS_FILTi э Є`RеPl+Planned (expected) value for FILTERi (cf). D F(UF UTккhSгккSS_GRAT ю 7 Ё`TеDPlanned (expected) grating, echelle or mirror in use: GRATING (cf). QUD UTккhUгSS_LEDMO я ` ю`Vе9Planned (expected) led calibration status: LEDMODE (cf). zUB UTккhWгSS_LINES Ё Й ь`Xе 2Planned (expected) lines per frame: LINEPFM (cf). гU@ UTккhYг).SS_LOFF ё ▓ ъ`Zе ш.Planned (expected) line offset: LINEOFF (cf). ╠U> UTккh[гCTSS_MODE Є █ ш`\еSS(Planned (expected) value for MODE (cf). (eїU< UTккh]гteSS_NCHNL є ц`^екк4Planned (expected) number of channels: NCHNLS (cf). (eU: UTккh_гtoSS_NXSTP Ї - ф``еM4Planned (expected) number of x steps: NXSTEPS (cf). ecGU8 UTккhaг: SS_OPRLY ї V т`bеSS5Planned (expected) optical relay used: OPTCRLY (cf). spU6 UTккhcгSS_OPTEi Ў р`dеIL1Planned (expected) optical element used: OPTELTi ldЄ┘ккєєF HH╘Иє┌ЄecHH╘Иёї■AT f) UT UTккheгUSS_OVSCN ў ■`fеV3Planned (expected) overscan number: OVERSCAN (cf). ODE2UR UTккhgгккSS_PFILi ° A №`hе0Preflash Filter i number (0-48): PFILTERi (cf). PF[UP UTккhiгккSS_PFTIM ∙ j ·`jе3Predicted preflash time in seconds: PREFTIME (cf). ). ДUN UTккhkгCTSS_POLAR · У °`lеSS0Planned (expected) polarizer id: POLAR_ID (cf). UTнUL UTккhmгCHSS_PTSRC √ ╝ Ў`nеne9Planned (expected) HSP point source flag: PTSRCFLG (cf). к╓UJ UTккhoг SS_PXFMT № х Ї`pе(e6Planned (expected) format of the image: PXFORMT (cf). UH UTккhqг SS_SAMPS ¤ Є`rе(e3Planned (expected) samples per line: SAMPPLN (cf). кк(UF UTккhsг SS_SOFF ■ 7 Ё`tе(e0Planned (expected) sample offset: SAMPOFF (cf). QUD UTккhuгSS_SHTMO ` ю`vе/Planned (expected) shutter mode: SHTMODE (cf). zUB UTккhwгATSS_SMMMO Й ь`xеVSBPlanned (expected) spectrographic mirror mechanism: SMMMODE (cf). гU@ UTккhyгURSTATICD ▓ ъ`zе №*number of "static defect" pixels (DQF=4): ╠U> UTккh{гf)STDCFFF █ ш`|е -0=(no st dcf fill), 1=(st dcf fill present): mїU< UTккh}гTISTDCFFP ц`~еSSst dcf fill pattern (hex): еSSU: UTккhгd)STEPPATT - ф`АеULstep pattern sequence: C GU8 UTккhБгnSTEPTIME V т`Ве s1integration time at step pattern position (sec): SpU6 UTккhГгSUNANGLE р`Деor4angle between sun and V1 axis (deg): Computed as: SSdЇ┘PlїїGesHH╘Иї┌ЇHH╘Иєў■t'Pl`Елam,sunangle = cosd(declnsun) * cosd(declnv1) * Жл ю-cosd(rtascsun - rtascnv1)+ (sind(declnsun) * d"@Жлsind(declnv1)) гAT0`Зл ь'sunangle = acosd (sunangle)(cgaang) troIUT UTккhИгhaSUN_ALT X ■ Йеy`altitude of the sun above Earth╒s limb (deg): The algorithm calculates the altitude using the {d ■Йе ]rectangular coordinates of HST and the coordinates of the sun from the SHP header. For a Fp ■Йе\long exposure, this wouldn╒t be as useful as, say, the maximum altitude of the sun during UL| ■Йеue\the exposure. The other problem of this algorithm is that it assumes a spherical earth, teИ ■Йе S`which results in an error of about 0.4 degrees. Another effect is that it ignores atmospheric mpФ ■Йеarefraction. This will be very small at high altitudes but can be as large as one degree near а ■@Йеўthe horizon. (cgasun) ║UR UTккhКгsuSURFALTD ╔ № ЛеlnJplanetographic coordinate system parameters: altitude of surface feature. ╒ №@Ле[qobservation.feature_alt] яUP UTккhМг =SURFLATD ■ · НеUTJplanetographic coordinate system parameters: latitude of surface feature. ·@Неde[qobservation.feature_lat] s t$UN UTккhОгthSURFLONG 3 ° ПеlaKplanetographic coordinate system parameters: longitude of surface feature.For? °@ПеЙ[qobservation.feature_long] dnYUL UTккhРг, SURF_B mh Ў`Се sexpected B surface brightness: \thВUJ UTккhТгhe SURF_R tС Ї`Уеhaexpected R surface brightness: teлUH UTккhФг S SURF_U ║ Є`Хеutexpected U surface brightness: th╘UF UTккhЦгsp SURF_V у Ё`Чеacexpected V surface brightness: t h¤UD UTккhШгcaT51_ANGL ю Ще Yposition angle of motion of aperture (deg): This parameter is determined only for moving юЩеraRtargets (TARGET_TYPE=M). The position angle in degrees from North towards East of $ юЩеat[the angular velocity which is arctan( a_E, a_N ) converted to degrees. (cect51) [a_N, a_E: te 0 ю@Ще l3angular velocity in the North and East directions] bseJUB UTккhЪгt]T51_RATE Y ь ЫеUrate of motion commanded (arcsecs/sec): This parameter is determined only for moving fe ьЫе °Ptargets (TARGET_TYPE=M). The magnitude of the angular velocity is sqrt(a_N**2 + mq ьЫе s[a_E**2) [a_N, a_E: angular velocity in the North and East directions] times the conversion ex} ь@Ыеri,factor from radians to arcseconds. (cect51) dЎ┘urўўHUFHH╘Иў┌Ў ЁHH╘Иї∙■tn) h UT UTккhЬгcaTARAQMOD ■`Эе H(00-03)...the target acquisition mode used for the observation. Where: o& ■`Юл ю00 = null, еra4 ■`ЯлTY01 = ground assisted, B ■`алNo 02 = onboard computer assisted, ЩP ■`блve803 = fixed simple pointing.[qobservation.target_acqmd] cejUR UTккhвгe TARDESCR y № геci^target description: The Target Description will be one of the key fields used by archival Е №геomWresearchers in searching through the HST data archive; thus it is important that the PtaС №ге=M\information be filled out completely and accurately for each target, and following a well-, Э №геitZdefined format. Each target should be assigned one and only one Target Category. This й №геco^should be followed by as many Target Keywords (at least one is required) as are relevant. ╡ №@ге(PROP_INST--SEC_5.TEX;1) ∙╧UP UTккhдг hTARGCAT ▐ ·`ееtarget category: ь ·`жлrgSTAR Galactic stellar object e· · злe:.STAR CLUSTER Galactic star cluster, group, or ·@зл gassociation , ·`илNo)INTERSTELLAR MEDIUM Galactic gas or dust " ·`йл f$EXT-STAR Star in an external galaxy rg0 ·`клUT/EXT-CLUSTER Star cluster in an external galaxy ^ta> ·`лл 5EXT-MEDIUM Interstellar medium in an external galaxy eL ·`мл №GALAXY Galaxy, AGN, or QSO inZ ·`нл t,GALAXY CLUSTER Cluster or group of galaxies ath ·`ол(PROP_INST--SEC_5.TEX;1) lВUN UTккhпг aTARGDIST С ° ░еnd[distance to target from Earth╒s center (km): This parameter is determined only for moving e aЭ °░е CWtargets (TARGET_TYPE=M). This is calculated using the time of the observation and the easй °░еd)_Chebychev coefficients for that target. The software determines the geocentric position data ╡ °░ее]for position (3-vector in kilometers) and velocity (3-vector in kilometers per second). The :┴ °@░еac>target distance is the norm of the position vector. (cect51) █UL UTккh▒гNoTARGNAME ъ Ў`▓е oproposer╒s target name: fUJ UTккh│г aTARKEYi Ї`┤екTtarget key description number i: (i=1..10) Key description entered by the proposer. UM-UH UTккh╡гumTAR_TYPE < Є`╢е/P/A/M/G/I.....specifies the target type where J Є`╖лLUP = point target, X Є`╕л ·A = area target, Pf Є`╣лX;G = generic target, at Є`║л °*M = moving target.[qtargets.target_type] d°┘ i∙∙ImoHH╘И∙┌°etHH╘Иў√■ng*im UT UTккh╗гonTECTEMP ■`╝еChTEC temperature (Celcius): t t2UR UTккh╜гe THRESH gA №`╛еn PPAD (Pulse Amplitude Discriminator) threshold setting for the object detector: (3[UP UTккh┐гerTIME-OBS j · └е░UUT time of start of observation (hh:mm:ss): PODPS calcuted time using packet times ov ·└е ЎZgenerated at the spacecraft at the time of the data measurement. The seconds place is not В ·└еey`always accurate as the fractions of a section information is discarded rather than used for TAО ·└еRrounding. (ETS-d) FOS: merely the FPKTIME translated from MJD (keeping only whole Ъ ·└е, Wseconds) see EXPSTART for relation to shutter opening. (ETS-d) WFPC: Note that this is ж ·└еmo[not necessarily the start of the exposure. For example, the WFPC observation starts on a mo▓ ·└е┌Ymajor frame pulse, while the exposure actually starts 16.4 seconds later following a E╛ ·@└еmemory clear. See EXPSTART. (C╪UN UTккh┴гUTTIMEBIAS ч ° ┬е]instrument time bias (in 1/1.024 microseconds): The value of the time biases that is used to 3є °┬еeracorrect the integration time for internal instrument delays. The timebias is a function of the t °┬еimPparticular HSP data format (BYTE, WORD, LWRD, ALOG, or ALL) and the instrument ur °@┬е p)mode (SCP, ARS, SSP1, or SSP2). (cgptme) a%UL UTккh├гctTIMEFFEC 4 Ў ─еisXThe time the parameters took effect onboard; given in the form of the number of seconds KT@ Ў@─еm (since 1/1/85. [wiephemeris.time_effect] , ZUJ UTккh┼гSTTRAILER i Ї`╞еg.reject array exists: tГUH UTккh╟гTRK_TYPE Т Є ╚еstXtrack 48 or track 51 commanding used (T48, T51, NO): Specifies the ST pointing mode. If ┌Ю Є╚еls\the pointing mode is track48 or track 51, the target must be a moving target. Track 51 mode meк Є╚еPS[is a single uninterruptable profiled slew command which tracks along a great circle. Track 1.0╢ Є╚еS48 is the secondary motion command which can follow more complicated motions using tio┬ Є@╚еal?fourth degree polynomials. [qalignment.pointing_mode] (cecqal) ▄UF UTккh╔гarTRUE_CNT ы Ё ╩е, Ycompute the true count rates: Compute the true count rates. This switch applies only to cў Ё╩екк\digital data, it has no effect on analog data. True counts are corrected according to the en Ё@╩еe following equation: Ў Ё`╦лsiz = (y-d-e)/(h*r) Ё`╠л, Where: кк- Ё`═л+z is the final calibrated true count rate, : t; Ё`╬лy is the observed count rate, I Ё`╧лtrd is the dark signal, W Ё`╨лcie is the pre-amplifier noise, e Ё`╤лls"h is the high-voltage factor, and s Ё`╥л mr is the relative sensitivity. modБ Ё ╙л╚8If the target is an extended source (i.e., the value of icd·┘ck√√JHH╘И√┌·ndHH╘И∙¤■ u+io╙лal;the header keyword PTSRCFLG is "E"), z is further divided al)@╙л╔"by the aperture area. (calguide) -UT UTккh╘гtrTRUE_PHC < ■ ╒еcoZcompute the true photocurrents: Compute the true photocurrents. This switch applies only H ■╒еTr\to analog data, it has no effect on digital data. True photocurrents are corrected by the T ■@╒е(yfollowing equation: b ■`╓лккz = ((y-i)/g - d - e)/(h*r) fp ■`╫лueWhere: e,~ ■`╪л╬+z is the final calibrated true count rate, М ■`┘л d"y is the observed digital number, Ъ ■`┌лeri is the CVC offset, ╤и ■`█лh-g is the gain factor, ╢ ■`▄лr d is the dark signal, ─ ■`▌лe is the pre-amplifier noise, ╥ ■`▐л.,"h is the high-voltage factor, and р ■`▀лr is the relative sensitivity. Ию ■ рлnd8If the target is an extended source (i.e., the value of · ■рлhe;the header keyword PTSRCFLG is "E"), z is further divided ■@рлhe"by the aperture area. (calguide) UR UTккhсг_PTUBEGAIN! / № теutZscaled tube gain factor: Gain factor used to convert digital numbers (DN) in the analog ; №теnaZmode to count rates, in DN/(counts/second). This keyword is filled by the calibration G №@теfo.software only for analog data files. (calhsp) aUP UTккhуг*rUNICORR " p · феe,_uniform de correction: Flat field correction (normal images only). This correction is called e o| ·феmb]the uniform detector efficiency correction, and it is applied by multiplying by the uniform ■И ·феd ^detector efficiency reference file, which is the reciprocal of a flat field. These reference Ф ·феe [files are full-frame in size, which is 1024 x 1024 because we have dezoomed. As with the theа ·феnd^dark-count correction, if the science image is smaller than full-frame then only a subset of м ·@фе'the reference file is used. (calguide) a. ╞UN UTккhхгUTUNIHFILE# ╒ ° цеVUniform Detector Efficiency Files (UNI): The uniform Detector Efficiency (DE) files---с °це №Walso known as relative detector efficiency files---contain data used to remove the FOC thэ °це №[instrument╒s spatial non-uniformities from the FOC science data. This step is known as the ∙ °цефWuniform DE calibration. A uniform DE file has the same form as an FOC image. It always is °цеVhas dimensions 1024 samples by 1024 lines. Each entry is a REAL*4 scaling factor used °це ■Xto multiply the corresponding pixel DN count in the FOC science data file that is to be at °@цеrecorrected. 7UL UTккhчгe UNITAB $ sF Ў`ше2table of relative detective efficiency filenames: `UJ UTккhщгdaUTC0 % ecto Ї ъеe TCoordinated Universal Time (Modified Julian Date): This value is as input from the re{ Їъе(c^ground, it is updated only after spacecraft safings and/or when the difference in spacecraft d№┘r ¤¤K--HH╘И¤┌№s HH╘И√ ■in(usъеOCWtime from a POCC time ╘obtained from White Sands╒ is 10msec. (ETS-a) (UTC02 * 2**32 . TъеasW+ UTC01) give the decimal value of the VAX 64 bit time format which, when translated, as ъеalWgives the reference UTC0 in MJD of the spacecraft clock. i.e. UTC when the spacecraft REA,@ъе u$clock read SPLINCN ticks. (ETS-c) thEUT UTккhыгxeUTCO1 & thT ■`ье fbytes 5-8 of UTC0: °nUR UTккhэгcoUTCO2 ' UL} № юеUN`bytes 1-4 of UTC0: Decimal representation of bits 1-4, using a place value for each bit as if щЙ №@юеctKthey were bits 5-8. i.e, the given value is really UTC02 / 2**32. (ETS-d) s vгUP UTккhягroV2APERCE( ▓ · ЁеndWV2 offset of target from aper. center (arcsec): The X component of the aperture offset ╛ ·Ёе\position in the ST coordinate system. The V2 offset of the target from the aperture center. ╩ ·@Ёеin[qobservation.v2v3_xcoord] WtiфUN UTккhёгmeV3APERCE) є ° Єе0mWV3 offset of target from aper. center (arcsec): The Y component of the aperture offset the °Єеfo\position in the ST coordinate system. The V3 offset of the target from the aperture center. sp °@Єеe.[qobservation.v2v3_ycoord] ,%UL UTккhєгclVAC_CORR* 4 Ў Їеth\vacuum to air correction: Apply vacuum-to-air correction to the wavelengths. This routine э@ Ў@ЇеULQconverts vacuum wavelengths to air wavelengths above 2000 Angstroms. (calguide) ZUJ UTккhїгeaVDATAFMT+ i Ї`Ўеct Format of current observation: enw Ї`ўлTC 1: byte, Е Ї`°лUT 2: word, oУ Ї`∙л · 3: longword, dб Ї`·лge 4: analog п Ї`√лTh7: all nen╔UH UTккh№гofVELABBRA, ╪ Є ¤еti^aberration in position of the target: Magnitude of aberration due to ST and earth velocities. ф Є¤еse]This is the absolute angular correction that must be applied to the apparent position of the tЁ Є¤еenStarget as seen from the ST to compensate for the velocity of the ST and the earth. n i№ Є@¤еe [qobservation.velabbra] heUF UTккh■гpeVELOCSTX- % Ё еe.\velocity of space telescope along the x axis (km/sec): X component of the velocity of space um1 Ё е: Xtelescope in geocentric J2000,0 inertial coordinates. This is a orthogonal right handed co= Ё еleUcoordinate system centered in the earth, with the X axis pointing towards the vernal FI Ё е]equinox for the year 2000, the Z axis pointing towards the north celestial pole for the year TU Ё@ еA2000, and the Y axis orthogonal to both. [qobservation.velocstx] oUD UTккhгllVELOCSTY. ~ ю е\velocity of space telescope along the y axis (km/sec): Y component of the velocity of space Sd■┘ LabHH╘И ┌■t HH╘И¤■ t'еetXtelescope in geocentric J2000,0 inertial coordinates. This is a orthogonal right handed еatUcoordinate system centered in the earth, with the X axis pointing towards the vernal p еg ]equinox for the year 2000, the Z axis pointing towards the north celestial pole for the year g,@еinA2000, and the Y axis orthogonal to both. [qobservation.velocsty] EUT UTккhгteVELOCSTZ/ T ■ еh \velocity of space telescope along the z axis (km/sec): Z component of the velocity of space a` ■еdsXtelescope in geocentric J2000,0 inertial coordinates. This is a orthogonal right handed nal ■еvaUcoordinate system centered in the earth, with the X axis pointing towards the vernal px ■еg ]equinox for the year 2000, the Z axis pointing towards the north celestial pole for the year Д ■@еA2000, and the Y axis orthogonal to both. [qobservation.velocstz] ЮUR UTккhгVFAPVECX0 н № еe WVector pointing from the desired position of the candidate to the home position of the ╣ №еte_image. The vector is set by the user with a default of 0. It can be used to point from a small ]eq┼ №@е 2Lobserving aperture to the center of the finding aperture image. (norton.51) ▀UP UTккhг, VFAPVECY1 ю · е [WVector pointing from the desired position of the candidate to the home position of the y o· ·еal_image. The vector is set by the user with a default of 0. It can be used to point from a small n g ·@еinLobserving aperture to the center of the finding aperture image. (norton.51) co UN UTккhгntVFCENVEX2 / ° е p_Vector from the coarse target to the target centroid. The vector points from the coarse target tow; °@ еesEto the centroid of the target╒s individual measurements. (norton.52) oUUL UTккh гbsVFCENVEY3 d Ў е_Vector from the coarse target to the target centroid. The vector points from the coarse target atep Ў@еioEto the centroid of the target╒s individual measurements. (norton.52) wКUJ UTккhг. VFCTVECX4 Щ Ї еll\Vector from the center of the finder image to the coarse target. The vector points from the toе Ї еккWcenter of the finding aperture image to the row and column representing the candidate. f t▒ Ї@ е(norton.51) of╦UH UTккhгVFCTVECY5 ┌ Є е b\Vector from the center of the finder image to the coarse target. The vector points from the obц Єеo Wcenter of the finding aperture image to the row and column representing the candidate. Є Є@е p(norton.51) thUF UTккhг tVFFTVECX6 Ё еnt[Vector from the center of the finder image to the target centroid. This is the fine target mea' Ё@е.5Avector, representing the sum of VFCENVE and VFCTVEC. (norton.52) rAUD UTккhгarVFFTVECY7 P ю еct[Vector from the center of the finder image to the target centroid. This is the fine target ivi\ ю@е (Avector, representing the sum of VFCENVE and VFCTVEC. (norton.52) lvUB UTккhгceVFOBJCNT8 d┘ vMtoHH╘И┌e HH╘И ■mn&se еe.Mcount of trg obj: Gives the total number (in the range between VFLOFLIM and ЄеVe\VFHIFLIM) of Target Acquisition and Verification objects found. Only the brightest 20 are Є @еceBsaved, although this count could exceed that number. (norton.50) 9UT UTккhг VFOCUS 9 H ■`еthfocus of the object detector: bUR UTккhгVFOCUSn : q №`еe focus n: n=1..4 e ЛUP UTккhгhiVFOCUSD ; Ъ · еUfocus command value for object detector: Equivalent to VFOCUSDn for when the object кж ·@еdetector=n. (cgpulk) t└UN UTккhгceVFOCUSDn< ╧ ° еrgTfocus command value for detector n: n=1..4 Sets the 12bit DAC which determines the s█ °@еVFLinitial focus for the image dissector tube deflection current. (norton.36) їUL UTккhгVFPFACTX= Ў е┌ZTarget Acquisition and Verification vector conversion factors. These constants define the ЎеYconversion between the TAV image scale and the scale of the image projected by the Space Ў@е a3Telescope on the face of the detector. (norton.47) ar6UJ UTккh гVFPFACTY> E Ї !еouZTarget Acquisition and Verification vector conversion factors. These constants define the Q Ї!еecYconversion between the TAV image scale and the scale of the image projected by the Space P] Ї@!еVF3Telescope on the face of the detector. (norton.47) fowUH UTккh"г VFSLWVEX? Ж Є #еe [X component of the slew vector for Target Acquisition and Verification. This is the vector Т Є#еs Sissued as a slew request. It represents the vector sum of VFFTVEC and VFAPVEC, and Ю Є#еiaUpoints from the desired observing aperture to the centroid of the target╒s inidivual к Є@#е measurements. (norton.52) ─UF UTккh$гerVFSLWVEY@ ╙ Ё %еs.[Y component of the slew vector for Target Acquisition and Verification. This is the vector the▀ Ё%еe Sissued as a slew request. It represents the vector sum of VFFTVEC and VFAPVEC, and (noы Ё%еUTUpoints from the desired observing aperture to the centroid of the target╒s inidivual eў Ё@%еctmeasurements. (norton.52) UD UTккh&г!VFTAVERRA ю`'еma8TAV (Target Acquisition and Verification) error status: P:UB UTккh(гVF VGAIND B tI ь`)еecTgain setting: Gain setting of the object or sky depending on data source. (cgpsdh) encU@ UTккh*гorVGAINDn C r ъ +еca^gain setting of detector n: n=1..5 Sets the value of the full-scale gain of the CVC (Current ~ ъ@+еC 7to Voltage Converter) Full scale values allowed are: ded┘ntNniHH╘И┌urHH╘И■VF)`,л%0: 1 nanoamp; `-л Ў2: 10 nanoamps; it$`.лon3: 100 nanoamps; r2`/л%6: 1 microamp; sl@`0лre7: 10 microamps; mN`1лAP(norton.36) ЁgUT UTккh2гpoVGAINDS D v ■`3еer/gain setting of detector "sky": See VGAINDn. ў ЁРUR UTккh4гmeVHDEFLn E Я №`5екк horizontal deflection n: n=1..4 ╣UP UTккh6гge VHORIZ F n╚ · 7еroYhorizontal deflection (command value) of the object detector: Equivalent to VHORIZn for e╘ ·@7еt %when the object detector=n. (cgpulk) hюUN UTккh8г*VHORIZn G ¤ ° 9е+^Horizontal deflection for detector n: n=1..4 Sets the 12bit DAC which determines the initial °@9е+Ahorizontal image dissector tube deflection current. (norton.35) #UL UTккh:гVHORSTPTH 2 Ў ;еni[no. of horiz steps/spatial point in area scans: Deflection steps correspond to about 4.42 > Ў;е n^microns on the face of the image dissector tube. If the incrementing process (starting with J Ў;е m_the initial deflection) causes the deflection value to exceed the 12-bit capacity (4096), the ккV Ў@;е4counter wraps and starts over at zero. (Norton.33) y"pUJ UTккh<г ЁVHPOINTSI Ї`=е -no. of horiz points (columns) in area scans: nЩUH UTккh>гккVIGHFILEJ и Є ?еKVignetting Files (VIG): The removal of vignetting and wavelength-dependent val┤ Є?е e\photocathode variations is done using data from the vignetting files. Vignetting correction └ Є?е+Tfiles contain multiple groups of responses. Each group contains the responses for a e ╠ Є?е\particular carrousel position and line position. Within the group, responses are ordered by ╪ Є?е ЎQequally spaced sample positions determined by the keywords, SAMPBEG and SAMPOFF. ф Є@?еt JData in the vignetting correction data files are stored in REAL*4 format. ■UF UTккh@гntVIG_CORRK Ё AеQremoval of vignetting nonuniformity: Remove vignetting and wavelength-dependent - ЁAе),[photocathode variations by dividing each count value by the vignetting response contained кк% ЁAеZin the vighfile file. This routine removes the vignetting and low frequency photcathode 1 ЁAе ЄYresponse using a reference file that has a vignetting map. This map is has a vignetting t= ЁAе?Vvector for multiple line position and carrousel positions. At each line position the I ЁAе^granularity is tabulated with a constant starting sample for all lines and a constant delta U ЁAе?]sample. To compute the response for the data╒s line and sample, tri-linear interpolation is ba ЁAе?_used within the reference file over carrousel position, line position and sample position. If m ЁAеthVDoppler compensation is specified, the response is smoothed by a weighting function y Ё@AеNdescribing the motion of the data samples along the photocathode. (calguide) d┘),OonHH╘И┌ tHH╘И■%A UT UTккhBгfiVNOINTPTL ■ Cеvi_no. of integrations/pt in area scans: Number of integrations to be done at each of the points t h$ ■@Cеp._in an area scan. the default value for this parameter after initialization is 1. (norton.33) ous>UR UTккhDгacVOFFn M n M №`EеA vertical offset bin n+1: n=1..6 thgUP UTккhFгngVREQDET N v ·`Gеnt0requested detector for the object observation: heД ·`Hлda!1: IDT1 (Image Dissector Tube 1) nТ ·`Iл Ё!2: IDT2 (Image Dissector Tube 2) eа ·`Jлc!3: IDT3 (Image Dissector Tube 3) dо ·`KлIf!4: IDT4 (Image Dissector Tube 4) c╝ ·`Lлci5: PMT (Photomultiplier) h╓UN UTккhMгfVSKYDET O х °`Nеri"currently selected sky detector: є °`Oлth!1: IDT1 (Image Dissector Tube 1) ┘ °`Pл!2: IDT2 (Image Dissector Tube 2) °`Qл t!3: IDT3 (Image Dissector Tube 3) °`RлUT!4: IDT4 (Image Dissector Tube 4) ■+ °`Sлno5: PMT (Photomultiplier) aEUL UTккhTг iVVERSTPTP T Ў UеthYno. of vert. steps/spatial pt. in area scans: Deflection steps correspond to about 4.42 t` ЎUеi^microns on the face of the image dissector tube. If the incrementing process (starting with l ЎUеUP_the initial deflection) causes the deflection value to exceed the 12-bit capacity (4096), the on:x Ў@UеH4counter wraps and starts over at zero. (Norton.33) IТUJ UTккhVгgeVVERT Q e б Ї WеJVvertical deflection (command value) of the object detector: Equivalent to VVERTn for н Ї@Wе%when the object detector=n. (cgpulk) N╟UH UTккhXгVS VVERTn R °╓ Є Yеcu\Vertical deflection for detector n: n=1..4 Sets the 12bit DAC which determines the initial т Є@YеDT?vertical image dissector tube deflection current. (norton.35) Dis№UF UTккhZг °VVPOINTSS Ё`[еis-no. of vertical points (rows) in area scans: h%UD UTккh\гUL VXMOON T i4 ю`]е Ў'Moon velocity: geocentric J2000 frame: ialNUB UTккh^г: VXSUN U ep] ь`_еou&Sun velocity: geocentric J2000 frame: wU@ UTккh`гim VYMOON V ud┘stPHH╘И┌caHH╘И ■2-%pa`aеn:'Moon velocity: geocentric J2000 frame: sta!UT UTккhbг(NVYSUN W UJ0 ■`cеVV&Sun velocity: geocentric J2000 frame: JUR UTккhdгma VZMOON X eY №`eеE'Moon velocity: geocentric J2000 frame: еsUP UTккhfг ЎVZSUN Y ulВ ·`gеX&Sun velocity: geocentric J2000 frame: ЬUN UTккhhгioWAVCORR Z л ° iе 1\compute photometric parameters: Compute the absolute sensitivity. This does not affect the ef╖ °iеnoYdata values. The inverse sensitivity, pivot wavelength, and RMS bandwidth are computed s├ °iеanPand stored in the header of the output image. The zero-point magnitude and the nt╧ °iеalNobservation mode are also saved in the output header. See keywords PHOTMODE, █ °@iеU@0PHOTFLAM, PHOTZPT, PHOTPLAM, PHOTBW. (calguide) ┘їUL UTккhjгWAV_CORR[ Ў kеWwavelength scale generation: Compute a vacuum wavelength scale for each object or sky еn: ЎkеeoVspectrum. Wavelengths are computed using coefficients stored in table ccs6. This is Ўkе J[computed differently for the gratings and for the prism. This step is a spectroscopy mode ic ( Ў@kеUPcalibration step. (calguide) lBUJ UTккhlгXWBLDASNR\ Q Ї`mеra"Blade A sensor: 0:closed, 1:open: kUH UTккhnгiWBLDBSNR] z Є`oеrs"Blade B sensor: 0:closed, 1:open: ФUF UTккhpгecWCANLTIM^ г Ё qе vYtime of cancel operation command: To obtain control of the exposure, a Cancel Operation п ЁqеstWCommand is issued to the instrument a minimum of 16.525 seconds after the initiating i╗ ЁqеmoWmajor frame pulse. The spacecraft time (in the same format as for WEXPOTIM) is stored TFL╟ Ё@qеLAin WCANLTIM. (norton.22) LсUD UTккhrгWAWEXPOCMD_ Ё ю`sеwaexpose command image: UB UTккhtгumWEXPODUR` ь`uеor*Commanded duration of exposure (seconds): 3U@ UTккhvгteWEXPOTIMa B ъ wеleZMajor frame pulse time preceding exposure start (cnts): Decimal representation of the 16 N ъwе s]low order bits (lsb) of the time tag given by the spacecraft to the major frame pulse (mfp) BZ ъ@wе0preceding the start of a WFPC exposure. (ETS-c) UHtU> UTккhxгWBWEXPTMHIb Г ш yеBlZmajor frame pulse time preceding exp start (cnts): Decimal representation of the 16 high d┘o QexHH╘И ┌HH╘И■st( ayе sXorder bits (Msb) of the time tag given by the spacecraft to the major frame pulse (mfp) meyеma^preceding the start of a WFPC exposure. (but using a place value for each bit as if they were yе Plsb!. i.e, the given value is really WEXPTMHI/2**16) Spacecraft clock at mfp = ь,@yеCo$(WEXPTMHI*2**16 + WEXPOTIM) (ETS-c) : EUT UTккhzгteWFCSTAT c T ■`{еle#control/status word for exposure: posb ■ |лD00 if nominal WFPC microprocessor control of the sn ■@|лls shutters. | ■ }лhe81 if NSCC-1 controlled the shutters. (generally meaning wИ ■@}лe "an interrupted exposure.)(ETS-c) вUR UTккh~гWBWFOCTMnnd ▒ № еBlWtime of nnth open or close of B shutter: nn=1..15 Telemetered values to determine the gh ╜ №@е┘Zactual exposure time nn=odd: Time of shutter closing; nn=even: Time of shutter opening. ╫UP UTккhАгWORDS e aц ·`Бе s'number of HSP words samples in a line: by UN UTккhВгthWRD11_14f ° ГеXword 11/14 ... A number assigned by sms for each observation. the word 11/14 is a count t °ГеYwhich is kept for each instrument and updated for each observation using the instrument. ' °@Ге:The count rolls over every 255.[qobservation.word_11_14] AUL UTккhДг WSCALE g P Ў`ЕеstScale factor for output image: jUJ UTккhЖг nWTIMEXPOh y Ї Зе oTtime of 110 msec expose command: As its last action at the end of an exposure, the heЕ ЇЗеllKWFSHCON command is executed. That command generates a 110 msec Executable ккС ЇЗеYExposure Command to reset the WF/PC microprocessor╒s shutter control logic, as well as lЭ ЇЗеheQto initiate the CCD readout. The spacecraft time of this command is recorded in nй Ї@ЗеttWTIMEXPO. (norton.22) ├UH UTккhИгeWWCANCM i ╥ Є Йеf Ucancel operation command bit: To obtain control of the exposure, a Cancel Operation ▐ ЄЙе nWCommand is issued to the instrument a minimum of 16.525 seconds after the initiating еъ ЄЙеr Wmajor frame pulse. The spacecraft time (in the same format as for WEXPOTIM) is stored еЎ Є@Йеov5in WCANLTIM and the bit WWCANCM is set. (norton.22) ДUF UTккhКг WWLOGOF j Ё Ле f\log overflow bit: The spacecraft times for the WFPC shutter opens and closes are recorded e+ ЁЛе iXin the telemetered fields WFOCTMnn. However, only the first 8 ╒close╒ commands ( and 7 ex7 ЁЛеndZadditional ╒open╒ commands) can be accomodated in the SHP. If more activity occurs, the C ЁЛеs Ysubsequent times are not recorded, but the WWLOGOF flag is set to indicate that the log sO Ё@Леthoverflowed. (norton.22) niUD UTккhМгtt WWSCAP k rx ю Неккdshutter control application processor bit: This bit is set if, as its last action at the end of an exd ┘RiHH╘И┌ umHH╘И ■"Неr Pexposure, the WFSHCON command was executed. That command generates a 110 msec НеovQExecutable Exposure Command to reset the WF/PC microprocessor╒s shutter control O @Не UTккhдгe:YDATALIMw # ш`ее high byte of acquisition limit: al=U< UTккhжгUNYDEAD x L ц зе °Xaccum close time: The accumulator "close time" (interval during which the accumulator vaX ц@зеflNcounting is disabled) is specified in units of 7.8125 microsecs. (norton.35) rU: UTккhигxpYDEF y █ °Б ф`йеtivertical deflection: nd┘ SntHH╘И ┌ШHH╘И■X-!ti UT UTккhкгio YINTEG z к ■ ле Wnumber of integrations/X-step: The number of integrations controls the number of open/FFS$ ■ле^close time pairs of FOS Analog Signal Processor samples of the output from the rate limiter 0 ■@леt Cthat are done with no changes in magnetic deflection. (norton.34) JUR UTккhмгisYLINSFRM{ Y №`неpackets per frame: sUP UTккhог( YLIVE | дВ · пе Vaccum open time: The accumulator "open time" (interval during which the accumulator О ·@пезMcounting is enabled) is specified in units of 7.8125 microsecs. (norton.34) eиUN UTккh░г цYMCLEARS} ╖ °`▒еbl memory clears/data acquisition: 5 ╤UL UTккh▓гn.YMOON ~ ккр Ў`│е 'Moon position: geocentric J2000 frame: tio·UJ UTккh┤гYMSLICES Ї`╡еnumber of memory slices: ┌#UH UTккh╢гYNOISELMА 2 Є`╖еburst noise rejection limit: oLUF UTккh╕г ■YNUMCHNLБ [ Ё`╣еat$number of channels to be processed: nsuUD UTккh║гerYOVRSCANВ Д ю`╗еclX-deflection overscan: aloЮUB UTккh╝г s YPITCH Г uн ь`╜еe #Y-deflection pitch between diodes: e d╟U@ UTккh╛гs YPOS Д def╓ ъ`┐е4)y-position on photocathode: SFЁU> UTккh└г YPTRNS Е t ш`┴еUPpatterns per readout: U< UTккh┬г YRANGE Ж ( ц`├еcu Y range: eBU: UTккh─гduYREADCYCЗ Q ф`┼еreadouts/memory clear: enkU8 UTккh╞гd YSPACE И 1z т`╟еrtyrange * 32 / ysteps: d┘▒TtaHH╘И┌n.HH╘И ■ p n: UT UTккh╚гfr YSTEP1 Й T ■`╔еIC+first ystep data type: OBJ, SKY, BCK, NUL: y s2UR UTккh╩гкк YSTEP2 К EA №`╦е,second ystep data type: OBJ, SKY, BCK, NUL: UT[UP UTккh╠гCH YSTEP3 Л j ·`═еer+third ystep data type: OBJ, SKY, BCK, NUL: h║ДUN UTккh╬г YSTEPS М ╗У °`╧е onumber of y steps: ккнUL UTккh╨гГYSUN Н ╝ Ў`╤еti&Sun position: geocentric J2000 frame: ╓UJ UTккh╥г YTYPE О х Ї`╙еon!observation type: OBJ, SKY, BCK: └ UH UTккh╘г tYWRDSLINП Є`╒е rwords per line: кк(UF UTккh╓гЖ YXBASE Р 7 Ё`╫е eX-deflection base: YRQUD UTккh╪гYXPITCH С ` ю`┘еr:"X-deflection pitch between diode: zUB UTккh┌г╟YXSTEPS Т Й ь`█еX-deflection sub-steps: ▒гU@ UTккh▄гYXYDFTMPУ ▓ ъ`▌еXY-deflection focus: ╠U> UTккh▐г YYBASE Ф T█ ш`▀еYSY-deflection base: їU< UTккhргte YYPATH Х J ц`се spath identification: SU: UTккhтгYYPITCH Ц - ф`уеpeY-deflection pitch: UTGU8 UTккhфгCHYYSTEPS Ч V т`хеerY-deflection sub-steps: BJpU6 UTккhцг║Y_OFFSETШ р`че ╗'y_offset for GIMP correction (diodes): ккd┘USuHH╘И┌: HH╘И■$╙ UT UTккhшгtyZACMODE1Щ ■`ще╘acquisition mode: Є& ■`ълwo0: spectral science data к4 ■`ылР1: focus diode field map -B ■`ьлYR3: single frame P ■`эл ю(SO-01p3-424) jUR UTккhюгchZDOPMAG Ъ y №`яе╟QOCT (Observation Control Table) doppler shift correction magnitude: See DOPMAG УUP UTккhЁг ъ ZFLUXM Ы в · ёеcuQflux measurement at end of targ. acq. obs.: The flux measurement, taken through о ·ёеteVwhichever aperture (large or small), contains the target at the very end of a target ║ ·ёе]acquisition observation. As the last (and always executable) phase of a target acquisition l╞ ·ёеBJOobservation, one more frame of data is obtained from the instrument. The flux cti╥ ·@ёеWmeasurement is the sum of the counts of the 8 target acquisition diodes. SO-01p3-262. : ьUN UTккhЄгZFSPYBF Ь √ °`єеUT&control bits for spectrum y-balance: °`Їлis,1: Spectrum y balance offset should be used ra °`їл ■02: Spectrum y balance offset should be computed 1UL UTккhЎгinZFXMAPC Э @ Ў`ўе(S)x deflection of the center of field map: ZUJ UTккh°гяZFYMAPC Ю i Ї`∙еle)y deflection of the center of field map: ГUH UTккh·гккZINTPER Я Т Є √еXOCT (Observation Control Table) integration period (number of 50 ms slices): Number of Ю Є√еteW50ms blocks accumulated internally to produce 1 line of science data (1-255). SE-01p3-║ ·к Є@√еac266. o─UF UTккh№г tZLCOEF1 а ╙ Ё`¤еasline mapping function L0: эUD UTккh■гBJZLCOEF2 б № ю` еatline mapping function A: tUB UTккhгtiZMOON в ё% ь`еis'Moon position: geocentric J2000 frame: cqu?U@ UTккhг-0ZSCOEF1 г N ъ`еZF%first coefficient of sample mapping: ohU> UTккhгm ZSCOEF2 д w ш`е1:&second coefficient of sample mapping: d┘ruVulHH╘И┌inHH╘И■fl! o UT UTккhгelZSCOEF3 е ■`еAP%third coefficient of sample mapping: i2UR UTккhгf ZSCOEF4 ж A №` еZI&fourth coefficient of sample mapping: [UP UTккh г TZSPYBALUз j ·`еf spectrum y-balance offset: Ю ЄДUN UTккhг50ZSPYBLU и У °` еo spectrum y-balance offset: ta нUL UTккhг ·ZSRCHLCEй ╝ Ў`еUT;OCT (Observation Control Table) y increment for field map: g f╓UJ UTккhгUTZSRCHLCFк х Ї`е;OCT (Observation Control Table) x increment for field map: ZM UH UTккhгZSUN л 'Mo Є`еnt&Sun position: geocentric J2000 frame: (UF UTккhг ъ ZTREFH м F7 Ё еt XOCT (Observation Control Table) time of zero doppler correction: Doppler shift 0 phase icC ЁеpiXtime (the time of zero doppler correction) Higher order bits in spacecraft clock units O Ё@е&(125ms since Jan 1,1979) SE-01p3-266 iUD UTккhгelZXDCALP н x ю`еAP*proportional x-deflection cal correction: ТUB UTккhгZSZXDCALU о б ь`еfo'x comp null deflection cal correction: UT╗U@ UTккhгBAZYDCALP п ╩ ъ`еtr*proportional y-deflection cal correction: фU> UTккhг °ZYDCALU ░ є ш`еce'y comp null deflection cal correction: E ш еg-------------------------------------------------------------------------- Sources: ETS: Ed T. Smith х Ї шеOCSETS-a: Phone converstations with Jeff Lawson and Ed Kimmer at POCC. ETS-b: Cutler N шеIcomments in SOGS routine CGWCEX. ETS-c: WFPC SOGS Notebook ND-1002C, by H% шеVNorton. ETS-d: My inspection of science headers keyword values. ETS-e: Conversation 1 шеVwith CALFOS programmer, Steve Hulbert. ETS-f: My inspection of actual keyword names = ш@е Ё(ETS-g: Phase II proposal instructions. K ш`ЪбUTк%╟?H5▀v%╟?HDD rr: hнлZS м▌Ї╙UDFH┤D┌vulFK5ct&·КCю╛qFрGDIJAL =√ЫКC?&Ч╔7Ю1Х╣/╩2╓╟&·4H┤,ф 4"/Щ/A{3╝╙'├A2╨""/2°жКC+$nКC╪ж gl ЕCiуGсFHDHKuldeМ┌iуgliуь7 +ьпiу#m▓iу■░м ╗Fи---ЖУКC╨╛qHсGIDGJK-- --М┌КCЖУ&Ч╔щў1Х╣&╛^2╓╟/Оc4H┤)вJ4"&яi/A{"╦г'├A#╕S"/#П╨КCЛwКC╪жsta2°жКCїIсHJDFJert 2°жКC=√ЫКC■░м ╗Fи&·КCю╛qJтIKDHK CFIgl .ШФ+H┤K┘JD00GJqWFduonLeftdvenRighte kdА C Reference шdН CdРlbdТ odФ шdЦhadШs.dЪкdЬdЮdа dв d д┌d !жKd! 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