PODPS KEYWORD DICTIONARY 04 SEPT 1991 ABSHFILE TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Absolute Sensitivity Files (ABS): The absolute sensitivity scale files contain data that are used to perform HRS absolute flux calibration. These files are used in conjunction with the HRS wavelength net files that specify the wavelength net (grid) used for interpolation of absolute sensitivity scale values. Absolute sensitivity files contain two groups of data that correspond to the large and small apertures of the HRS. Because the HRS wavelength net files contain the wavelength net corresponding to these sensitivity values it is not assumed that the spacing between wavelength values is uniform. Data in the absolute sensitivity files are stored in REAL*4 format. ACCPDATE TYPE=C*7 INSTRUMENT=ALL FILETYPE=SHP UNITS=DATE proposal acceptance date (yyyyddd): ADC_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI application of dispersion constants: Convert the sample positions on the photocathode to wavelengths by applying the dispersion constants using tables ccr5, ccr6, and ccr7 containing spectral order, dispersion, and thermal constants. This routine computes spectral orders and wavelengths. For first order gratings, the spectral order is set to 1. For echelle gratings the spectral order is computed by the following formula: order = NINT( numerator/ denominator) numerator = b*A*sin((C-carpos)/B) denominator = ydef-a-d*A(sin((C-carpos)/B) Where: NINT is the nearest integer, A,B,C are in table ccr5, a,b,d are in table ccr5, carpos is the carrousel position, and ydef is the Y-deflection adjusted for the proper aperture And: The wavelengths are computed by solving the dispersion relation for wavelength using Newton's iterative method. The dispersion relation is described by the following equation: s = a0 + (a1*m*w) + (a2*m*m*w) + (a3*m) + (a4*w) + (a5*m*m*2) + (a6*m*w*w) Where: m is the spectral order, w is the wavelength, a0,a1,.. are the dispersion coefficients, and s is the sample position. (calguide) AFFILIAT TYPE=C*18 INSTRUMENT=ALL FILETYPE=SHP observer organization or affiliation: Obtained directly from the cover page of the proposal form: GO = general observer, AR = archival researcher, IDT = investigation definition team, IS = interdisciplinary scientist, SCI = ST Science staff, ESA = european space agency, MOC = mission operation contractor. (qpersonnel) ALIASi TYPE=C*68 INSTRUMENT=ALL FILETYPE=SHP synonym for target name: (i=1..2) In addition to the catalog name, a target should be assigned at most two 'common names', or aliases. These might include the Bayer (Greek-letter) designation or Flamsteed number with the standard three-letter constellation abbreviation (eg, ZETA-CAP, 22VUL), the Bright Star Catalog number (eg, HR5270), or other names, if they exist (eg, CYG-X1, BARNARDS-STAR, PROXIMA-CEN). Star clusters, nebulae, galaxies, and clusters of galaxies should be assigned commonly used names (eg, HYADES, OMEGA-CEN, CRAB-NEBULA, ABELL63, COMA-CLUSTER) or Messier numbers (eg, M13, M31, M67). (PROP_INST--SEC_5.TEX;1) ANGLESEP TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSECONDS target angular separation in arcsec. user input if qextpf=t. computed from target position (qtara2, qtadc2) and computed target position (qexcra, qexcdc) if qextpf=a. together with the position angle this field specifies offset data from the referenced target position (qtara2,qtadc2) in polar coordinates (1 x 10e-3 precision). [qexposure] ANG_SIDE TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES (0.,360.) angle between sides of scan parallelogram clockwise angle, about the beginning of the first scan, from the direction of the first scan to the side of the scan parallogram. (1x10e-04 precision). [qexposure] ANNPARRA TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSECONDS par. shift in position, non-solar sys target: the magnitude of the parallactic shift in the position of the non-solar system target at the time of observation. [qobservation.annparra] APERAREA TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI UNITS=ARCSECONDS^2 aperature area: Area of the aperture used, in square arc seconds. This keyword is filled by calibration software only when the target is an extended source. APEROBJ TYPE=C*10 INSTRUMENT=ALL FILETYPE=SHP UNITS=NAME si object aperture id: SI object aperture and coordinate system id; specifies the aperture and coordinate system of the instrument to be used for the observation of the target. It is the aperture id concatenated with the aperture coordinate system id. These ids are defined in ST_ICD_26 part III. WFPC: W//[WF|PC]//aperture//summode, where: aperture: ALL (for ALL or ANY); 4ND (for ALL-ND); 1,2,3,4; summode: S (for mode= 2x2); WFLOOD: if mode=UVFLOOD; [qobservation.coord_id] APEROFFX TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSECONDS x component of offset of object in aperture (arcsec): X component of the offset of the target from the center of the aperture. If coord_typ = SIAS, then units are pixels; if coord_typ = SICS, then units are arc-seconds. APEROFFY TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSECONDS y component of offset of object in aperture (arcsec): Y component of the offset of the target from the center of the aperture. If coord_typ = SIAS, then units are lines; if coord_typ = SICS, then units are arc-seconds. APERSKY TYPE=C*10 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSECONDS si sky aperture id: SI sky aperture and coordinate system id: specifies the aperture and coordinate system of the instrument to be used for the sky background light observations in conjunction with the observation of the target. It is the aperture id concatenated with the aperture coordinate system id. These ids are defined in ST_ICD_26 part III. APERTOBJ TYPE=C*10 INSTRUMENT=HSP FILETYPE=SCI aperture in use - object data: APERTSKY TYPE=C*10 INSTRUMENT=HSP FILETYPE=SCI aperture in use - sky data: APERTURE TYPE=C*10 INSTRUMENT=HSP FILETYPE=SCI name of the aperture used for this file: APERTURE TYPE=C*10 INSTRUMENT=HRS FILETYPE=SCI aperture name: APERTYPE TYPE=C*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=NAME SIDS/SIAS/SICS ... aperture coordinate system type where SIDS = si detector system, a coordinate system derived from si readouts in the science or engineering data stream; SIAS = si aperture system, a coordinate system based on the aperture or fov of the si; SICS = si corrected system which in general differs from the sias by removal of distortions and scale changes. [qexposure.coord_type] APER_k TYPE=C*15 INSTRUMENT=ALL FILETYPE=SHP UNITS=NAME TYPE=C*15 instrument aperture: (k=1..4) APER_ID TYPE=C*3 INSTRUMENT=FOS FILETYPE=IMG/SCI The entrance aperture id: A-1 4.3 A-2 0.5-PAIR A-3 0.25-PAIR A-4 0.1-PAIR B-1 0.5 B-2 0.3 B-3 1.0 B-4 C-1 1.0-PAIR C-2 0.25x2.0 C-3 2.0-BAR C-4 0.7x2.0-BAR ERR error (tguide 7.0-11) APER_POS TYPE=CHR INSTRUMENT=FOS FILETYPE=SCI aperture used: ARGPERIG TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=REV/SEC argument of perigee (revolutions/second): ASA_FILE TYPE=L*1 INSTRUMENT=HSP FILETYPE=UDL area scan analog is present: ASD_FILE TYPE=L*1 INSTRUMENT=HSP FILETYPE=UDL area scan digital is present: ASK_FILE TYPE=L*1 INSTRUMENT=HSP FILETYPE=UDL analog sky science is present: AST_FILE TYPE=L*1 INSTRUMENT=HSP FILETYPE=UDL analog star science is present: ATODCORR TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Do A-to-D correction: YES, NO, DONE: Replace each pixel with the appropriate value from the AtoD correction lookup table. The name of the lookup table must be provided in the keyword ATODFILE. The AtoD table may consist of multiple lookup tables. The lookup table whose temperature is closest to the value of the input science image header keyword WBA3PCTM is selected. (calguide) ATODFILE TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI UNITS=FILENAME A-to-D Lookup Tables Files (A2D): The A-to-D lookup table files are used to correct the image data for a pattern introduced by the Analog to Digital converter electronics. This is done by replacing the short integer pixel values obtained from the WF/PC with floating point values that remove the systematic degradation introduced by this hardware problem. ATODSAT TYPE=I*4 INSTRUMENT=WFP FILETYPE=SCI number of "AtoD saturated" pixels (DQF=8): BACCORR TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI background subtraction correction: Subtract dark-count images. The dark-count reference file multiplied by the exposure time is subtracted from the input science file. The dark-count file is a full-frame image (512 x 1024 or 1024 x 1024), so if the science file is smaller than full frame, only the appropriate section of the dark-count file is used. (calguide) BACHFILE TYPE=C*18 INSTRUMENT=FOC FILETYPE=SCI UNITS=FILENAME Background (Dark Count) Files (BAC): The background files contain data used to subtract dark count from FOC science images. It is used for the background calibration. Background data files contain one group of data. Every background data file has the same format as an image. It is either a 1024 sample by 1024 line image for use with normal pixel format images, or a 512 sample by 1024 line image for use with zoom pixel format images. Each pixel in the background data file is a single-precision real (REAL*4) count rate value in counts per second. BACHFILE TYPE=C*18 INSTRUMENT=FOS FILETYPE=SCI UNITS=FILENAME Background Files (BAC): FOS background reference files contain the default background data used during background subtraction (spectroscopy ground software mode) for both object and sky spectra. BAC_CORR TYPE=C*8 INSTRUMENT=FOS FILETYPE=SCI background subtraction: Subtract the background from sky and object spectra. The observed background is first repaired; bad points (i.e., points at which the data is flagges as lost or garbled in the telemetry process) are filled by linearly interpolating between "good neighbors". Next, the background is smoothed with a median, followed by two iterations of a mean filter before subtraction. Filter widths are contained in table ccs3. If no background was taken, a default reference background, bachfile, is used. No smoothing is done to the reference file background, if used. This is a spectroscopy mode calibration step. (calguide) BADPIXEL TYPE=I*4 INSTRUMENT=WFP FILETYPE=SCI number of "generic bad" pixels (DQF=32): BCK_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI background removal: Subtract the background counts from the raw counts of the diode array. This routine subtracts the background by one of four methods. The first applicable method is used. (1) Subtract sky spectra (header keyword BINID of 5 or 6). For this case the background is smoothed by a median filter followed by a mean filter. (2) Subtract interorder from main diode array. (header keyword BINID of 3 or 4). For this case, the background is smoothed by a median filter followed by a mean filter. (3) Use background diodes from separate substep bins with header keyword BINID between 8 through 15. The diodes to use are selected on the basis of the value of BINID. (4) Use all background diodes from the same bins as gross spectrum. (calguide) BDEXPFLG TYPE=I*2 INSTRUMENT=HSP FILETYPE=SCI bus director expander flag: BIASCORR TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Do bias correction: YES, NO, DONE: Subtract the bias image reference file from the input science image. The names of the bias image and its DQF must be provided in the keywords BIASFILE and BIASDFIL. (calguide) BIASEVEN BIASODD TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI UNITS= Bias level from EED extended register Information garnered from columns 3-14 of the extracted engineering (.x0h) file. Note that the BIASEVEN value should be the mean of columns 3,5,7,9..., and the BIASODD value should be the mean of columns 4,6,8,10,...---i.e., the overscan columns are 180 degrees out of phase from the science image. (opr.21796) BIASFILE TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI UNITS=FILENAME Bias Files (BAS): The structure in the electronic bias is removed by subtracting the bias reference file (with its accompanying data quality file). The most notable component of this structure is a 0.6 DN even/odd column pattern. The BIASDFIL is the name of the bias frame reference data quality file. BINID TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI binid: BINIDi TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI bin id of substep i where: 0 = no data, 1 = star small aperture, 2 = star large aperture, 3 = upper interorder, 4 = lower interorder, 5 = sky small aperture, 6 = sky large aperture, 7 = dark cur BITPIX TYPE=I*2 INSTRUMENT=HRS FILETYPE=UDL bits per data value: BLEVCORR TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Do bias level correction: YES, NO, DONE: Determine the global bias level from the mean of the extended register pixels in the extracted engineering data file (.x0h) and subtracted from each pixel in the input science image. Only pixels not flagged in the extracted engineering DQF (.q1h) are included in the averaging. The names of these files must be provided in the keywords BLEVFILE and BLEVDFIL. (calguide) BLEVDFIL TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI UNITS=FILENAME Engineering file DQF: BLEVFILE TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI UNITS=FILENAME Engineering file with extended register data: BLMHFILE TYPE=C*18 INSTRUMENT=FOC FILETYPE=SCI UNITS=FILENAME Data Quality Initialization Files (BLM): The FOC data quality initialization files contain a priori information about the effect of the FOC's photocathodes on the quality of output data values. The data quality initialization file is used in conjunction with relation CGQ1_FIL_MSK to construct the FOC data quality mask. BRIGHT TYPE=R*4 INSTRUMENT=HRS FILETYPE=IMG upper threshold for star presence (counts) BUNIT TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI brightness units: CALIBDEF TYPE=I*4 INSTRUMENT=WFP FILETYPE=SCI UNITS=COUNT number of "calibration defect" pixels (DQF=2): CALIBRAT TYPE=C*1 INSTRUMENT=ALL FILETYPE=SHP UNITS=Y/N calibrate data flag: CALIBTYP TYPE=C*1 INSTRUMENT=ALL FILETYPE=SHP UNITS=TYPE i/e... calibration type where i = internal, e = external. set if qextyp_type = cal. [qexposure.calibr_typ] CAMERA TYPE=C*10 INSTRUMENT=WFP FILETYPE=SCI camera in use: WF (wide-field), PC (planetary): This indicates which of the two cameras was used to obtain the scientific data. The possible values are 'WIDE-FIELD' and 'PLANETARY'. [qexposure.camera] CAMMODE TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI coronographic apodizer mask: INBEAM, NOTUSED: In the FOC/288 configuration, the OCC Mode uses the f/96 camera with the compact Cassegrain assembly and an apodizing mask. The 0.4-arcsec occulting finger is used to produce a Lyot-type coronagraph. The 0.8-arcsec occulting finger is not available in this Operating Mode. (PROP_INST--SEC_8_2.TEX) CARPOS TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI carrousel position: CCG2 TYPE=C*18 INSTRUMENT=FOS FILETYPE=SCI UNITS=FILENAME paired pulse correction: Paired-pulse correction table. Deadtime constants are used to correct for the non-linear channel response of each diode. These constants are not expected to change during the lifetime of the FOS. Analysis of prelaunch data indicate that the same constants can be used for both FOS detectors. (calguide) CCP0 TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI UNITS=FILENAME Aperture Areas Relation: A CDBS table containing the names and areas of all the HSP's apertures and are used by the HSP calibration. Each entry contains an aperture name and an aperture area, which is used to convert HSP count rates into count rates per square arc-second. This information is loaded only from the Project Data Base Tape. See ICD-47 for further information. CCP1 TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI UNITS=FILENAME High Voltage Factor Relation: A CDBS table containing the coefficients and base values used in computing the high voltage detector characteristic for the HSP calibration. Each set of base values and coefficients corresponds to a particular HSP detector high voltage setting (command value), and data type. In each set there are a base value, a reference time, a reference temperature, and sixteen polynomial coefficients. CCP2 TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI UNITS=FILENAME Gain Factor Relation: A CDBS table containing the coefficients and base values used in computing the gain detector characteristic for HSP calibration. Each set of base values and coefficients corresponds to a particular HSP detector and a gain setting (command value). In each set there are a base value, a reference time, a reference temperature, and sixteen polynomial coefficients. CCP3 TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI UNITS=FILENAME Pre Amp Relation: A CDBS table containing the coefficients and base values used in computing the pre-amplifier detector characteristic for the HSP calibration. The PRE AMP detector characteristic is the contribution to the digital count rate or analog current from the electronics. Each set of base values and coefficients corresponds to a particular HSP detector and data type. In each set there are a base value, a reference time, a reference temperature, and sixteen polynomial coefficients. CCP4 TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI UNITS=FILENAME Efficiency Relation: A CDBS table containing the coefficients and base values used in computing the efficiency (relative sensitivity) detector characteristic for the HSP calibration. Each set of base values and coefficients corresponds to a particular HSP aperture and detector. In each set there are point and extended base values, a reference time, a reference temperature, and sixteen polynomial coefficients. CCP5 TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI UNITS=FILENAME Dark Count Relation: A CDBS table containing the coefficients and base values used in computing the dark count characteristic for the HSP calibration. Each set of base values and coefficients corresponds to a particular HSP dark aperture, a high voltage setting (command value), and data type. In each set there are a base value, a reference time, a reference temperature, and sixteen polynomial coefficients. CCP7 TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI UNITS=FILENAME CVC Offset Relation: A CDBS table containing the coefficients used in computing the current to voltage convertor (CVC) offset detector characteristic for the HSP calibration. Each set of base values and coefficients corresponds to a particular HSP detector and analog gain setting (command value). In each set there are a base value, a reference time, a reference temperature, and sixteen polynomial coefficients. CCP8 TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI UNITS=FILENAME Dead Time Relation: A CDBS table containing the coefficients and base values used in computing the dead time (tau) which is used for paired-pulse corrections in HSP calibration. Each set of base values and coefficients corresponding to a particular HSP detector, high voltage setting (command value), and pulse amplifier/discriminator (PAD) threshold setting (command value). In each set there are a base value, a reference temperature, and one coefficient. CCP9 TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI UNITS=FILENAME Dark Aperture Relation: A CDBS table containing the corresponding dark aperture names for each of the regular HSP aperture names. The dark aperture names are later used to calibrate HSP dark counts. Each regular HSP aperture name has a corresponding dark aperture name. Each image dissector tube (IDT) has three dark apertures and the photo-multiplier (PMT) has one dark aperture name. CCR1 TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Line Mapping Parameters Relation: A CDBS table containing the coefficients of the line mapping function that relates Y-deflection to line position in the photocathode. CCR2 TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Sample Mapping Parameters Relation: A CDBS table containing the coefficients of the sampke mapping function that relates Y-deflection and diode position to sample position in the photocathode. CCR3 TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Detector Parameters Relation: A CDBS table containing miscellaneous calibration parameters that are functions of detector. These parameters are used to compute effective channel numbers of background diodes, mean and median filter widths, and tolerances used to relate bins of data to gross spectra, and corresponding background data. CCR4 TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Wavelength Ranges Relation: A CDBS table containing the valid wavelength range for each HRS grating and eschelle mode. CCR5 TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Spectral Order Constants Relation: A CDBS table containing the constants used to determine the spectral order of an HRS observation when an eschelle mode is used. CCR6 TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Dispersion Constants Relation: A CDBS table containing the dispersion constants and a corresponding calibration temperature value that are used to generate an HRS wavelength scale as a function of grating mode and carrousel position. CCR7 TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Thermal Constants Relation: A CDBS table containing the observation temperature mnemonic (ZRIUTA, ZRIUTB, etc) and the scaling factor for each grating/ eschelle mode. These data are used in performing thermal motion correction for the 0th order dispersion constant. CCR8 TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Incidence Angle Constants Relation: A CDBS table containing the constants required to perform the incidence angle correction as a function of aperture, grating carrousel position and spectral order. CCR9 TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Echelle Interpolation Constants Relation: A CDBS table containing the constants used in the echelle ripple correction. These constants are used to compute the normalized grating efficiency as a function of spectral order and carrousel position. CCRA TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Echelle Non-interpolation Constants Relation: A CDBS table containing further constants used in the echelle ripple correction. These constants are used to compute the normalized grating efficiency as a function of grating/echelle mode. CCRB TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Scattered Light Coefficients Relation: A CDBS table containing the coefficients for determining the contribution of scattered light to the background. Records contain four scattered light coefficients and are organized by aperture, grating/echelle mode and spectral order. The four coefficients (a_scat, b_scat, c_scat, and d_scat) are used in the following equation to determine the background spectrum: B(i) = 0.5 * [a_scat*U(i) + b_scat*L(i)] - c_scat*N(i) + d_scat*N where: N(i) = O(i) - 0.5*[U(i) + L(i)] U(i) is the upper interorder count rate per diode L(i) is the lower interorder count rate per diode N(i) is the net on-order count rate per diode O(i) is the gross object spectrum count rate per diode N is the average net on-order count rate per diode averaged over all science diodes i is the science diode index CCS0 TYPE=C*18 INSTRUMENT=FOS FILETYPE=SCI UNITS=FILENAME Aperture Parameters Relation: A CDBS table containing parameters used to describe the FOS apertures. The relation is filled using data from the project data base tape. Records of aperture parameters are organized by detector and aperture ID. Aperture areas required to scale a sky spectrum taken in one aperture of a paired aperture before subtraction from the object spectrum taken in the other aperture. Values for this relation are required only for the paired apertures. (calguide) CCS1 TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME Aperture Position Parameters Relation: A CDBS table containing the two Y position values used to determine which of the apertures (upper or lower) was used for a given observation. Records of aperture position parameters are organized by detector and disperser. Aperture position parameters used to determine which aperture (UPPER or LOWER) of an aperture pair, was used for observing an object or sky spectrum. (calguide) CCS2 TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME Emission Lines Relation: A CDBS table containing the beginning and ending data point numbers of known emission line regions to be avoided during the smoothing of sky spectra. Records of emission line data points are organized by detector, disperser, first channel and the number of X-substeps. Beginning and ending data point numbers of known emission line regions in which a sky spectrum should not be smoothed before it is subtracted from the object spectrum. (calguide) CCS3 TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME Filter Widths Relation: A CDBS table containing the mean and median filter spectra widths used to smooth the sky and background. Records of detector parameters are organized by detector. CCS4 TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME Wollaston/Wavelength Parameters Relation: FOS Wollaston/Waveplate parameters are stored in the reference table which contains the initial position of the waveplate and the measures of the angles of each of two pass directions with respect to the Q = 1 coordinate axis of the polarization reference frame. Records of the two pass direction angles and the initial waveplate position are organized by detector, disperser, and polarizer. CCS5 TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME Sky Shift Parameters Relation: A CDBS table containing the FOS sky shift parameters used to offset wavelength scales of sky data. Records of sky wavelength scale offsets are organized by detector, aperture, disperser, and the number of X-substeps. CCS6 TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME Wavelength Coefficients Relation: A CDBS table containing the FOS wavelength coefficients which are used to generate a wavelength scale for FOS spectral data. Records of wavelength coefficients are organized by detector, disperser, aperture, polarizer, and pass direction. CCS7 TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME GIMP-Correction Coefficients Relation: A CDBS table containing the FOS GIMP-correction scale factors which are used to correct for the geomagnetically-induced image motion problem. CCS8 TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME predicted background count rates: ??? CD1_1 TYPE=R*4 INSTRUMENT=ALL FILETYPE=ALL partial of the right ascension w.r.t. x: CD1_2 TYPE=R*4 INSTRUMENT=ALL FILETYPE=ALL partial of the right ascension w.r.t. y: CD2_1 TYPE=R*4 INSTRUMENT=ALL FILETYPE=ALL partial of the declination w.r.t. x: CD2_2 TYPE=R*4 INSTRUMENT=ALL FILETYPE=ALL partial of the declination w.r.t. y: CDBSDATA TYPE=C*5 INSTRUMENT=ALL FILETYPE=SHP cdbs notification flag: 'CAL' or 'FALSE': CDBSFILE TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI CDBS file: GENERIC/BIAS/DARK/PREF/FLAT/MASK/ATOD/NO: CIRVELOC TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=METERS/SEC Circular orbit linear velocity in meters per second [wiephemeris.cir_vel] CLKDRFTR TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=SEC/COUNT^2 spacecraft clock drift rate: A POCC generated value. Checked daily. Stored onboard and dumped with the science telemetry. This value is as input from the ground, it is updated only after spacecraft safings and/or when the difference in spacecraft time from a POCC time `obtained from White Sands' is > 10msec. Used in PODPS translation of spacecraft generated time tags. See EXPSTART for usage. (ETS-a) CLKRATE TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=SEC/COUNT spacecraft clock rate: A POCC generated value. Checked daily. Stored onboard and dumped with the science telemetry. This value is as input from the ground, it is updated only after spacecraft safings and/or when the difference in spacecraft time from a POCC time `obtained from White Sands' is > 10msec. Used in PODPS translation of spacecraft generated time tags. See EXPSTART for usage. (ETS-a) CNT_CORR TYPE=C*8 INSTRUMENT=FOS FILETYPE=SCI count to count rate conversion: Convert from raw counts to count rates by dividing each data point by the exposure time and then correcting for disabled diodes. If DEFDDTBL=0, the disabled diodes are taken from the Unique Data Log (UDL), otherwise, the disabled diodes are found in the file DDTHFILE. This is a standard calibration step. (calguide) COL_B_V TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=??? expected B-V color: COL_U_B TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=??? expected U-B color: COL_V_R TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=??? expected V-R color: COMB_ADD TYPE=C*6 INSTRUMENT=HRS FILETYPE=SCI comb-addition (NO, TWO, FOUR, DSTWO, DSFOUR): COMPTAB TYPE=C*18 INSTRUMENT=FOC/HSP FILETYPE=SCI UNITS=FILENAME the HST components table: See PHOTMODE and related photometry keywords. CONFIG TYPE=C*15 INSTRUMENT=ALL FILETYPE=SHP UNITS=??? proposed instrument configuration: COSINCLI TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=??? Cosine of the orbit inclination angle [wiephemeris.cos_orb_incl] CRPIX1 TYPE=R*4 INSTRUMENT=ALL FILETYPE=SCI x-coordinate of reference pixel: CRPIX2 TYPE=R*4 INSTRUMENT=ALL 2-D FILETYPE=SCI y-coordinate of reference pixel: CRVAL1 TYPE=R*8 INSTRUMENT=ALL FILETYPE=SCI FOC: FOS: HRS: HSP (IMG): right ascension of the reference pixel HSP (SCI): time at reference pixel WFPC: CRVAL2 TYPE=R*8 INSTRUMENT=ALL FILETYPE=SCI FOC: FOS: HRS: HSP (IMG): WFPC: declination of reference pixel CTYPE1 TYPE=C*8 INSTRUMENT=ALL FILETYPE=SCI unitless, line, pixel, channel, sample, time: CTYPE2 TYPE=C*8 INSTRUMENT=ALL FILETYPE=SCI unitless, line, pixel, channel, sample, time: CVCOFSET TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI scaled CVC offset: Current-to-voltage converter (CVC) offset, in DN. This keyword is filled by the calibration software only for digital data files. (calhsp) DARKCORR TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Do dark correction: YES, NO, DONE: Scale the dark image reference file and subtract it from the input science image. The dark image is multiplied by the total dark accumulation time (obtained from the keyword DARKTIME in the input science image header, and expressed in seconds) and then subtracted from the input science image. The names of the dark image and its DQF must be provided in the keywords DARKFILE and DARKDFIL. (calguide) DARKFILE TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI UNITS=FILENAME Dark Files (DRK): The WF/PC dark reference file and its associated data quality file are used to correct the dark current. The WF/PC CCDs generate a spurious signal during exposures known as dark current. This signal is a function of the time since the last erase command and the operating temperature of the CCD detectors and varies from pixel to pixel. The dark reference file is scaled by the time since the last erase command and subtracted from the image. The DARKDFIL is the name fo the dark reference data quality file. DARKRATE TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI UNITS=COUNTS/SEC scaled cathode dark rate: Dark counts due to the detector, in counts/second, calculated by the calibration sofware (calhsp) DARKTIME TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI UNITS=SECONDS Dark time (seconds): DATALOST TYPE=I*4 INSTRUMENT=WFP FILETYPE=SCI UNITS=COUNTS number of "data lost" pixels (DQF=16): DATAMAX TYPE=R*4 INSTRUMENT=ALL FILETYPE=SCI the maximum value of the data: DATAMEAN TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI UNITS=COUNTS mean value of the "good" pixels: DATAMIN TYPE=R*4 INSTRUMENT=ALL FILETYPE=SCI the minimum value of the data: DATATYPE TYPE=C*10 INSTRUMENT=ALL FILETYPE=ALL datatype of the array: DATA_FMT TYPE=C*4 INSTRUMENT=HSP FILETYPE=SCI data format: byte, word, lwrd, alog, all: DATA_SRC TYPE=C*9 INSTRUMENT=HSP FILETYPE=SCI data source: star, sky, area scan: DATA_TYP TYPE=C*7 INSTRUMENT=HSP FILETYPE=SCI data type: digital, analog: DATE TYPE=C*8 INSTRUMENT=ALL FILETYPE=ALL UNITS=DATE date this file was written (dd/mm/yy): DATE-OBS TYPE=C*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=DATE UT date of start of observation (dd/mm/yy): Note that this is not necessarily the start of the exposure. For example, the WFPC observation starts on a major frame pulse, while the exposure actually starts 16.4 seconds later following a memory erase. See EXPSTART. DCFOBSN TYPE=I*4 INSTRUMENT=ALL FILETYPE=SHP DCF observation number in SHP: DDTHFILE TYPE=C*18 INSTRUMENT=FOS FILETYPE=SCI UNITS=FILENAME Disabled Diode Files (DDT): The disabled diode files contain a disabled diode table for use in the standard case reduction when the Unique Data Log (UDL) is not available. DEADTIME TYPE=I*4 INSTRUMENT=FOS FILETYPE=IMG accumulator close time (units of 7.8125 microsec): DEADTIME TYPE=I*4 INSTRUMENT=HSP FILETYPE=SCI Correct dead time. This switch applies only to digital data; if the data is analog, this switch has no effect. The following equation is used to correct for dead time: x = y/(1-y*t) Where: x is the true count rate, y is the observed count rate, and t is the dead time. (calguide) DEADTM TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI UNITS=SECONDS deadtime: Deadtime used in calculating pair-pulse correction for digital data, in seconds. This keyword is filled by the calibration software only for digital data files. (calhsp) DEA_TEMP TYPE=R*4 INSTRUMENT=HSP FILETYPE=SHP DEA temperature of the object detector: DECAPER1 TYPE=R*8 INSTRUMENT=HRS FILETYPE=SCI UNITS=DEGREES declination of the aperture (deg): DECAPER1 TYPE=R*8 INSTRUMENT=FOS FILETYPE=SCI UNITS=DEGREES declination of the aperture (deg): DEC_APER TYPE=R*8 INSTRUMENT=HSP FILETYPE=SCI UNITS=DEGREES declination of the aperture (deg): DEC_APER TYPE=R*8 INSTRUMENT=HRS FILETYPE=SCI UNITS=DEGREES declination of the aperture (deg): DEC_APER TYPE=R*8 INSTRUMENT=FOS FILETYPE=SCI UNITS=DEGREES declination of the aperture (deg): DEC_MOON TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES declination of moon in geocentric J2000.0 coordinates. [qobservation.declmoon] DEC_REF TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES declination of the reference target position. This is in heliocentric J2000.0. [qobservation.ref_obj_dec] DEC_SUN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES declination of sun in geocentric J2000.0 coordinates. [qobservation.declsun] DEC_TARG TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES Declination of the target. The epoch and equinox of the target position is J2000. For moving target, the epoch of the target position is the predicted start time for the observation. (Fixed - Heliocentric J2000, moving - Geocentric J2000.) [qobservation.dec_target] DEC_V1 TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES declination of v1 axis of space telescope in geocentric J2000.0 coordinates. The v1 axis is the optical axis of the space telescope (more or less the 'roll' axis). The epoch of the position of the v1-axis is the predicted start of observation. [qobsevation.declnv1] DEFAULTS TYPE=L*4 INSTRUMENT=ALL FILETYPE=SHP default values used in reformatting these data: DEFDDTBL TYPE=L*1 INSTRUMENT=FOS FILETYPE=IMG UDL disabled diode table used: DELAY TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI delay between integrations (in 1/1.024 microsec): DELTAS TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI delta sample position: DELTA_X TYPE=R*4 INSTRUMENT=HRS FILETYPE=IMG x increment for map (deflection units): DELTA_Y TYPE=R*4 INSTRUMENT=HRS FILETYPE=IMG y increment for map (deflection units): DETECTOB TYPE=I*2 INSTRUMENT=HSP FILETYPE=SCI/IMG detector in use (0-5) - object data: This holds the number of the detector that was used for data from the object during this observation. It is one of the five image dissector tubes (numbered from 1 to 5), including the two CsTe photocathodes, the two bialkali cathodes, and the photomultiplier tube. 0: none 1: POL 2: UV1 3: VIS 4: UV2 5: PMT [qexposure.detectob] DETECTOR TYPE=I*2 INSTRUMENT=ALL FILETYPE=SCI HRS: detector in use (1-2): WFPC: the ccd number of the data DETECTSK TYPE=I*2 INSTRUMENT=HSP FILETYPE=SCI detector in use (0-5) - sky data: This holds the number of the possible detector that was used for data from the sky (or background) during this observation. It is one of the five image dissector tubes (numbered from 1 to 5), including the two CsTe photocathodes, the two bialkali cathodes, and the photomultiplier tube. When MODE is SCP or ARS, this field will contain the null value (-1). [qexposure.detectsk] DET_CHR TYPE=C*8 INSTRUMENT=HSP FILETYPE=SCI retrieve detector characteristics: Retrieve detector characteristics. This keyword is not currently used, and it is not updated to COMPLETE by the calibration. (calguide) DET_TEMP TYPE=R*4 INSTRUMENT=HSP FILETYPE=SHP detector temperature of the object detector: Determined from the telemetered items VTPDET1..VTPDET5 as a function of detector number DETECTOB. DEZERO TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI Bias level from EED extended register: DGESTAR TYPE=C*12 INSTRUMENT=ALL FILETYPE=SHP the fgs id (f1, f2, f3) concatenated with the dominant gs id. [qobservation.dominant_gs] DIOHFILE TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Diode Response Files (DIO): Non-uniformities in diode responses for HRS detectors require science data to be normalized using data from the diode response files. Diode response data files contain a single group of normalization data with 512 entries corresponding to the 512 diodes of each HRS detector. Diode responses are stored in real*4 format. DIO_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI diode response correction: Divide the count value by the diode's response to correct for diode non-uniformity using the diode response file, diohfile. This routine corrects for diode response by dividing the input data by the diode response values. When comb-addition is used, a smoothed diode response array is computed using a weighted average of diode responses. Data with a diode response value less than the minimum value are set to 0.0. (calguide) DNFORMT TYPE=I*2 INSTRUMENT=FOC FILETYPE=SCI bits in each data number (8/16): DOHISTOS TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Make histograms: YES, NO, DONE: Create an image of three rows containing histograms of the pixel values in the input science image, following AtoD correction, and in the output (.c0h) image, respectively. This file has the extension .c2h. (calguide) DOPHOTOM TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Fill photometry keywords: YES, NO, DONE: DOPMAG TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI doppler shift scaling correction magnitude: See DOPPLER for a more complete description. DOPPLER TYPE=C*3 INSTRUMENT=HRS FILETYPE=SCI on-board doppler compensation (ON, OFF): An onboard doppler correction update can be performed once each minute at at the beginning of each observation. The update consists of computing a small correction factor to be added to each X-deflection as it is generated. The generated form of the correction is given by: dX = C*sin(2*pi*(t-t0)/P) where: dX: Correction Factor; C: DOPMAG: constant made up of a scale factor and the cosine of the orbital latitude - from OCT; P: orbital period - built into table of sines; t: current time - from spacecraft clock; t0: DOPZER: time of the doppler correction - from OCT; ST-ICD-08(III-80) DOPZER TYPE=R*8 INSTRUMENT=HRS FILETYPE=SCI doppler shift zero phase time (Modified Julian Date): See DOPPLER for a more complete description. DOP_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI doppler compensation: Correct for on-board Doppler compensation when removing photocathode nonuniformities and vignetting. This routine computes the percent of time spent at each Doppler offset. These are computed by dividing the observation into time segments and computing the deflection offset for each segment. The SHP packet time is used as the start of the readout and the packet time of the first science packet is used as the ending time of the readout. (calguide) DOSATMAP TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Output Saturated Pixel Map: YES, NO, DONE: Create a DQF flagging those pixels in the input science image which saturated the AtoD converter, or for which data was lost in transmission. This file has the extension .c3h. (calguide) DQ1HFILE TYPE=C*18 INSTRUMENT=FOS FILETYPE= UNITS=FILENAME ????? DQ2HFILE TYPE=C*18 INSTRUMENT=FOS FILETYPE= UNITS=FILENAME Data Quality Initialization Files (QIN): FOS data quality initialization reference files contain a priori information about the effect of the FOS's diode arrays on the quality of output data values. DQIHFILE TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Data Quality Initialization Files (QIN): The HRS data quality initialization files contain a priori information concerning the effect of the HRS's diode arrays on the quality of output data values. Data quality initialization data files contain a single group of data with 512 entries corresponding to the 512 diodes of each HRS detector. DQI_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI data quality initialization: Apply data quality initialization using the reference file, dqihfile. This routine performs the data quality initialization by flagging each data value with the values in the data quality initialization file. The file contains a data quality value for each diode. If the data quality value of the data is larger than the data qualify initialization file value for the diode, it is left unchanged. Quality values are never decreased. (calguide) DSK_FILE TYPE=L*1 INSTRUMENT=HSP FILETYPE=UDL digital sky science is present: DST_FILE TYPE=L*1 INSTRUMENT=HSP FILETYPE=UDL digital star science is present: DWELL_LN TYPE=I*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=COUNTS ( 1-99) dwell points per line for scan pointing mode; set if this is a dwell scan, otherwise equal to zero. [qexposure.dwells_line] DWELL_TM TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=COUNTS ???? ECBDX3 TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP eccentricity cubed times 3: ECBDX4D3 TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP eccentricity cubed times 4/3: ECCENTRY TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP Eccentricity of the orbit [wiephemeris.eccentricity] ECCENTX2 TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP 2 times the eccentricity of the orbit. [wiephemeris.two_x_ecc] ECH_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI correction for echelle ripple: If one of the echelle gratings is used, divide the flux value by the normalized grating efficiency to remove the echelle ripple using tables ccr9 and ccra, which contain echelle ripple constants. This routine performs the echelle ripple removal by dividing the flux by the following echelle ripple function: ripple = gnorm sinc(a*x+b)^^2 Where: gnorm = cos(A+B+C)/cos(A+B-C+e) x = [pi]*m*cos(A+B+C)*sin(A+e/2)/sin(A+C+e/2) And: e is arctan ( (samp-280.0)/f ), m is the spectral order, samp is the photocathode sample position, A is (r0 - carpos)*2*pi/65536.0, r0, B, C, f are grating parameters in table ccra, and a and b are coefficients from table ccr9. (calguide) EPCHTIME TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=SECONDS Epoch time of orbital parameters; given in the form of the number of seconds since 1/1/85. [wiephemeris.epoch_time] EPLONGPM TYPE=I*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=SECONDS planetographic coordinate system parameters: epoch of longitude of prime meridian of planetary target. seconds from 1980. [qtargets.epo_prim_mer] EQNX_SUN TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI equinox of the sun: EQRADTRG TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=KILOMETERS planetographic coordinate system parameters: equatorial radius of planetary target. [qobservation.equ_radius] EQUINOX TYPE=C*7 INSTRUMENT=ALL FILETYPE=SHP UNITS=DATE TYPE=C*7 equinox of the celestial coordinate system: eyyyy.f ... specifies the epoch of equinox of the input coordinate system for target position data e = j or b, yyyy = year, f is a fraction of yyyy. ERRCNT TYPE=I*4 INSTRUMENT=ALL FILETYPE=ALL UNITS=COUNTS number of segments containing errors: Science data is divided for telemetry purposes into lines and frames. A line is a maximum of 965 16-bit words of science data, and a frame is a collection of one or more lines. For transmission purposes, a line of data is accommodated in a packet, which in turn is divided into from 1..16 segments (each of which has 64 16-bit words.) ERR_CORR TYPE=C*8 INSTRUMENT=FOS FILETYPE=IMG propagated error computation: Compute the propagated error at each point in the spectrum. The photon statistical errors in the original data are carried through the reductions. The errors are scaled at each calibration step. Thus, the standard errors have the same units as the calibrated data. This step is a spectroscopy mode calibration step. (calguide) ESQDX5D2 TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP Eccentricity of the orbit squared times 5/2. [wiephemeris.ecc_sqd_x_fh] EXPACKET TYPE=I*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=COUNTS The expected number of source packets for an observation for the SI science instrument data. This value is used to determine whether data collected by data partitioning has all been collected. The estimate includes science data, unique definition log, and science header packets. [qobservation.expected_pkt] EXPEND TYPE=R*8 INSTRUMENT=ALL FILETYPE=SCI UNITS=MJD exposure end time (Modified Julian Date): WFPC: EXPEND = EXPSTART + EXPTIME (cgwcex) FOS: EXPEND = FPKTTME (1 readout), LPKTTIME (multiple readouts) EXPFLAG TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI Exposure interruption indicator: NORMAL - EXPTIME was successfully calculated from telemetry information, is equal to the predicted exposure time, and the value of NSHUTA17 is less than or equal to 1. EXPFLAG is also set to NORMAL when EXPTIME was successfully calculated and the predicted exposure time was not available. INTERRUPTED - EXPTIME was successfully calculated from telemetry information, is equal to the predicted exposure time, and the value of NSHUTA17 is greater than 1. INCOMPLETE - EXPTIME was successfully calculated from telemetry information and is not equal to the predicted exposure time. (Invariably the case in Rapid-Read mode FOS observations. ETS-E) EXTENDED - EXPTIME was successfully calculated from telemetry information and is greater than the predicted exposure time. UNCERTAIN - The Shutter Log Overflow flag (WWLOGOF) was set, which indicates that not all shutter open/close times are available. EXPTIME was calculated from the shutter open/ close times that are available. INDETERMINATE - EXPTIME could not be successfully calculated from the telemetry and the predicted exposure time was not available. PREDICTED - EXPTIME could not be successfully calculated from the telemetry and EXPTIME was set to the predicted exposure time. EXPFLAG TYPE=C*18 INSTRUMENT=FOC FILETYPE=SCI Exposure interruption indicator: EXPFLAG TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI Exposure interruption indicator: EXPFLAG TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI Exposure interruption indicator: EXPFLAG TYPE=C*18 INSTRUMENT=FOS FILETYPE=SCI Exposure interruption indicator: EXPOSURE TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI UNITS=SECONDS exposure time (seconds): EXPOSURE TYPE=R*4 INSTRUMENT=FOS FILETYPE=SCI UNITS=SEC/PIXEL exposure time per pixel (seconds): As opposed to the misleading EXPTIME which gives the total time the accumlation of photons took even though that time includes independent pixels (nxsteps) and the sum of all groups. (ETS-D) EXPSTART TYPE=R*8 INSTRUMENT=ALL FILETYPE=SCI UNITS=MJD exposure start time (Modified Julian Date): WFPC: Calculated as follows: EXPSTART = UTC0 + (CLKRATE * T) + (CLKDRFTR * T**2)/2 + DELAY T = (WEXPTMHI*2**16 + WEXPOTIM) - SPCLINCN where: SPCLINCL = spacecraft ticks since UTC0 DELAY = 16.4 seconds if non-NSCC-1 controlled exposure (generally means, the NSCC-1 didn't have take over to deal with loss of PCS lock.) = 16.5 seconds if NSCC-1 controlled exposure (rather than WFPC micro-processor controlled.) (ETS-f) FOS: EXPSTART = FPKTTIME - (EXPTIME + EXPDEADTM) where: EXPDEADTM= (DEADTIME*7.8125E-6)*INTS*[NXSTEPS*OVERSCAN*YSTEPS*SLICES] *NPAT*NREAD*NMCLEARS NOTE: EXPSTART only gives the start time of the FIRST group of data in the final PODPS product. (ETS-f) EXPTIME TYPE=R*8 INSTRUMENT=ALL FILETYPE=SCI UNITS=SECONDS exposure duration (seconds)--calculated: WFPC: If the WFPC exposure was a DARK FRAME, the exposure time code in WEXPORTH is used to obtain EXPTIME from the WFPC Exposure Time Table. Otherwise, the exposure time code in WEXPOCMD is used to obtain EXPTIME from that table. In addition, if the number of shutter closures (NSHUTA17) was greater than 1, the WFOCTIME values are used to calculate the amount of time that the shutter was closed: EXPTIME = EXPTIME - shutter_closed_time When EXPFLAG is set to PREDICTED, EXPTIME was set to the predicted exposure time. FOS: EXPTIME reflects the total accumulator open time (livetime): EXPTIME= (LIVETIME*7.8125E-6)*INTS*[NXSTEPS*OVERSCAN*YSTEPS* SLICES]*NPAT*NREAD*NMCLEARS Misleading exposure time: This gives the total time the accumlation of photons took even though that time includes independent pixels (nxsteps) and separate spectra (ysteps) and is the sum of ALL groups. See EXPOSURE. (ETS-f) EXP_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI division by exposure time: Convert to count rates. This routine converts the input data to count rates by dividing by the exposure times. The exposure time is computed for each bin as 0.05*NCOADD*INTPER, where NCOADD is the number of coadds to the bin and INTPER is the integration period in 0.05 second intervals. If either value contains fill, no exposure time can be computed and the entire bin is flagged as unusable. (calguide) EXTNCT_V TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP extinction in V: EX_EFFIC TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI UNITS=UNITLESS scaled extended source cathode efficiency: Extended source sensitivity relative to that of the reference aperture, unitless. This keyword is filled by the calibration software only when the target is an extended source. E_B_V TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP E(B-V): FAINT TYPE=R*4 INSTRUMENT=HRS FILETYPE=IMG lower threshold for star presence (counts): FCHNL TYPE=I*2 INSTRUMENT=FOS FILETYPE=SCI UNITS=CHANNEL NUMBER first channel: ACTUAL FLAGS AND INDICATORS COMMON (FOS keyword: NCHNLS). The first channel to be processed: 0,2,4,...,510 or -1 for error. [qexposure.fchnl] FDMEANAN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=REV/SEC First derivative coefficient for mean anomaly in revolutions per second [wiephemeris.fd_mean_anom] FGSLOCK TYPE=C*7 INSTRUMENT=ALL FILETYPE=SCI status of FGS lock (FINE, COARSE, GYROS, UNKNOWN): Keyword source is the field qbs_obset.scenario_acq which is translated into simpler terms. (cgalok) FGWA_ID TYPE=C*3 INSTRUMENT=FOS FILETYPE=SCI UNITS=NAME The disperser id: Disperser Disperser ID G130H H13 G190H H19 G270H H27 G400H H40 G570H H57 G780H H78 G160L L15 G650L L65 PRISM PRI MIRROR CAM or ERR for error. [qexposure.fgwa_id] FILLCNT TYPE=I*4 INSTRUMENT=ALL FILETYPE=ALL UNITS=COUNTS number of segments containing fill: Science data is divided for telemetry purposes into lines and frames. A line is a maximum of 965 16-bit words of science data, and a frame is a collection of one or more lines. For transmission purposes, a line of data is accommodated in a packet, which in turn is divided into from 1..16 segments (each of which has 64 16-bit words.) FILTER1 TYPE=I*2 INSTRUMENT=WFP FILETYPE=SCI first filter number (0-48): This holds the number of the first filter used. Possible values are 0 to 48 (0 meaning the clear filter and 1-48 meaning one of the 48 filters). [qexposure.filter1] FILTER2 TYPE=I*2 INSTRUMENT=WFP FILETYPE=EXT second filter number (0-48): This holds the number of the second filter used. Possible values are are 0 to 48 (0 meaning the clear filter and 1-48 meaning one of the 48 filters). [qexposure.filter2] FILTNAMi TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI filter name: (i=1..2) FILTNAMi TYPE=C*6 INSTRUMENT=FOC FILETYPE=SCI filter name: (i=1..4) FINCODE TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI observation termination code: ZFINCOD: a status code giving the reason for the dump of the HRS Unique Data Log. Thse codes are given in Section 3.8.3 of SE-01: 101: Observation Processing initiated 102: Observation pattern complete 103: Under-exposure termination 104: Over-exposure termination 105: Bad-data termination 106: Observation time-out FL1HFILE TYPE=C*18 INSTRUMENT=FOS FILETYPE=SCI UNITS=FILENAME first flat-field header file: FL2HFILE TYPE=C*18 INSTRUMENT=FOS FILETYPE=SCI UNITS=FILENAME Flat Field Files (FLT): FOS flat field reference files contain diode and photocathode sensitivity data used to reduce flat-field spectra (spectroscopy ground software mode). FLATCORR TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Do flat field correction: YES, NO, DONE: Correct the input science image for variations in gain among pixels by applying a flat-field image. The input science image is multiplied by the flat-field image. The names of the flat field image and its DQF must be provided in the keywords FLATFILE and FLATDFIL. (calguide) FLATDFIL TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI name of the flat field reference DQF: FLATFILE TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI UNITS=FILENAME Flat Field Reference Files (FLT): The variations in sensitivity between pixels in the CCD detectors are corrected by applying a flat field reference file. This file contains the normalized inverse sensitivity (gain) for each pixel in the detector. It is made from internal flat lamp exposures, the combination of streaked earth flats or processed observations of astronomical sources. The image is multiplied by the flat field file after correcting for bias, preflash, superpurge, and dark. The FLATDFIL is the name of the flat field reference data quality file. FLATNTRG TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=??? planetographic coordinate system parameters: flattening of planetary target, the difference between the equatorial and polar radius divided by the equatorial radius. [qobservation.flattening] FLT_CORR TYPE=C*8 INSTRUMENT=FOS FILETYPE=SCI flat-fielding: Remove diode-to-diode sensitivity variations and fine structure by multiplying by the flat field response. The object spectra and sky spectra (if obtained) are flat-fielded. This process requires the use of the flat field response file, fl1file. A second flat field file, fl2file, is required for paired aperture or spectropolarimetry observations. This step is a spectroscopy mode calibration step. (calguide) FLX_CORR TYPE=C*8 INSTRUMENT=FOS FILETYPE=IMG flux scale generation: Convert the object spectra to absolute flux units. The object spectra are converted to flux units by multiplying by the inverse sensitivity vector. This routine requires the inverse sensitivity file iv1file. A second inverse sensitivity file, iv2file, is required for paired- aperture or spectropolarimetry observations. This calibration step converts the count rates to units of ergs/cm^^2/sec/Angstrom. This step is a spectroscopy mode calibration step. (calguide) FLX_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=IMG flux scale generation: Calculate the absolute flux by dividing the flux by the absolute flux coefficients using the absolute flux file, abshfile, and corresponding wavelength file, nethfile. This routine converts the input flux to absolute flux units by dividing it by a sensitivity stored in absfil (sensitivities) and netfil (wavelengths for the sensitivities). Quadtratic interpolation is used within the sensitivity file to compute sensitivities for the input wavelengths. (calguide) FPKTTIME TYPE=R*8 INSTRUMENT=ALL FILETYPE=SCI the time of the first packet: Each packet contains ancillary information including a spacecraft time code value. This value contains the spacecraft time of transmission of the 'Line Start' signal. FP_SPLIT TYPE=C*6 INSTRUMENT=HRS FILETYPE=SCI fp-split (NO, TWO, FOUR, DSTWO, DSFOUR): F_RATIO TYPE=I*2 INSTRUMENT=FOC FILETYPE=SCI focal ratio: Set to 48 if the optic relay (OPTCRLY) is 'F48'; set to 288 if the coronographic apodizer mask (CAMMODE) is in the beam; otherwise the focal ratio is set to 96. (OPR.20224) GCOUNT TYPE=I*2 INSTRUMENT=ALL FILETYPE=ALL UNITS=COUNT number of groups: GEOCORR TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI geometric correction: Geometric correction. A raw FOC image is slightly distorted (about 2%) by the optics and the detector. The distortions are comparable in magnitude. The optical distortion was computed by ray tracing, and the detector distortion is measured by taking flat-field images and observing the positions of reseau marks that are uniformly spaced on the photocathode. A geometric correction reference file includes both optical and detector distortion. It consists of two sets of positions: a uniform grid of reference positions (i.e., on the sky) and where those positions would be observed in a raw FOC image. Removing the distortion involves determining the location in the input (distorted) image of each pixel in the output (undistorted) image, and then interpolating the DN (in counts) for that location. Bilinear interpolation is used for both the position and DN. (calguide) GEODEFV TYPE=R*4 INSTRUMENT=FOC FILETYPE=SCI UNITS=???? geo DN value for areas outside sci image: GEOHFILE TYPE=C*18 INSTRUMENT=FOC FILETYPE=SCI UNITS=FILENAME Geometric Distortion Files (GEO): The geometric distortion correction data files contain data used to correct FOC science images for the geometric distortion caused by the FOC optics and the Photon Detector Assembly (PDA). It is used for the geometric calibration. The geometric distortion correction data files consist of the distorted and undistorted, sample and line coordinate values (REAL*4) of a grid of reference points on the FOC detector screen. GMF_CORR TYPE=CHR INSTRUMENT=FOS FILETYPE=SCI scale reference background: GOODMAX TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI maximum value of the "good" pixels: GOODMIN TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI minimum value of the "good" pixels: GPIXELS TYPE=I*4 INSTRUMENT=WFP FILETYPE=SCI UNITS=COUNT number of "good" pixels (DQF=0): GRAPHTAB TYPE=C*18 INSTRUMENT=HSP FILETYPE=SCI UNITS=FILENAME the HST graph table: See PHOTMODE and related photometry keywords. GRATING TYPE=C*3 INSTRUMENT=HRS FILETYPE=IMG grating, echelle or mirror in use: GRATING -- grating/echelle mode: Spectral Element Grating Detector G140M G-1 Digicon 1 G160M G-2 Digicon 2 G200M G-3 Digicon 2 G270M G-4 Digicon 2 G140L G-5 Digicon 1 ECH-A E-A Digicon 1 ECH-B E-B Digicon 2 SAFE1 SAF Digicon 1 SAFE2 SAF Digicon 2 MIRROR-N1 MN1 Digicon 1 MIRROR-A1 MA1 Digicon 1 MIRROR-N2 MN2 Digicon 2 MIRROR-A2 MA2 Digicon 2 NDF (NDF = NOT DEFINED, ERR = ERROR) [qexposure.grating] GRNDMODE TYPE=C*18 INSTRUMENT=FOS FILETYPE=SCI/IMG ground software mode: LED-FLAT-FIELD-MAP (IMAGE) TIME-RESOLVED (PERIOD) TIME-TAGGED (TAG) RAPID-READOUT (RAPID) TARGET ACQUISITION (ACQ,ACQ/BINARY,ACQ/PEAK,ACQ/FIRMWARE) SPECTROSCOPY (no polarizer) SPECTROPOLARIMETRY (with polarizer) (tguide 7.0-10) GROUPS TYPE=L*1 INSTRUMENT=ALL FILETYPE=ALL image is in group format: HEADER TYPE=L*1 INSTRUMENT=FOS FILETYPE=SCI science header line exists: HEL_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI conversion to heliocentric wavelengths: Convert wavelengths to heliocentric coordinate system. This routine corrects for the Earth's motion around the Sun. (calguide) HIGHVOLT TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI scaled high voltage factor: Scaling factor relative to the reference volatge, unitless, calculated by the calibration software (calhsp). HOFFi TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI horizontal offset bin i+1: i=1..6 HSTHORB TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=SECONDS half the duration of the ST orbit (seconds): HVPSM TYPE=R*4 INSTRUMENT=HSP FILETYPE=SHP high voltage power supply output of the object detector: IAC_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI incidence angle correction: Adjust the zero-point of the wavelength scale for the large science aperture and the two spectral lamp apertures using table CCR8 containing incidence angle coefficients. This routine adjusts the wavelenght array for the difference in incidence angle of apertures LSA, SC1 and SC2 from the SSA. Table CCR8 is searched for the correct grating, spectral order, aperture, and carrousel position to obtain two coefficients, A and B. Interpolation of the coefficients (in carrousel position) is used if an exact match is not found. These coefficients are then used to compute an offset using the following formula: w = w + (A+B*s)/m Where: w is the wavelength, A and B are coefficients in ccr8, s is the photocathode sample position, and m is the spectral order. (calguide) IMAGETYP TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI image type: DARK/BIAS/INTFLAT/KSPOTS/EXTERNAL/EARTH-CALIB: INFOB TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI deflection pairs/substep pattern: INFOC TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI largest repeat code in the substep pattern: INSTRUME TYPE=C*4 INSTRUMENT=ALL FILETYPE=ALL instrument in use: FGS: Fine Guidance System FOC: Faint Object Camera FOS: Faint Object Spectrograph HRS: Goddard High Resolution Spectrograph HSP: High Speed Photometer WFPC: Wide Field/Planetary Camera INTOBS TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI expected number of intermediate readouts: INTS TYPE=I*4 INSTRUMENT=FOS FILETYPE=SCI number of integrations: INT_TIME TYPE=I*4 INSTRUMENT=HSP FILETYPE=SCI time of integration (in 1/1.024 microseconds): ITFCORR TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI intensity transfer function correction: Apply format-dependent photometric correction. The reference files used in this step are called ITF files for historical reasons. They are not full-frame; there is one such file for each format. The format-dependent correction is applied by multiplying the image from the previous step (i.e., the dark-count subtracted image) by this file. (calguide) ITFHFILE TYPE=C*18 INSTRUMENT=FOC FILETYPE=SCI UNITS=FILENAME Intensity Transfer Function Files (ITF): The Intensity Transfer Function (ITF) files contain data used to correct FOC science images for spatial nonuniformities that depend on the image format. It is used for the format-dependent photometric correction. An ITF data file has the same form as an FOC image. The lengths of the axes are the same or larger than those of the image to be calibrated. Each entry is a REAL*4 scaling factor that is used to multiply the corresponding pixel DN count in the FOC science data file that is to be corrected. IV1HFILE TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME first inverse sensitivity header file: IV2HFILE TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME Inverse Sensitivity Files (IVS): FOS inverse sensitivity reference files contain data used to convert object data to an absolute flux scale (spectroscopy ground software mode). IXDEFi TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI initial x deflection i: i=1..5 IYDEFi TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI initial y deflection i: i=1..5 KSPOTS TYPE=C*3 INSTRUMENT=WFP FILETYPE=SCI Status of Kelsall spot lamps: ON, OFF: Determined by PODPS on the basis of the packet format code of the observation: KSPOTS=OFF unless the packet format code='24'x or '2C'x. (cgwsdh) LEDCOLOR TYPE=C*10 INSTRUMENT=FOC FILETYPE=SCI LED color (a color, blank , NONE or ERROR): If at least one telemetry item (XC1LEDSL, XC2LEDSL) is NOT fill, then the FOC LED selection table will be searched to determine the significance of the telemetered value or values. If the telemetry measurements are above a threshold count, then LEDMODE is ON , else it is OFF. If both telemetry measurements are valid, then both must agree on whether LEDMODE is ON or OFF. If they disagree, an error condition is generated. (cp2jld) LEDMODE TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI led calibration status: ACTIVE, NOTUSED: calibration LED mode: ACTIVE,NOTUSED. [qexposure.ledmode] LINE TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI line positions: LINEBEG TYPE=I*2 INSTRUMENT=WFP FILETYPE=EXT line number (1st line: wrt source format): LINEBEG TYPE=I*2 INSTRUMENT=FOC FILETYPE=QIN line number (1st line: wrt source format): LINENUM TYPE=C*15 INSTRUMENT=ALL FILETYPE=ALL UNITS=LINE_NUMBER PEP proposal line number: LINEOFF TYPE=R*4 INSTRUMENT=FOC FILETYPE=SCI line offset (0.0-1023.75): Line offset, mnemonic = XCCCUVRO. [qexposure.lineoff] LINEPFM TYPE=I*2 INSTRUMENT=FOC FILETYPE=SCI lines per frame (64, 128, 256, 512, or 1024): Number of lines per frame [qexposure.linepfm] LINES TYPE=I*4 INSTRUMENT=HSP FILETYPE=IMG number of lines in a group: LIVETIME TYPE=I*4 INSTRUMENT=FOS FILETYPE=SCI accumulator open time (units of 7.8125 microsec): LOCATE TYPE=CHR INSTRUMENT=HRS FILETYPE=IMG do a locate after the spiral search: LONGPMER TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES planetographic coordinate system parameters: longitude of prime meridian of planetary target. [qtargets.long_prim_me] LPKTTIME TYPE=R*8 INSTRUMENT=ALL FILETYPE=SCI UNITS=MJD the time of the last packet: Each packet contains ancillary information including a spacecraft time code value. This value contains the spacecraft time of the start of the DMA (Direct Memory Access) transfer that produced the data for the packet. MAG_B TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=??? expected B Magnitude: MAG_R TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=??? expected R Magnitude: MAG_U TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=??? expected U Magnitude: MAG_V TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=??? expected V Magnitude: MAP TYPE=CHR INSTRUMENT=HRS FILETYPE=IMG dwell points at which to image the aperture: MAP_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI mapping function: Perform the photocathode mapping function using tables ccr1 and ccr2 containing the photocathode line mapping and sample parameters. This routine computes the mapping function for each of the substep bins using the following formulae: SAMPLE(bin) = x0 + b*XD + c*XD^^2 DELTAS(bin) = e LINE(bin) = L0 + A*YD Where: SAMPLE -- is the sample position of the first diode, DELTAS-- is the spacing between sample positions, LINE -- is the line position of the diodes, XD -- is the X-deflection minus 2048, YD -- is the Y-deflection minus 2048, s0, b, c and e are coefficients in ccr2, interpolated for the given Y-deflection, and L0, and A -- are coefficients in ccr1. (calguide) MAP_NUM TYPE=I*4 INSTRUMENT=HRS FILETYPE=IMG mosaic map number: MASKCORR TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Do mask correction: YES, NO, DONE: Include the static bad pixel mask in the output DQF. The name of the static bad pixel mask must be provided in the keyword MASKFILE. This file is in the same format as a DQF. (calguide) MASKFILE TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI UNITS=FILENAME Static Bad Pixel Mask Files (MSK): The static mask files (formerly known as the data quality masks) contain flags for those pixels which always contain degraded values. This mask is routinely incorporated into the data quality file generated in the RSDP pipeline by calwfp. The static mask file is a short integer (INTEGER*2) image file of of four (4) groups with the same dimensions as the WF/PC science image. The image contains values of zero (0) in all pixels, except for those with known static defects. Defective pixels are flagged with the value four (4). MAXCLK TYPE=I*4 INSTRUMENT=FOS FILETYPE=SCI maximum clock count: MAXGSS TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI maximum substep patterns/observation: read from the value telemetered in the HRS Unique Data Log (UDL): ZMAXGSS. MAXWAVE TYPE=R*8 INSTRUMENT=FOS FILETYPE=SCI UNITS=ANGSTROMS maximum wavelength: MAXWAVE TYPE=R*8 INSTRUMENT=HRS FILETYPE=SCI UNITS=ANGSTROMS maximum wavelength: MDF_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI median filter of background spectra: Use a median filter on the background. This routine performs a median filter of the background with a user-specified (i.e., specified in the table) filter width. The edge points are filled with the value of the closest position that can be filtered. (calguide) MEANANOM TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=REVOLUTIONS mean anomaly. [wiephemeris.mean_anomaly] MERGED TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI number of merged spectra in this pattern: MER_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI merging of substep bins: Merge the substep bins. This routine merges the spectral data. Unmerged output data is just a copy of the input data. Both the input and output data arrays are 2-dimensional arrays treated as 1-dimensional arrays by this routine. The input is treated as 1-dimensional to make copying faster (2-dimensional copying takes longer) and the output array is treated as 1-dimensional because this routine computes its dimensions. (calguide) METER TYPE=C*1 INSTRUMENT=HRS FILETYPE=SCI observation terminated by exposure meter? (Y or N): MINWAVE TYPE=R*8 INSTRUMENT=FOS FILETYPE=SCI UNITS=ANGSTROMS maximum wavelength: MINWAVE TYPE=R*8 INSTRUMENT=HRS FILETYPE=SCI UNITS=ANGSTROMS maximum wavelength: MIR_REVR TYPE=L*4 INSTRUMENT=ALL FILETYPE=IMG is the image mirror reversed: MNF_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI mean filter of background spectra: Use a mean filter on the background. This routine performs a mean filter of the background with a user-specified (i.e., specified in the table) filter width. The edge points are filled with the value of the closest position that can be filtered. (calguide) MODE TYPE=C*18 INSTRUMENT=HSP FILETYPE=IMG instrument mode SCP, SSP, ARS: instrument mode for hsp: SCP = single color photometry, SSP = star/sky photometry, ARS = area scan, DUM = a dump; wfpc: FULL = full-resolution (800X800), AREA = area-integration (400x400); fos: modes specify how the data should be calibrated: target acquisition, spectroscopy, rapid-readout, time-tagged, time-resolved, spectropolarimetry. hrs: direct readout, accumulation, target acquisition [qexposure.mode] MODHFILE TYPE=C*18 INSTRUMENT=FOC FILETYPE=SCI UNITS=FILENAME Reseau Mark Model Files (MOD): A reseau mark model data file contains from one to fifty models of reseau marks. A reseau mark model is a small image file containing a reseau mark in the center and just a few background pixels around the edge. It is used during the reseau calibration. Each group of a reseau mark model file has the form of a miniature rectangular image, i.e., a reseau mark model which is used to determine the actual location of each reseau mark listed in the reseau reference file. Modified Julian Date TYPE=R*8 INSTRUMENT=ALL FILETYPE=ALL Universal Time is defined as time since 00:00 17-Nov-1858, in 100-nanosecond units. This is the Smithsonian base date & time for the astronomical calendar. The Modified Julian Date (MJD) is defined as time since 00:00 17-Nov-1858, in units of days and fractions of a day. (cgamjd) MOD_CORR TYPE=C*8 INSTRUMENT=FOS FILETYPE=IMG ground software mode dependent reductions: Perform ground software mode-dependent reductions for time-resolved, spectropolarimetry, and rapid-readout observations. The following processing steps are performed in addition to the standard case and spectroscopy mode calibration steps. Rapid-Readout: The total and its statistical error for each frame are calculated. Time-Resolved: The average of all slices (bins) and the differences from the average for each slice (bin) of the last frame of time-resolved data are computed. Spectropolarimetry: The spectropolarimetry reductions require the Wollaston and Waveplate parameter table, ccs4, and the retardation reference file, rethfile. On an initial pass, the reference data is read. On all calls to the special processing routine, the flux and errors are saved for use on the last call---in which the processing is done. The Stokes parameters, linear and circular polarization, and the polarization angle (theta) for FOS polarimetry data are computed. Interference is corrected using the coefficients in ccs4 and theta is changed to sky coordinates by adding PANGAPER. If you are truly interested in how this works, talk to Rich Allen. (calguide) MOONANGL TYPE=R*4 INSTRUMENT=ALL FILETYPE=SCI UNITS=DEGREES angle between moon and V1 axis (deg): Computed as: moonangle = cosd(declmoon) * cosd(declnv1) * cosd(rtasmoon - rtascnv1) + (sind(declmoon) * sind(declnv1)) moonangle = acosd (moonangle) (cgaang) MTFLAG TYPE=C*1 INSTRUMENT=ALL FILETYPE=SHP moving target flag; t => this is a moving target. [qobservation.mt_flag] MT_LVi_k TYPE=C*68 INSTRUMENT=ALL FILETYPE=SHP moving target information: Proposer comments on moving targets (i=1..3, k=1..5). Extracted directly from the pepsi/sogs relation qtcomments. MU_DEC TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=???? expected DEC proper motion: MU_EPOCH TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=???? epoch of the proper motion: MU_RA TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=???? expected RA proper motion: NAXIS TYPE=I*2 INSTRUMENT=ALL FILETYPE=ALL UNITS=COUNT number of data axes: NAXIS1 TYPE=I*2 INSTRUMENT=ALL FILETYPE=ALL UNITS=PIXELS length of 1st data axis: NAXIS2 TYPE=I*2 INSTRUMENT=ALL FILETYPE=IMG UNITS=LINES length of second data axis (lines per image): NBINS TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI UNITS=COUNT number of substep bins in this pattern: NCHNLS TYPE=I*2 INSTRUMENT=FOS FILETYPE=SCI UNITS=COUNT number of channels: ACTUAL FLAGS AND INDICATORS COMMON (FOS keyword: NCHNLS). The number of channels to be processed: 2,4,...,512 or -1 for error. [qexposure.nchnls] NETHFILE TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Wavelength Net Files (NET): The wavelength net files contain data that are used to perform HRS absolute flux calibration. These data provide the non-uniform interpolation net (grid) used to compute an absolute sensitivity scale from data in the HRS absolute sensitivity files. Wavelength net files contain two groups of data that correspond to the large and small apertures of the HRS. Because the HRS absolute sensitivity files contain the absolute sensitivities corresponding to the wavelength net values, these two sets of files have exactly the same structure. Data in the wavelength net files are stored in REAL*4 format. NINIT TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI number of initial deflections: NMCLEARS TYPE=I*4 INSTRUMENT=FOS FILETYPE=IMG number of memory clears per acquisition: NOISELM TYPE=I*4 INSTRUMENT=FOS FILETYPE=SCI burst noise rejection limit: NO_LINES TYPE=I*4 INSTRUMENT=ALL FILETYPE=SHP number of lines per scan (1-99): NPAT TYPE=I*4 INSTRUMENT=FOS FILETYPE=SCI number of patterns per readout: NPDECTRG TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES planetographic coordinate system parameters: declination of north pole of planetary target. [qobservation.north_dec] NPRATRG TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES north pole right ascension of target: NREAD TYPE=I*4 INSTRUMENT=FOS FILETYPE=IMG number of readouts per memory clear: NSHUTA17 TYPE=I*4 INSTRUMENT=WFP FILETYPE=SCI Number of AP17 shutter B closes: NXSTEPS TYPE=I*2 INSTRUMENT=FOS FILETYPE=IMG number of x steps: ACTUAL FLAGS AND INDICATORS COMMON (FOS keyword: NXSTEPS). The number of xsteps per ystep: 1,...,32 or -1 for error. [qexposure.nxsteps] OBSERVTN TYPE=C*4 INSTRUMENT=ALL FILETYPE=SHP observation number (base 36): OBSET_ID TYPE=C*2 INSTRUMENT=ALL FILETYPE=SHP observation set id: The observation set id, these are numbered sequentially throughout the proposal. A base 36 number which allows for 1295 observation sets. [qobservation.obset_id] OBSINT TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI intermediate readout number: OBSMODE TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI observation mode: 'DIRECT READOUT' if proposed mode is 'RAPID','ENGINEERING', 'PULSE-HEIGHT', 'THRESHOLD'; 'ACCUMULATION' if proposed mode is 'ACCUM','OSCAN','WSCAN', 'PHOTOSCAN'; 'TARGET ACQUISITION' if proposed mode is 'ACQ','IMAGE','DEFCAL', 'ACQ/PEAKUP'. (tguide 7.0-12) OBSRPT TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI observation repeat number: OBSSTRTT TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=SECONDS predicted obs. start time (seconds since 01/01/1985) OBSSTRTT is the predicted start time PSTRTIME (which comes from the relation qobservation) converted to sogs_seconds (seconds since 01-jan-1980 00:00:00.00) less the number of seconds between 1980 and 1985 (157852800). (cecosp) OFFS_TAB TYPE=CHR INSTRUMENT=FOS FILETYPE=SCI GIMP offsets (post-pipeline processing only): OFF_CORR TYPE=CHR INSTRUMENT=FOS FILETYPE=SCI Perform GIMP correction: OPFORMAT TYPE=C*18 INSTRUMENT=ALL FILETYPE=SHP output product format specification: OPMODE TYPE=C*15 INSTRUMENT=ALL FILETYPE=SHP proposed operation mode: OPTCRLY TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI optical relay: F48, F96: optical relay: F48,F96,F288. These are the three possible magnifications in which the camera operates. [qexposure.optcrly] OPTELTn TYPE=I*2 INSTRUMENT=FOC FILETYPE=SCI This specifies which filter or optical element was used on (F48,F96) wheel n: 0,...,11. (wheel n=1..4) ORIENTAT TYPE=R*4 INSTRUMENT=ALL FILETYPE=IMG the orientation of the image (deg): OUTDTYPE TYPE=C*6 INSTRUMENT=WFP FILETYPE=SCI Output image datatype: REAL, LONG, SHORT: Select the data type of the output (.c0h) image. The allowed options are REAL, SHORT, and LONG corresponding to single-precision real, short integer, and long integer pixels. The data is scaled with the keywords WSCALE and WZERO if the SHORT or LONG option is selected. (calguide) OVERSCAN TYPE=I*2 INSTRUMENT=FOS FILETYPE=SCI overscan number: ACTUAL FLAGS AND INDICATORS COMMON (FOS keyword: OVERSCAN). The overscan number: 1,2,3,4,...,256 or -1 for error. PARALLAX TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSECS expected parallax of target: (0.,1000.)... target parallax in arcsec (1 x 10e-3 precision) the change in direction of a celestrial object which results from the change from heliocentric to geocentric coordinate systems. (default = zero). [qtargets.parallax] PAR_CORR TYPE=C*1 INSTRUMENT=ALL FILETYPE=SHP UNITS=T/F parallax correction used (T or F): PASS_DIR TYPE=I*4 INSTRUMENT=FOS FILETYPE=IMG polarization pass direction: PA_APER TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES position angle of aperture used with target (deg): This value is as input from the ground, not spacecraft measured. FOS: In the right-handed XY coordinate system of the detector, this is the angle one rotates the image CW in order for North to coincide with +Y. (if you're working in left-handed XY at the detector, rotate CCW.) (ETS-g) PA_REF TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES pos. angle of target from ref. object (deg): PA_V3 TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES position angle of v3 axis of st (deg): PCOUNT TYPE=I*2 INSTRUMENT=ALL FILETYPE=ALL UNITS=COUNT number of group parameters: PDTYPEi TYPE=CHR INSTRUMENT=ALL FILETYPE=ALL Data type of the group parameter number i. This is a required FITS keyword. PEP_EXPO TYPE=C*15 INSTRUMENT=ALL FILETYPE=SHP PEP exposure identifier including sequence: PEQUINOX TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP equinox of the celestial coordinate system (from proposal): PFILTERi TYPE=I*2 INSTRUMENT=WFP FILETYPE=SCI Preflash Filter i number (0-48): (i=1..2) PHCHFILE TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Photocathode Response Files (PHC): Non-uniformities in the responses of the photocathodes of the HRS detectors require science data to be normalized using data from the photocathode response files. Photocathode response files contain multiple groups of responses. Each group contains the responses for a particular line position. Within the group, responses are ordered by equally spaced sample positions determined by the keywords SAMPBEG and SAMPOFF. Photocathode responses are stored as REAL*4 values. PHC_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI removal of photocathode nonuniformity: Remove photocathode nonuniformity by dividing the count value by the photocathode response contained in the phchfile file. This routine removes the photocathode granularity using a reference file that has a granularity map. This map has a granularity vector for multiple line positions. At each line position the granularity is tabulated with a constant starting sample for all lines and a constant delta sample. To compute the response for the data's line and sample, bilinear interpolation is used within the reference file. If Doppler compensation is specified, the response is smoothed by a weighting function describing the motion of the data samples along the photocathode. (This calibration will only be known initially for a very few selected wavelength ranges. Using FPSPLITS will generally be required for high S/N work.) (calguide) PHOTBW TYPE=R*4 INSTRUMENT=ALL FILETYPE=SCI UNITS=ANGSTROMS RMS Bandwidth of the Filter and Detector: PHOTBW is a measure of the root-mean-square width of the passband P(lam). The rms bandwidth is defined as in the WF/PC instrument handbook: rmslam^2 = barlam^2 <[ln(lam/barlam)]^2> , where barlam is the bar wavelength, defined by Schneider, Gunn and Hoessel ( 1983 ApJ 264,337 ) as barlam = exp() , and < > denotes an average over the passband in ln(lam) = ( Int P(lam) X(lam) dlam/lam ) / ( Int P(lam) dlam/lam ) . Note that the dimensionless bandwidth is (rmslam/barlam)^2 = < [ln( lam/barlam)]^2 > = < [ln(lam) - ]^2 >, = - ^2 . The latter formula is used in the numerical calculation below. [Koornneef et al. (1986), Horne (1988)] PHOTFLAM TYPE=R*4 INSTRUMENT=ALL FILETYPE=SCI Inverse Sensitivity: (erg/cm^2/s/Angstrom) PHOTFLAM is the flux-density that produces a count rate of 1 per second with the HST observing mode. Multiply an observed count rate by PHOTFLAM to get the mean broad-band flux-density of the target in the passband with which the target was observed. In terms of the spectral energy distribution of the target FLAM(LAM), and the passband sensitivity vs wavelength P(LAM), the mean broad-band flux density is given by: INTEGRAL ( FLAM(LAM) * P(LAM) * LAM * DLAM ) FLAM(P) = ------------------------------------------- INTEGRAL ( P(LAM) * LAM * DLAM ) Even when the spectral energy of the target is unknown, this mean flux density is exactly determined by the measured count rate in the passband. [Koornneef et al. (1986), Horne (1988)] PHOTMODE TYPE=C*8 INSTRUMENT=ALL FILETYPE=SCI Photometric Mode: PHOTMODE is a character string giving a list of keywords that specify the HST observing mode. For example, WF,1,F336W FOC,F/96,F195W FOS,BLUE,G160L,1.0 HSP,UV1,F248M,A are all valid PHOTMODEs. The PHOTMODE is used by the STSDAS.SYNPHOT package to look up the passband P(LAM) (sensitivity vs wavelength) of the observing mode. [Koornneef et al. (1986), Horne (1988)] PHOTPLAM TYPE=R*4 INSTRUMENT=ALL FILETYPE=SCI UNITS=ANGSTROMS Pivot Wavelength: The pivot wavelength is the wavelength at which a broad-band flux converts exactly between FNU and FLAM units. It does not depend on the spectrum of the target observed, but only on the shape of the observing passband P(LAM). The definition of the pivot wavelength is LAM_P = SQRT( < LAM > / < 1/LAM > ) where < LAM > = ( INTEGRAL P(LAM)*LAM*DLAM ) / ( INTEGRAL P(LAM)*DLAM ) and < 1/LAM > = ( INTEGRAL P(LAM)*DLAM/LAM ) / ( INTEGRAL P(LAM)*DLAM ) [Koornneef et al. (1986), Horne (1988)] PHOTTAB TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI name of the photometry keyword reference table: PHOTZPT TYPE=R*4 INSTRUMENT=ALL FILETYPE=SCI ST magnitude zero point: PHOTZPT is the zero-point of the ST magnitude system. The ST magnitude is STMAG = -2.5 * LOG_10( FLAM ) + 21.10, thus constant STMAG corresponds to constant FLAM, and the zero-point is PHOTZPT = -21.10. This value is chosen so that Vega has an ST magnitude of zero for the Johnson V passband. If the absolute calibration of Vega changes, this value may also change slightly. [Koornneef et al. (1986), Horne (1988)] PKTFMT TYPE=I*4 INSTRUMENT=ALL FILETYPE=ALL packet format code: WFPC: Type of Exposure WF PC ---------------- ----- ----- EXTERNAL '60'X '61'X w/PREFLASH '62'X '63'X w/PURGE '64'X '65'X w/PURGE & PREFLASH '66'X '67'X EXTERNAL '68'X '69'X with Serial Clocks On w/PREFLASH '6A'X '6B'X with Serial Clocks On w/PURGE '6C'X '6D'X with Serial Clocks On w/PURGE & PREFLASH '6E'X '6F'X with Serial Clocks On BIAS '20'X '28'X DARK '21'X '29'X INTFLAT '22'X '2A'X EXTFLAT '23'X '2B'X KSPOT '24'X '2C'X UVFLOOD '25'X '2D'X DARK w/CLOCKS=ON '26'X '2E'X PREFLASH '27'X '2F'X PKTTIME TYPE=R*8 INSTRUMENT=ALL FILETYPE=ALL time from the packet ancillary data: Each packet contains ancillary information including a spacecraft time code value. This value contains the spacecraft time associated with the SHP (standard header packet) which contains ancilliary data. PLY_CORR TYPE=CHR INSTRUMENT=HRS FILETYPE=SCI polynomial smoothing of background spectra: PODPSFF TYPE=C*1 INSTRUMENT=ALL FILETYPE=SCI 0=(no podps fill), 1=(podps fill present): POLANG TYPE=R*4 INSTRUMENT=FOS FILETYPE=SCI initial angular position of polarizer: POLAR_ID TYPE=C*1 INSTRUMENT=FOS FILETYPE=SCI polarizer id: A: polarizer A; B: polarizer B; C: no polarizer; E: error. POSTNSTX TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KILOMETERS position of space telescope x axis (km): X axis coordinate of the space telescope position in orbit at the time of observation. In geocentric J2000.0 inertial coordinate system. This is a orthogonal right handed coordinate system centered in the earth, with the X axis pointing towards the vernal equinox for the year 2000, the Z axis pointing towards the north celestial pole for the year 2000, and the Y axis orthogonal to both. POSTNSTY TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KILOMETERS position of space telescope y axis (km): Y axis coordinate of the space telescope position in orbit at the time of observation. In geocentric J2000.0 inertial coordinate system. This is a orthogonal right handed coordinate system centered in the earth, with the X axis pointing towards the vernal equinox for the year 2000, the Z axis pointing towards the north celestial pole for the year 2000, and the Y axis orthogonal to both. POSTNSTZ TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KILOMETERS position of space telescope z axis (km): Z axis coordinate of the space telescope position in orbit at the time of observation. In geocentric J2000.0 inertial coordinate system. This is a orthogonal right handed coordinate system centered in the earth, with the X axis pointing towards the vernal equinox for the year 2000, the Z axis pointing towards the north celestial pole for the year 2000, and the Y axis orthogonal to both. PPC_CORR TYPE=C*8 INSTRUMENT=FOS FILETYPE=SCI TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI paired pulse correction: Correct the raw count rates for saturation in the detector electronics using table coccg2r, which contains the paired-pulse correction table. On the first call, the paired pulse parameters are read from table ccg2. The following equation is used: x = y/(1-yt) Where: x -- is the true count rate, y -- is the observed count rate, t = q0 if y is less than or equal to F, and t = q0 + q1 * (y - F) if y is greater than F. q0, q1, and F are coefficients in ccg2r. This is a standard calibration step. (calguide) PRECISN TYPE=CHR INSTRUMENT=HRS FILETYPE=IMG number of diodes used to map (HIGH=1,NORMAL=2): PREFCORR TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Do preflash correction: YES, NO, DONE: If the value in keyword PREFTIME is less than zero, the preflash image reference file is scaled and subtracted from the input science image. The preflash image is multiplied by the preflash lamp exposure time (obtained from the keyword PREFTIME in the input science image header and expressed in seconds) and then subtracted from the input science image. If the keyword PREFTIME = 0, the CTE fixup is applied. The names of the preflash or CTE image and its DQF must be provided in the keywords PREFFILE and PREFDFIL. (calguide) PREFDFIL TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI name of the preflash reference DQF: PREFFILE TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI UNITS=FILENAME Preflash Files (PRF): The WF/PC Preflash Reference File and its associated data quality file are used to remove the signal introduced by the preflash lamp. This signal is removed by subtracting this reference file. The reference file is scaled by the preflash exposure time to allow for variations in the requested preflash exposure. The subtraction of the reference file corrects for the uneven illumination pattern of the preflash image. Since the preflash is obtained by illuminating the backside of the shutter with an internal lamp, the difference in reflectivity of the two shutter blades requires reference files specific to each shutter blade. The PREFDFIL is the name of the preflash reference data quality file. PREFTIME TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI UNITS=SECONDS Predicted preflash time in seconds: PRE_AMP TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI UNITS=COUNTS/SEC scaled tube pre-amp contribution: Pre-amplifier noise, in counts/seconds. Calculated by the calibration software. (calhsp) PROC_TYP TYPE=C*6 INSTRUMENT=ALL FILETYPE=ALL level of reprocessing (NORMAL, MINOR, MAJOR): If the keyword is set to MINOR the proprietary date in DADS will not be changed and the data will not be automatically distributed to the Guest Observers (GOs). If the keyword is set to MAJOR the proprietary date in DADS will be reset as if this were new data the data will be automatically distributed to the GO as if it were new data. PRODTYPE TYPE=C*18 INSTRUMENT=ALL FILETYPE=SHP output product medium type: PROGRMID TYPE=C*4 INSTRUMENT=ALL FILETYPE=SHP A base 36 program id assigned by the pm software to a proposal that has been accepted. (1-46,655 possible ids) PROPOSID TYPE=I*4 INSTRUMENT=ALL FILETYPE=ALL PEP proposal identifier: PR_INV_F TYPE=C*18 INSTRUMENT=ALL FILETYPE=SHP first name of principal investigator: PR_INV_L TYPE=C*18 INSTRUMENT=ALL FILETYPE=SHP last name of principal investigator: PR_INV_M TYPE=C*1 INSTRUMENT=ALL FILETYPE=SHP middle initial of principal investigator: PSIZEi TYPE=I*2 INSTRUMENT=ALL FILETYPE=ALL number of bits allowed for the group parameter number i. This is a required FITS keyword. PSTPTIME TYPE=C*17 INSTRUMENT=ALL FILETYPE=SHP UNITS=DATE yyyy.ddd:hh:mm:ss ... Predicted date and time of end of execution where yyyy is year, ddd is day of year, hh is hour, mm is minutes, ss is seconds. [qobservation.pred_stop_tm] PSTRTIME TYPE=C*17 INSTRUMENT=ALL FILETYPE=SHP UNITS=DATE yyyy.ddd:hh:mm:ss ... Predicted date and time of start of execution where yyyy is year, ddd is day of year, hh is hour, mm is minutes, ss is seconds. [qobservation.pred_strt_tm] PTSRCFLG TYPE=C*1 INSTRUMENT=HSP FILETYPE=SCI P/E...HSP point source flag. P = Point (default), E = Extended. [qexposure.pt_src_flg] PTYPEi TYPE=CHR INSTRUMENT=ALL FILETYPE=ALL Name of the group parameter number i. This is a required FITS keyword. See the definition for that group parameter name. PT_EFFIC TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI scaled point source cathode efficiency: Point source sensitivity relative to that of the reference aperture, unitless. This keyword is filled by the calibration software only when the target is a point source. PURGCORR TYPE=C*8 INSTRUMENT=WFP FILETYPE=SCI Do purge correction: YES, NO, DONE: The names of the superpurge image and its DQF must be provided in the keywords PURGFILE and PURGDFIL. The scaling is obtained from the keywords DARKTIME and PURGTIME. (calguide) PURGDFIL TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI name of the purge reference DQF: PURGFILE TYPE=C*18 INSTRUMENT=WFP FILETYPE=SCI UNITS=FILENAME Superpurge Files (SPG): The WF/PC superpurge reference file and its associated data quality file are used in the superpurge calibration procedure. The superpurge procedure removes residual images of highly overexposed sources. However, it creates a non-uniform residual image over the entire detector which decays with time. The level of this global residual image in a readout depends upon both the time since the purge was performed and the time since the last erase prior to the readout. The superpurge reference file must be scaled and subtracted from all images obtained after a superpurge in which the residual is still significant. The PURGDFIL is the name of the purge reference data quality file. PURGTIME TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI UNITS=SECONDS Time since last SuperPurge (seconds): The time of the observation, which was dredged from qobservation, is used to establish the search limit. 24 hours are subtracted from the current observation time, and a join of qolink and qesiparm is queried to determine if any purge observations were taken within the previous 24 hours. If one is found, the number of seconds is calculated. If none are found, the limit of 24 hours (172800 seconds) is written into the keyword PURGTIME. (cgwprg) PXFORMT TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI format of the image: NORMAL, ZOOM: (pixel size) pixel format: NORMAL: 512 samples, 512 lines 0.022x0.022 arcsec^2 ZOOM: 512 samples, 1024 lines 0.044x0.022 arcsec^2 PXLCORR TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI split zoom-format pixels: Correct for zoom mode. If the image was taken in zoom mode, the next step is to split the data values along the first image axis (the sample direction). For example, suppose the first three digital number values (DN) in the image are A, B, C. The first six DN values of the dezoomed image would be A/2, A/2, B/2, B/2, C/2, C/2. The length of the first axis (NAXIS1) is doubled, and the length of the second axis (NAXIS2) remains unchanged. (calguide) RAD_VEL TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KILOM/SEC (-300,000.,+300,000.)... radial velocity of a star the velocity of a star along the line of sight of an observer. it is calculated directly from the doppler shift in the lines of the stars spectrum. [qtargets.radial_vel] RASCASCN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=REVOLUTIONS Right ascension of ascending node [wiephemeris.rt_asc_node] RA_APER TYPE=R*8 INSTRUMENT=ALL FILETYPE=SCI UNITS=DEGREES right ascension of the aperture (deg): RA_APER1 TYPE=R*8 INSTRUMENT=FOS FILETYPE=SCI UNITS=DEGREES right ascension of the aperture (deg): RA_APER1 TYPE=R*8 INSTRUMENT=HRS FILETYPE=SCI UNITS=DEGREES right ascension of the aperture (deg): RA_MOON TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES right ascension of moon in geocentric J2000.0 coordinates. [qobservation.rtasmoon] RA_REF TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES right ascension of the reference target position. This is in heliocentric J2000.0. [qobservation.ref_obj_ra] RA_SUN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES right ascension of sun in geocentric J2000.0 coordinates. [qobservation.rtascsun] RA_TARG TYPE=R*8 INSTRUMENT=ALL FILETYPE=LOG UNITS=DEGREES Right Ascension of the target. The epoch and equinox of the target position is J2000. For moving target, the epoch of the target position is the predicted start time for the observation. (Fixed - Heliocentric J2000, moving - Geocentric J2000.) (OSS) [qtargets.right_ascsn] RA_V1 TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES right ascension of v1 axis of space telescope in geocentric J2000.0 coordinates. The v1 axis is the optical axis of the space telescope (more or less the 'roll' axis). The epoch of the position of the v1-axis is the predicted start of observation. [qobservation.rtascnv1] RCARGPER TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=REV/SEC Rate of change of the argument of perigee in revolutions per second. [wiephemeris.rt_chng_peri] RCASCNRD TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=RADS/SEC Rate of change of the right ascension of ascending node in radians per second. [wiephemeris.rt_node_rad] RCASCNRV TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=REVS/SEC Rate of change of the right ascension of ascending node in revolutions per second. [wiephemeris.rt_node_rev] REDSHIFT TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=???? expected redshift of target: redshift; a displacement of spectral lines toward longer wavelength values. the redshift of astronomical objects within the galaxy are interpreted as doppler shift caused by movement of the source away from the observer. [qtargets.redshift] RETHFILE TYPE=C*18 INSTRUMENT=FOS FILETYPE=IMG UNITS=FILENAME Retardation Files (RET): The FOS retardation files contain values computed from the retardation of the waveplate used during spectropolarimetric calibration to create observation matrix f(w). ROOTNAME TYPE=C*12 INSTRUMENT=ALL FILETYPE=ALL UNITS=IPPPSSOOT rootname of the observation set: Follows the ipppssoot convention where: i: instrument identifier: V:hsp, W:wfpc, X:foc, Y:fos, Z:hrs ppp: program_id ss : obset_id oo : observation number t : T:tape, R:realtime. ROTRTTRG TYPE=R*4 INSTRUMENT=ALL FILETYPE=ALL UNITS=DEGREES/DAY planetographic coordinate system parameters: rate of change of longitude. [qobservation.long_rate] RPTCDi TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI UNITS=CODE repeat code bin i (i=1..6) where: 0 = no def offset, 1 = every time, 2 = every 2nd time, 4 = every 4th time, 8 = every 8th time. RPTOBS TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI UNITS=COUNT expected number of observation repeats: RSDPFILL TYPE=I*2 INSTRUMENT=WFP FILETYPE=SCI UNITS=FILL_VALUE bad data fill value for calibrated images: RTAMATCH TYPE=C*18 INSTRUMENT=ALL FILETYPE=SHP above f&i match RTA (TRUE,FALSE,NO RTA F&I AVL): If an RTA (Real Time Activity) file for this observation is received, and if the 'Flags and Indicators' which are derived from the support schedule match those in the telemetry, then this flag is set to TRUE. If there are any mismatches, then this flag is set to FALSE. If no RTA file was received for this observation, this field should read 'NO RTA FI AVAILABL'. S0INVMAG TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=1/KM SO inverse magnitude of previous #48 command. (1/kilometers) [qobservation.so_inv] S0XDIR TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=???? SO 'X' direction of previous #48 command. [qobservation.sox_dir] S0YDIR TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=???? SO 'Y' direction of previous #48 command. [qobservation.soy_dir] S0ZDIR TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=???? SO 'Z' direction of previous #48 command. [qobservation.soz_dir] SAAAVOID TYPE=C*2 INSTRUMENT=ALL FILETYPE=SHP UNITS=MODEL_NUM the South Atlantic Anomaly model which was used by spss to schedule saa avoidance. An interger value with range of 02-99. The SAA/RFI region is modelled by a convex polygon, the arcs between whose vertices lie along great circles. The vertices are ordered such that the interior of the SAA/RFI region remains to the left as the boundary of the polygon is traced. [qobservation.saa_model] SAMPBEG TYPE=I*2 INSTRUMENT=WFP FILETYPE=EXT sample number (1st sample: wrt source format): SAMPBEG TYPE=I*2 INSTRUMENT=FOC FILETYPE=QIN sample number (1st sample: wrt source format): SAMPLE TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI sample position: SAMPOFF TYPE=R*4 INSTRUMENT=FOC FILETYPE=SCI sample offset (0.0-1023.75): Sample offset, mnemonic = XCCCUHZO. [qexposure.sampoff] SAMPPLN TYPE=I*2 INSTRUMENT=FOC FILETYPE=SCI samples per line (64, 128, 256, or 512): Number of samples per line [qexposure.samppln] SAMPTIME TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI time of integration (in seconds): SATURATE TYPE=I*2 INSTRUMENT=WFP FILETYPE=SCI Data value at which saturation occurs: SCAN_ANG TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES (0.,360.) position angle of scan line when scan_coord (qexsco) is equal to c, this is the counterclockwise angle, about the beginning of the first scan, from north at the target to the direction of the first scan. when scan_coord is equal to v, this is the counterclockwise angle from the positive v3-axis to the direction of the first scan. (1 x 10e-4 precision) [qexposure.scan_angle] SCAN_COR TYPE=C*1 INSTRUMENT=ALL FILETYPE=SHP c/v...flag to indicate the scan coordinate frame of reference c = celestial frame (ra-dec), v = vehicle (v1v2v3). [qexposure.scan_coord] SCAN_LEN TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSECONDS scan length ( 0.,3600.) in arcseconds. [qexposure.scan_length] SCAN_RAT TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSEC/SEC scan rate ... the commanded constant rate of the line scan (slew of the st optical axis from point a to b on the celestial sphere). [qexposure.scan_rate] SCAN_TYP TYPE=C*1 INSTRUMENT=ALL FILETYPE=SHP c/d/n ... continuous/dwell... scan type where c = a series of linear scans alternating in direction and offset from one another by a small angle separation (a linear scan is a slew of the st optical axis from point a to b on the celestial sphere at a constant commanded rate); d = like continuous with a specified number of dwell points per line and time to wait at each dwell point; n = not applicable. [qexposure.scan_type] SCAN_WID TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSECONDS scan width (0.,3600.) in arcseconds. [qexposure.scan_width] SCIDATA TYPE=L*1 INSTRUMENT=HRS FILETYPE=SHP science data present (T/F) (actual not predicted): SCIDMP TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI intermediate data dump (-1 = nodump): Number of substep patterms between intermediate data dumps (-1 for no intermediate dumps) SE-01p3-267 SCLAMP TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI spectral calibration lamp: SDECORR TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI spectrograph de correction: Apply spectrographic detector efficiency correction. This correction is only applied to spectrographic images. It includes both the flat-field correction and a conversion from counts to flux density. It is applied after geometric correction because the absolute sensitivity depends on wavelength, and a major function of the geometric correction for spectrographic images is to align the spectrum with the axes and set the dispersion. The correction is applied by multiplying by a spectrogaphic detector efficiency reference file. The use of an order-selecting filter can change the location of a given wavelength on the photocathode, so there are several reference files; the appropriate one is selected based on the filters used. These files are full-frame (1024 x 1024), so only a subset will be used if the science image is smaller than 1024 x 1024. (calguide) SDEHFILE TYPE=C*18 INSTRUMENT=FOC FILETYPE=SCI UNITS=FILENAME Spectrographic Detector Efficiency Files (SDE): The spectrographic detector efficiency data files are used for the spectrographic DE calibration step. A spectrographic DE data file has the same form as an FOC image. It always has dimensions 1024 samples by 1024 lines. Each entry is a REAL*4 scaling factor that is used to multiply the corresponding pixel DN count in the FOC science data file that is to be corrected. All images to be corrected will find their proper position inside the chosen spectrographic DE data file. SDMA3SQ TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=radians/second**2 3 * (SDMEANAN**2) SDMEANAN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=REVS/SEC/SEC 2nd derivative coef for mean anomly (revs/sec/sec): SEMILREC TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=METERS Semi-latus rectum [wiephemeris.semilat_rect] SEQLINE TYPE=C*15 INSTRUMENT=ALL FILETYPE=ALL PEP line number of defined sequence: SEQNAME TYPE=C*15 INSTRUMENT=ALL FILETYPE=ALL PEP define/use sequence name: SERIALS TYPE=C*3 INSTRUMENT=WFP FILETYPE=SCI serial clocks: ON, OFF: Determined by PODPS on the basis of the packet format code of the observation. Serial clocks are on if the packet format code = '68'x. (cgwsdh) SGESTAR TYPE=C*12 INSTRUMENT=ALL FILETYPE=SHP the fgs id (f1, f2, f3) concatenated with the subdominant gs id. [qobservation.subdominant] SHTMODE TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI shutter mode: INBEAM, NOTUSED: [qexposure.shtmode] SHUTTER TYPE=C*7 INSTRUMENT=WFP FILETYPE=SCI Shutter in place during preflash: A, B, UNKNOWN: SIMPLE TYPE=L*1 INSTRUMENT=ALL FILETYPE=ALL image conforms to the fits standard: SINEINCL TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP Sine of the orbit inclination angle. [wiephemeris.sin_orb_incl] SKY_CORR TYPE=C*8 INSTRUMENT=FOS FILETYPE=SCI sky subtraction: Subtract the sky from the object spectrum. If the sky was observed, the flat-fielded sky spectrum is smoothed with a median filter once and a mean filter twice---except in known regions of emission lines. The spectrum is then scaled by the aperture size, and shifted so that the wavelength scales of the object and sky are matched. The sky spectrum is then subtracted from the object spectra. This routine requires table ccs3 containing the filter widths, the aperture size table, ccs0, the emission line position table, ccs2, and the sky shift table, ccs5. This step is a spectroscopy mode calibration step. (calguide) SLICES TYPE=I*4 INSTRUMENT=FOS FILETYPE=SCI number of time slices: SMMMODE TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI spectrographic mirror mechanism: INBEAM,NOTUSED. [qexposure.smmode] SOFTERRS TYPE=I*4 INSTRUMENT=WFP FILETYPE=SCI UNITS=COUNT number of "soft error" pixels (DQF=1): SOPNTIME TYPE=R*8 INSTRUMENT=WFP FILETYPE=SCI UNITS=MJD First shutter open time (Modified Julian Date): SPCLINCN TYPE=I*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=MJD spacecraft clock at UTC0: Value of the counter which is keeping count of the number of 0.125 second ticks of the spacecraft clock. This value is as input from the ground. It is updated only after spacecraft safings and/or when the difference in spacecraft time from a POCC time `obtained from White Sands' is > 10msec. (ETS-a) SPEC_i TYPE=C*20 INSTRUMENT=ALL FILETYPE=SHP spectral element i: (i=1..4) SPORDER TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI spectral order: SP_TYPE TYPE=C*15 INSTRUMENT=ALL FILETYPE=SHP spectral type: SRCHSIZE TYPE=I*2 INSTRUMENT=HRS FILETYPE=IMG width of spiral-search in dwell points: STATICD TYPE=I*4 INSTRUMENT=WFP FILETYPE=SCI UNITS=COUNT number of "static defect" pixels (DQF=4): STDCFFF TYPE=C*1 INSTRUMENT=ALL FILETYPE=SCI 0=(no st dcf fill), 1=(st dcf fill present): STDCFFP TYPE=C*4 INSTRUMENT=ALL FILETYPE=SCI st dcf fill pattern (hex): STEPPATT TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI step pattern sequence: STEPTIME TYPE=I*2 INSTRUMENT=HRS FILETYPE=SCI integration time at step pattern position (sec): SUNANGLE TYPE=R*4 INSTRUMENT=ALL FILETYPE=SCI UNITS=DEGREES angle between sun and V1 axis (deg): Computed as: sunangle = cosd(declnsun) * cosd(declnv1) * cosd(rtascsun - rtascnv1) + (sind(declnsun) * sind(declnv1)) sunangle = acosd (sunangle) (cgaang) SUN_ALT TYPE=R*4 INSTRUMENT=ALL FILETYPE=SCI UNITS=DEGREES altitude of the sun above Earth's limb (deg): The algorithm calculates the altitude using the rectangular coordinates of HST and the coordinates of the sun from the SHP header. For a long exposure, this wouldn't be as useful as, say, the maximum altitude of the sun during the exposure. The other problem of this algorithm is that it assumes a spherical earth, which results in an error of about 0.4 degrees. Another effect is that it ignores atmospheric refraction. This will be very small at high altitudes but can be as large as one degree near the horizon. (cgasun) SURFALTD TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=KILOMETERS planetographic coordinate system parameters: altitude of surface feature. [qobservation.feature_alt] SURFLATD TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES planetographic coordinate system parameters: latitude of surface feature. [qobservation.feature_lat] SURFLONG TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES planetographic coordinate system parameters: longitude of surface feature. [qobservation.feature_long] SURF_B TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP expected B surface brightness: SURF_R TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP expected R surface brightness: SURF_U TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP expected U surface brightness: SURF_V TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP expected V surface brightness: T51_ANGL TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=DEGREES position angle of motion of aperture (deg): This parameter is determined only for moving targets (TARGET_TYPE=M). The position angle in degrees from North towards East of the angular velocity which is arctan( a_E, a_N ) converted to degrees. (cect51) [a_N, a_E: angular velocity in the North and East directions] T51_RATE TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSECS/SEC rate of motion commanded (arcsecs/sec): This parameter is determined only for moving targets (TARGET_TYPE=M). The magnitude of the angular velocity is sqrt(a_N**2 + a_E**2) [a_N, a_E: angular velocity in the North and East directions] times the conversion factor from radians to arcseconds. (cect51) TARAQMOD TYPE=C*2 INSTRUMENT=ALL FILETYPE=SHP (00-03)...the target acquisition mode used for the observation. Where 00 = null, 01 = ground assisted, 02 = onboard computer assisted, 03 = fixed simple pointing. [qobservation.target_acqmd] TARDESCR TYPE=C*68 INSTRUMENT=ALL FILETYPE=SHP target description: The Target Description will be one of the key fields used by archival researchers in searching through the HST data archive; thus it is important that the information be filled out completely and accurately for each target, and following a well-defined format. Each target should be assigned one and only one Target Category. This should be followed by as many Target Keywords (at least one is required) as are relevant. (PROP_INST--SEC_5.TEX;1) TARGCAT TYPE=C*24 INSTRUMENT=ALL FILETYPE=SHP target category: STAR Galactic stellar object STAR CLUSTER Galactic star cluster, group, or association INTERSTELLAR MEDIUM Galactic gas or dust EXT-STAR Star in an external galaxy EXT-CLUSTER Star cluster in an external galaxy EXT-MEDIUM Interstellar medium in an external galaxy GALAXY Galaxy, AGN, or QSO GALAXY CLUSTER Cluster or group of galaxies (PROP_INST--SEC_5.TEX;1) TARGDIST TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM distance to target from Earth's center (km): This parameter is determined only for moving targets (TARGET_TYPE=M). This is calculated using the time of the observation and the Chebychev coefficients for that target. The software determines the geocentric position data for position (3-vector in kilometers) and velocity (3-vector in kilometers per second). The target distance is the norm of the position vector. (cect51) TARGNAME TYPE=C*30 INSTRUMENT=ALL FILETYPE=SHP proposer's target name: TARKEYi TYPE=C*24 INSTRUMENT=ALL FILETYPE=SHP target key description number i: (i=1..10) Key description entered by the proposer. TAR_TYPE TYPE=C*1 INSTRUMENT=ALL FILETYPE=SHP P/A/M/G/I.....specifies the target type where P = point target, A = area target, G = generic target, M = moving target. [qtargets.target_type] TECTEMP TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI TEC temperature (Celcius): THRESH TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL PAD (Pulse Amplitude Discriminator) threshold setting for the object detector: TIME-OBS TYPE=C*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=MJD UT time of start of observation (hh:mm:ss): PODPS calcuted time using packet times generated at the spacecraft at the time of the data measurement. The seconds place is not always accurate as the fractions of a section information is discarded rather than used for rounding. (ETS-d) FOS: merely the FPKTIME translated from MJD (keeping only whole seconds) see EXPSTART for relation to shutter opening. (ETS-d) WFPC: Note that this is not necessarily the start of the exposure. For example, the WFPC observation starts on a major frame pulse, while the exposure actually starts 16.4 seconds later following a memory clear. See EXPSTART. TIMEBIAS TYPE=I*4 INSTRUMENT=HSP FILETYPE=SCI instrument time bias (in 1/1.024 microseconds): The value of the time biases that is used to correct the integration time for internal instrument delays. The timebias is a function of the particular HSP data format (BYTE, WORD, LWRD, ALOG, or ALL) and the instrument mode (SCP, ARS, SSP1, or SSP2). (cgptme) TIMEFFEC TYPE=C*30 INSTRUMENT=ALL FILETYPE=SHP UNITS=SECONDS The time the parameters took effect onboard; given in the form of the number of seconds since 1/1/85. [wiephemeris.time_effect] TRAILER TYPE=L*1 INSTRUMENT=FOS FILETYPE=SCI reject array exists: TRK_TYPE TYPE=C*3 INSTRUMENT=ALL FILETYPE=SHP track 48 or track 51 commanding used (T48, T51, NO): specifies the st pointing mode. if the pointing mode is track, the target must be a moving target, and optimal gs hand-off sequences will be generated in the response for tracking the target. see [qalignment.pointing_mode] (cecqal) TRUE_CNT TYPE=C*8 INSTRUMENT=HSP FILETYPE=SCI compute the true count rates: Compute the true count rates. This switch applies only to digital data, it has no effect on analog data. True counts are corrected according to the following equation: z = (y-d-e)/(h*r) Where: z is the final calibrated true count rate, y is the observed count rate, d is the dark signal, e is the pre-amplifier noise, h is the high-voltage factor, and r is the relative sensitivity. If the target is an extended source (i.e., the value of the header keyword PTSRCFLG is "E"), z is further divided by the aperture area. (calguide) TRUE_PHC TYPE=C*8 INSTRUMENT=HSP FILETYPE=SCI compute the true photocurrents: Compute the true photocurrents. This switch applies only to analog data, it has no effect on digital data. True photocurrents are corrected by the following equation: z = ((y-i)/g - d - e)/(h*r) Where: z is the final calibrated true count rate, y is the observed digital number, i is the CVC offset, g is the gain factor, d is the dark signal, e is the pre-amplifier noise, h is the high-voltage factor, and r is the relative sensitivity. If the target is an extended source (i.e., the value of the header keyword PTSRCFLG is "E"), z is further divided by the aperture area. (calguide) TUBEGAIN TYPE=R*4 INSTRUMENT=HSP FILETYPE=SCI scaled tube gain factor: Gain factor used to convert digital numbers (DN) in the analog mode to count rates, in DN/(counts/second). This keyword is filled by the calibration software only for analog data files. (calhsp) UNICORR TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI uniform de correction: Flat field correction (normal images only). This correction is called the uniform detector efficiency correction, and it is applied by multiplying by the uniform detector efficiency reference file, which is the reciprocal of a flat field. These reference files are full-frame in size, which is 1024 x 1024 because we have dezoomed. As with the dark-count correction, if the science image is smaller than full-frame then only a subset of the reference file is used. (calguide) UNIHFILE TYPE=C*18 INSTRUMENT=FOC FILETYPE=SCI UNITS=FILENAME Uniform Detector Efficiency Files (UNI): The uniform Detector Efficiency (DE) files---also known as relative detector efficiency files---contain data used to remove the FOC instrument's spatial non-uniformities from the FOC science data. This step is known as the uniform DE calibration. A uniform DE file has the same form as an FOC image. It always has dimensions 1024 samples by 1024 lines. Each entry is a REAL*4 scaling factor used to multiply the corresponding pixel DN count in the FOC science data file that is to be corrected. UNITAB TYPE=C*18 INSTRUMENT=FOC FILETYPE=SCI table of relative detective efficiency filenames: UTC0 TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=MJD Coordinated Universal Time (Modified Julian Date): This value is as input from the ground, it is updated only after spacecraft safings and/or when the difference in spacecraft time from a POCC time `obtained from White Sands' is > 10msec. (ETS-a) (UTC02 * 2**32 + UTC01) give the decimal value of the VAX 64 bit time format which, when translated, gives the reference UTC0 in MJD of the spacecraft clock. i.e. UTC when the spacecraft clock read SPLINCN ticks. (ETS-c) UTCO1 TYPE=I*4 INSTRUMENT=ALL FILETYPE=SHP bytes 5-8 of UTC0: UTCO2 TYPE=I*4 INSTRUMENT=ALL FILETYPE=SHP bytes 1-4 of UTC0: Decimal representation of bits 1-4, using a place value for each bit as if they were bits 5-8. i.e, the given value is really UTC02 / 2**32. (ETS-d) V2APERCE TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSEC the X component of the aperture offset position in the st coordinate system. The v2 offset of the target from the aperture center. [qobservation.v2v3_xcoord] V3APERCE TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSEC V3 offset of target from aper. center (arcsec): the Y component of the aperture offset position in the st coordinate system. The v3 offset of the target from the aperture center. [qobservation.v2v3_ycoord] VAC_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI vacuum to air correction: Apply vacuum-to-air correction to the wavelengths. This routine converts vacuum wavelengths to air wavelengths above 2000 Angstroms. (calguide) VDATAFMT TYPE=C*4 INSTRUMENT=HSP FILETYPE=UDL Format of current observation: 1: byte, 2: word, 3: longword, 4: analog 7: all VELABBRA TYPE=R*4 INSTRUMENT=ALL FILETYPE=SHP UNITS=ARCSEC aberration in position of the target: magnitude of aberration due to st and earth velocities. This is the absolute angular correction that must be applied to the apparent position of the target as seen from the st to compensate for the velocity of the st and the earth. [qobservation.velabbra] VELOCSTX TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM/SEC velocity of space telescope along the x axis (km/sec): X component of the velocity of space telescope in geocentric J2000,0 inertial coordinates. This is a orthogonal right handed coordinate system centered in the earth, with the X axis pointing towards the vernal equinox for the year 2000, the Z axis pointing towards the north celestial pole for the year 2000, and the Y axis orthogonal to both. [qobservation.velocstx] VELOCSTY TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM/SEC velocity of space telescope along the y axis (km/sec): Y component of the velocity of space telescope in geocentric J2000,0 inertial coordinates. This is a orthogonal right handed coordinate system centered in the earth, with the X axis pointing towards the vernal equinox for the year 2000, the Z axis pointing towards the north celestial pole for the year 2000, and the Y axis orthogonal to both. [qobservation.velocsty] VELOCSTZ TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM/SEC velocity of space telescope along the z axis (km/sec): Z component of the velocity of space telescope in geocentric J2000,0 inertial coordinates. This is a orthogonal right handed coordinate system centered in the earth, with the X axis pointing towards the vernal equinox for the year 2000, the Z axis pointing towards the north celestial pole for the year 2000, and the Y axis orthogonal to both. [qobservation.velocstz] VFAPVECX TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Vector pointing from the desired position of the candidate to the home position of the image. The vector is set by the user with a default of 0. It can be used to point from a small observing aperture to the center of the finding aperture image. (norton.51) VFAPVECY TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Vector pointing from the desired position of the candidate to the home position of the image. The vector is set by the user with a default of 0. It can be used to point from a small observing aperture to the center of the finding aperture image. (norton.51) VFCENVEX TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Vector from the coarse target to the target centroid. The vector points from the coarse target to the centroid of the target's individual measurements. (norton.52) VFCENVEY TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Vector from the coarse target to the target centroid. The vector points from the coarse target to the centroid of the target's individual measurements. (norton.52) VFCTVECX TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Vector from the center of the finder image to the coarse target. The vector points from the center of the finding aperture image to the row and column representing the candidate. (norton.51) VFCTVECY TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Vector from the center of the finder image to the coarse target. The vector points from the center of the finding aperture image to the row and column representing the candidate. (norton.51) VFFTVECX TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Vector from the center of the finder image to the target centroid. This is the fine target vector, representing the sum of VFCENVE and VFCTVEC. (norton.52) VFFTVECY TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Vector from the center of the finder image to the target centroid. This is the fine target vector, representing the sum of VFCENVE and VFCTVEC. (norton.52) VFOBJCNT TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL count of trg obj: Gives the total number (in the range between VFLOFLIM and VFHIFLIM) of Target Acquisition and Verification objects found. Only the brightest 20 are saved, although this count could exceed that number. (norton.50) VFOCUS TYPE=R*4 INSTRUMENT=HSP FILETYPE=SHP focus of the object detector: VFOCUSn TYPE=R*4 INSTRUMENT=HSP FILETYPE=SHP focus n: n=1..4 VFOCUSD TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL focus command value for object detector: Equivalent to VFOCUSDn for when the object detector=n. (cgpulk) VFOCUSDn TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL focus command value for detector n: n=1..4 Sets the 12bit DAC which determines the initial focus for the image dissector tube deflection current. (norton.36) VFPFACTX TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Target Acquisition and Verification vector conversion factors. These constants define the conversion between the TAV image scale and the scale of the image projected by the Space Telescope on the face of the detector. (norton.47) VFPFACTY TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Target Acquisition and Verification vector conversion factors. These constants define the conversion between the TAV image scale and the scale of the image projected by the Space Telescope on the face of the detector. (norton.47) VFSLWVEX TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL X component of the slew vector for Target Acquisition and Verification. This is the vector issued as a slew request. It represents the vector sum of VFFTVEC and VFAPVEC, and points from the desired observing aperture to the centroid of the target's inidivual measurements. (norton.52) VFSLWVEY TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Y component of the slew vector for Target Acquisition and Verification. This is the vector issued as a slew request. It represents the vector sum of VFFTVEC and VFAPVEC, and points from the desired observing aperture to the centroid of the target's inidivual measurements. (norton.52) VFTAVERR TYPE=R*4 INSTRUMENT=HSP FILETYPE=SHP TAV (Target Acquisition and Verification) error status: VGAIND TYPE=I*2 INSTRUMENT=HSP FILETYPE=SCI gain setting: Gain setting of the object or sky depending on data source. (cgpsdh) VGAINDn TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL gain setting of detector n: n=1..5 Sets the value of the full-scale gain of the CVC (Current to Voltage Converter) Full scale values allowed are: 0: 1 nanoamp; 2: 10 nanoamps; 3: 100 nanoamps; 6: 1 microamp; 7: 10 microamps; (norton.36) VGAINDS TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL gain setting of detector "sky": See VGAINDn. VHDEFLn TYPE=R*4 INSTRUMENT=HSP FILETYPE=SHP horizontal deflection n: n=1..4 VHORIZ TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL horizontal deflection (command value) of the object detector: Equivalent to VHORIZn for when the object detector=n. (cgpulk) VHORIZn TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Horizontal deflection for detector n: n=1..4 Sets the 12bit DAC which determines the initial horizontal image dissector tube deflection current. (norton.35) VHORSTPT TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL no. of horiz steps/spatial point in area scans: Deflection steps correspond to about 4.42 microns on the face of the image dissector tube. If the incrementing process (starting with the initial deflection) causes the deflection value to exceed the 12-bit capacity (4096), the counter wraps and starts over at zero. (Norton.33) VHPOINTS TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL no. of horiz points (columns) in area scans: VIGHFILE TYPE=C*18 INSTRUMENT=HRS FILETYPE=SCI UNITS=FILENAME Vignetting Files (VIG): The removal of vignetting and wavelength-dependent photocathode variations is done using data from the vignetting files. Vignetting correction files contain multiple groups of responses. Each group contains the responses for a particular carrousel position and line position. Within the group, responses are ordered by equally spaced sample positions determined by the keywords, SAMPBEG and SAMPOFF. Data in the vignetting correction data files are stored in REAL*4 format. VIG_CORR TYPE=C*8 INSTRUMENT=HRS FILETYPE=SCI removal of vignetting nonuniformity: Remove vignetting and wavelength-dependent photocathode variations by dividing each count value by the vignetting response contained in the vighfile file. This routine removes the vignetting and low frequency photcathode response using a reference file that has a vignetting map. This map is has a vignetting vector for multiple line position and carrousel positions. At each line position the granularity is tabulated with a constant starting sample for all lines and a constant delta sample. To compute the response for the data's line and sample, tri-linear interpolation is used within the reference file over carrousel position, line position and sample position. If Doppler compensation is specified, the response is smoothed by a weighting function describing the motion of the data samples along the photocathode. (calguide) VNOINTPT TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL no. of integrations/pt in area scans: Number of integrations to be done at each of the points in an area scan. the default value for this parameter after initialization is 1. (norton.33) VOFFn TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI vertical offset bin n+1: n=1..6 VREQDET TYPE=C*8 INSTRUMENT=HSP FILETYPE=UDL requested detector for the object observation: 1: IDT1 (Image Dissector Tube 1) 2: IDT2 (Image Dissector Tube 2) 3: IDT3 (Image Dissector Tube 3) 4: IDT4 (Image Dissector Tube 4) 5: PMT (Photomultiplier) VSKYDET TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL currently selected sky detector: 1: IDT1 (Image Dissector Tube 1) 2: IDT2 (Image Dissector Tube 2) 3: IDT3 (Image Dissector Tube 3) 4: IDT4 (Image Dissector Tube 4) 5: PMT (Photomultiplier) VVERSTPT TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL no. of vert. steps/spatial pt. in area scans: Deflection steps correspond to about 4.42 microns on the face of the image dissector tube. If the incrementing process (starting with the initial deflection) causes the deflection value to exceed the 12-bit capacity (4096), the counter wraps and starts over at zero. (Norton.33) VVERT TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL vertical deflection (command value) of the object detector: Equivalent to VVERTn for when the object detector=n. (cgpulk) VVERTn TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL Vertical deflection for detector n: n=1..4 Sets the 12bit DAC which determines the initial vertical image dissector tube deflection current. (norton.35) VVPOINTS TYPE=I*4 INSTRUMENT=HSP FILETYPE=UDL no. of vertical points (rows) in area scans: VXMOON TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM/SEC Moon velocity: geocentric J2000 frame: VXSUN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM/SEC Sun velocity: geocentric J2000 frame: VYMOON TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM/SEC Moon velocity: geocentric J2000 frame: VYSUN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM/SEC Sun velocity: geocentric J2000 frame: VZMOON TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM/SEC Moon velocity: geocentric J2000 frame: VZSUN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM/SEC Sun velocity: geocentric J2000 frame: WAVCORR TYPE=C*8 INSTRUMENT=FOC FILETYPE=SCI compute photometric parameters: Compute the absolute sensitivity. This does not affect the data values. The inverse sensitivity, pivot wavelength, and RMS bandwidth are computed and stored in the header of the output image. The zero-point magnitude and the observation mode are also saved in the output header. See keywords PHOTMODE, PHOTFLAM, PHOTZPT, PHOTPLAM, PHOTBW. (calguide) WAV_CORR TYPE=C*8 INSTRUMENT=FOS FILETYPE=SCI wavelength scale generation: Compute a vacuum wavelength scale for each object or sky spectrum. Wavelengths are computed using coefficients stored in table ccs6. This is computed differently for the gratings and for the prism. This step is a spectroscopy mode calibration step. (calguide) WBLDASNR TYPE=I*4 INSTRUMENT=WFP FILETYPE=SHP Blade A sensor: 0:closed, 1:open: WBLDBSNR TYPE=I*4 INSTRUMENT=WFP FILETYPE=SHP Blade B sensor: 0:closed, 1:open: WCANLTIM TYPE=R*4 INSTRUMENT=WFP FILETYPE=SHP time of cancel operation command: To obtain control of the exposure, a Cancel Operation Command is issued to the instrument a minimum of 16.525 seconds after the initiating major frame pulse. The spacecraft time (in the same format as for WEXPOTIM) is stored in WCANLTIM. (norton.22) WEXPOCMD TYPE=I*4 INSTRUMENT=WFP FILETYPE=SHP expose command image: WEXPODUR TYPE=I*4 INSTRUMENT=WFP FILETYPE=SCI UNITS=SECONDS Commanded duration of exposure (seconds): WEXPOTIM TYPE=I*4 INSTRUMENT=WFP FILETYPE=SCI Major frame pulse time preceding exposure start (cnts): Decimal representation of the 16 low order bits (lsb) of the time tag given by the spacecraft to the major frame pulse (mfp) preceding the start of a WFPC exposure. (ETS-c) WEXPTMHI TYPE=I*4 INSTRUMENT=WFP FILETYPE=SHP major frame pulse time preceding exp start (cnts): Decimal representation of the 16 high order bits (Msb) of the time tag given by the spacecraft to the major frame pulse (mfp) preceding the start of a WFPC exposure. (but using a place value for each bit as if they were lsb!. i.e, the given value is really WEXPTMHI/2**16) Spacecraft clock at mfp = (WEXPTMHI*2**16 + WEXPOTIM) (ETS-c) WFCSTAT TYPE=I*4 INSTRUMENT=WFP FILETYPE=SHP control/status word for exposure: 0 if nominal WFPC microprocessor control of the shutters. 1 if NSCC-1 controlled the shutters. (generally meaning an interrupted exposure.) (ETS-c) WFOCTMnn TYPE=I*4 INSTRUMENT=WFP FILETYPE=SHP time of nnth open or close of B shutter: nn=1..15 Telemetered values to determine the actual exposure time nn=odd: Time of shutter closing; nn=even: Time of shutter opening. WORDS TYPE=I*2 INSTRUMENT=HSP FILETYPE=IMG number of HSP words samples in a line: WRD11_14 TYPE=I*2 INSTRUMENT=ALL FILETYPE=SHP word 11/14 ... A number assigned by sms for each observation. the word 11/14 is a count which is kept for each instrument and updated for each observation using the instrument. The count rolls over every 255. [qobservation.word_11_14] WSCALE TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI Scale factor for output image: WTIMEXPO TYPE=R*4 INSTRUMENT=WFP FILETYPE=SHP time of 110 msec expose command: As its last action at the end of an exposure, the WFSHCON command is executed. That command generates a 110 msec Executable Exposure Command to reset the WF/PC microprocessor's shutter control logic, as well as to initiate the CCD readout. The spacecraft time of this command is recorded in WTIMEXPO. (norton.22) WWCANCM TYPE=I*4 INSTRUMENT=WFP FILETYPE=SHP cancel operation command bit: To obtain control of the exposure, a Cancel Operation Command is issued to the instrument a minimum of 16.525 seconds after the initiating major frame pulse. The spacecraft time (in the same format as for WEXPOTIM) is stored in WCANLTIM and the bit WWCANCM is set. (norton.22) WWLOGOF TYPE=I*4 INSTRUMENT=WFP FILETYPE=SHP log overflow bit: The spacecraft times for the WFPC shutter opens and closes are recorded in the telemetered fields WFOCTMnn. However, only the first 8 'close' commands ( and 7 additional 'open' commands) can be accomodated in the SHP. If more activity occurs, the subsequent times are not recorded, but the WWLOGOF flag is set to indicate that the log overflowed. (norton.22) WWSCAP TYPE=I*4 INSTRUMENT=WFP FILETYPE=SHP shutter control application processor bit: This bit is set if, as its last action at the end of an exposure, the WFSHCON command was executed. That command generates a 110 msec Executable Exposure Command to reset the WF/PC microprocessor's shutter control logic, as well as to initiate the CCD readout. (norton.22) WZERO TYPE=R*4 INSTRUMENT=WFP FILETYPE=SCI Zero point for output image: XBASE TYPE=R*4 INSTRUMENT=FOS FILETYPE=IMG X-deflection base: XDEF TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI horizontal deflection: XEXPTMnn TYPE=I*4 INSTRUMENT=FOC FILETYPE=UDL exposure start or stop time nn (sc clock counts): nn=1..42 Telemetered values to determine the actual exposure time nn=odd: Exposure start or restart time nn=even: Exposure stop time. XMOON TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM Moon position: geocentric J2000 frame: XPITCH TYPE=I*4 INSTRUMENT=FOS FILETYPE=SCI X-deflection pitch between diode: XSUN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM Sun position: geocentric J2000 frame: X_OFFSET TYPE=R*4 INSTRUMENT=FOS FILETYPE=SCI x_offset for GIMP correction (diodes): Y1STCHNL TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL first channel to be processed: YAQMD TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL acquisition mode: YBASE TYPE=R*4 INSTRUMENT=FOS FILETYPE=IMG y base: YDATALIM TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL high byte of acquisition limit: YDEAD TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL accum close time: The accumulator "close time" (interval during which the accumulator counting is disabled) is specified in units of 7.8125 microsecs. (norton.35) YDEF TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI vertical deflection: YINTEG TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL number of integrations/X-step: The number of integrations controls the number of open/close time pairs of FOS Analog Signal Processor samples of the output from the rate limiter that are done with no changes in magnetic deflection. (norton.34) YLINSFRM TYPE=I*4 INSTRUMENT=FOS FILETYPE=SCI packets per frame: YLIVE TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL accum open time: The accumulator "open time" (interval during which the accumulator counting is enabled) is specified in units of 7.8125 microsecs. (norton.34) YMCLEARS TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL memory clears/data acquisition: YMOON TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM Moon position: geocentric J2000 frame: YMSLICES TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL number of memory slices: YNOISELM TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL burst noise rejection limit: YNUMCHNL TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL number of channels to be processed: YOVRSCAN TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL X-deflection overscan: YPITCH TYPE=I*4 INSTRUMENT=FOS FILETYPE=IMG Y-deflection pitch between diodes: YPOS TYPE=R*4 INSTRUMENT=FOS FILETYPE=SCI y-position on photocathode: YPTRNS TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL patterns per readout: YRANGE TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL Y range: YREADCYC TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL readouts/memory clear: YSPACE TYPE=R*4 INSTRUMENT=FOS FILETYPE=IMG yrange * 32 / ysteps: YSTEP1 TYPE=C*3 INSTRUMENT=FOS FILETYPE=IMG first ystep data type: OBJ, SKY, BCK, NUL: YSTEP2 TYPE=C*3 INSTRUMENT=FOS FILETYPE=IMG second ystep data type: OBJ, SKY, BCK, NUL: YSTEP3 TYPE=C*3 INSTRUMENT=FOS FILETYPE=IMG third ystep data type: OBJ, SKY, BCK, NUL: YSTEPS TYPE=I*4 INSTRUMENT=FOS FILETYPE=SCI number of y steps: YSUN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM Sun position: geocentric J2000 frame: YTYPE TYPE=CHR INSTRUMENT=FOS FILETYPE=IMG observation type: OBJ, SKY, BCK: YWRDSLIN TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL words per line: YXBASE TYPE=R*4 INSTRUMENT=FOS FILETYPE=UDL X-deflection base: YXPITCH TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL X-deflection pitch between diode: YXSTEPS TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL X-deflection sub-steps: YXYDFTMP TYPE=R*4 INSTRUMENT=FOS FILETYPE=SHP XY-deflection focus: YYBASE TYPE=R*4 INSTRUMENT=FOS FILETYPE=UDL Y-deflection base: YYPATH TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL path identification: YYPITCH TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL Y-deflection pitch: YYSTEPS TYPE=I*4 INSTRUMENT=FOS FILETYPE=UDL Y-deflection sub-steps: Y_OFFSET TYPE=R*4 INSTRUMENT=FOS FILETYPE=IMG y_offset for GIMP correction (diodes): ZACMODE1 TYPE=C*8 INSTRUMENT=HRS FILETYPE=SHP acquisition mode: 0: spectral science data 1: focus diode field map 3: single frame (SO-01p3-424) ZDOPMAG TYPE=I*4 INSTRUMENT=HRS FILETYPE=UDL OCT (Observation Control Table) doppler shift correction magnitude: See DOPMAG ZFLUXM TYPE=I*4 INSTRUMENT=HRS FILETYPE=UDL flux measurement at end of targ. acq. obs.: The flux measurement, taken through whichever aperture (large or small), contains the target at the very end of a target acquisition observation. As the last (and always executable) phase of a target acquisition observation, one more frame of data is obtained from the instrument. The flux measurement is the sum of the counts of the 8 target acquisition diodes. SO-01p3-262. ZFSPYBF TYPE=I*4 INSTRUMENT=HRS FILETYPE=UDL control bits for spectrum y-balance: 1: Spectrum y balance offset should be used 2: Spectrum y balance offset should be computed ZFXMAPC TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI x deflection of the center of field map: ZFYMAPC TYPE=I*4 INSTRUMENT=HRS FILETYPE=SCI y deflection of the center of field map: ZINTPER TYPE=I*4 INSTRUMENT=HRS FILETYPE=UDL OCT (Observation Control Table) integration period (number of 50 ms slices): Number of 50ms blocks accumulated internally to produce 1 line of science data (1-255). SE-01p3-266. ZLCOEF1 TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI line mapping function L0: ZLCOEF2 TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI line mapping function A: ZMOON TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM Moon position: geocentric J2000 frame: ZSCOEF1 TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI first coefficient of sample mapping: ZSCOEF2 TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI second coefficient of sample mapping: ZSCOEF3 TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI third coefficient of sample mapping: ZSCOEF4 TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI fourth coefficient of sample mapping: ZSPYBALU TYPE=R*4 INSTRUMENT=HRS FILETYPE=UDL spectrum y-balance offset: ZSPYBLU TYPE=R*8 INSTRUMENT=HRS FILETYPE=SCI spectrum y-balance offset: ZSRCHLCE TYPE=I*4 INSTRUMENT=HRS FILETYPE=UDL OCT (Observation Control Table) y increment for field map: ZSRCHLCF TYPE=I*4 INSTRUMENT=HRS FILETYPE=UDL OCT (Observation Control Table) x increment for field map: ZSUN TYPE=R*8 INSTRUMENT=ALL FILETYPE=SHP UNITS=KM Sun position: geocentric J2000 frame: ZTREFH TYPE=I*4 INSTRUMENT=HRS FILETYPE=UDL OCT (Observation Control Table) time of zero doppler correction: Doppler shift 0 phase time (the time of zero doppler correction) Higher order bits in spacecraft clock units (125ms since Jan 1,1979) SE-01p3-266 ZXDCALP TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI proportional x-deflection cal correction: ZXDCALU TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI x comp null deflection cal correction: ZYDCALP TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI proportional y-deflection cal correction: ZYDCALU TYPE=R*4 INSTRUMENT=HRS FILETYPE=SCI y comp null deflection cal correction: -------------------------------------------------------------------------- Sources: ETS: Ed T. Smith ETS-a: Phone converstations with Jeff Lawson and Ed Kimmer at POCC. ETS-b: Cutler comments in SOGS routine CGWCEX. ETS-c: WFPC SOGS Notebook ND-1002C, by Norton. ETS-d: My inspection of science headers keyword values. ETS-e: Conversation with CALFOS programmer, Steve Hulbert. ETS-f: My inspection of actual keyword names ETS-g: Phase II proposal instructions.