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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.