ACS
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MultiDrizzle was designed primarily for supporting pipeline
processing
of ACS data.
Supported modes:
It has been tested for all modes of ACS data, except:
Time-dependent distortion:
The time-dependent distortion (TDD) correction will automatically be
turned on for all ACS images. It can only be turned off through the use
of the TDDCORR
keyword in the primary header of the image which needs to be set to a
value
of "OMIT" in order to be turned off.
Units:
All output data from MultiDrizzle has the units of electrons/second.
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WFPC2
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Supported modes:
- Most WFPC2 observing modes have been tested and are
supported
by Multidrizzle, including area mode and subarray observations.
Full
support for WFPC2 is currently in development.
- Multidrizzle is able to accept GEIS and waivered FITS
format
files as input. However, these files are automatically converted to
multi
extension FITS format files. When file conversion occurs, an
association
file is created containing the names of the new files. The
association file will have the same rootname as the original input with
"MDZ_" prepended.
The output file name also has "MDZ_" prepended during the file
conversion
step (this won't occur in future versions).
- If IVM files are going to be provided as input, they must
be
formatted as multi-extension FITS files with a separate extension for
each
chip's IVM array. Each extension should also have 'EXTNAME' set
to
'IVM' as well.
Units:
All intermediate output products from MultiDrizzle have the units of electrons/sec. The units
for the final product can be selected by the user to be either counts/sec or electrons/sec through the
use of the 'proc_units'
parameter.
Processing Differences:
Sky Subtraction:
- Plate scale differences are taken into account during the
sky
subtraction step. The 'MDRIZSKY' header value for WFPC2 is taken to be
on
the WF3 plate scale.
Single Drizzle step:
- The single-drizzle step only uses the Static Mask for
weighting. As a result, the regions of each chip edge masked by
the WFPC2 pyramid do
not get removed. This goes into creating a median image where
those
regions are influenced by the noise of those vignetted edges, reducing
the
effectiveness of the cosmic-ray determination for those areas.
The
next version will allow the user to mask out the vignetted edges
through
the use of the 'bits' parameter if the corresponding '.c1h'
data-quality
image is present for each input WFPC2 science image.
Input file Updates
- MultiDrizzle updates the input images WCS keywords based on
the
distortion coefficients provided as input. In addition,
MultiDrizzle
also updates the input file DQ arrays with the pixels that it
identified
as cosmic-rays. WFPC2 GEIS images, though, get converted on input
to
multi-extension FITS files and ONLY those converted FITS files get
updated
by MultiDrizzle, not the original input GEIS images.
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STIS
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Supported modes:
- Support for STIS imaging is complete at this time.
STIS
spectroscopy is not yet supported.
- Multidrizzle allows for the use of multi-imset STIS _flt
files
as input. These files will be automatically split into separate
files
prior to processing by Multidrizzle. The files will be named "rootname_flt_extnX.fits" where X represents the original extension
number
of the input file.
Units:
All output products from MultiDrizzle have the units of electrons/sec.
Processing Differences:
Cosmic-ray flagging:
- Since MultiDrizzle
and calstis2 both assign the
value 8192 to cosmic rays in the DQI file of the input flt image, users
may
want to run Multidrizzle on basic2d-calibrated flt.fits files not
already
modified by calstis2 (or by
its equivalent, stsdas.hst_calib.stis.ocrreject
with crmask=yes).
Default Parameter
settings:
- MDRIZTAB (_mdz.fits)
reference files, which can be used to set parameter values, do not yet
exist
for STIS. Although the default values in MultiDrizzle were chosen with
ACS
in mind, they generally work well for STIS. Tests have shown that a
slightly
relaxed value of 'driz_cr_scale'
(1.5 0.7) preserves the peaks of well-centered stars while still
providing
good cosmic ray rejection.
PA_V3
- Until the PA_V3 keyword
is automatically included in the header of STIS science
exposures,
the spt files should be kept in the working directory for the initial
run.
Multidrizzle will then extract the keyword value from the spt files and
add
it to the primary science headers. The PA_V3
keyword should now be included for all STIS data retrieved from the HST
archive
as of June
2005.
Input file Updates
- MultiDrizzle updates the input images WCS keywords based on
the distortion coefficients provided as input. In addition,
MultiDrizzle also updates the input file DQ arrays with the pixels that
it identified
as cosmic-rays. Associated STIS images, though, get converted on
input
to multi-extension FITS files, one for each SCI extension named in the
ASN
file, and ONLY those converted FITS files get updated by MultiDrizzle,
not
the original input multi-extension file.
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NICMOS
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Supported modes:
- Support for NICMOS imaging is only preliminary at this
time.
Full support for NICMOS is under development.
- Multidrizzle only supports processing of NICMOS CAL files
and
ASN (*_asn.fits and *_asc.fits) tables.
Units:
All intermediate output products from MultiDrizzle have the units of electrons/sec. The units
for the final product can be selected by the user to be either counts/sec or electrons/sec
through the use of the 'proc_units'
parameter.
Processing Differences:
PA_V3
- Until the PA_V3 keyword is automatically included in the
header
of NICMOS science exposures, it should be read from the primary header
of
the spt files and added to the primary header of the science exposures
manually
before running Multidrizzle. The PA_V3
keyword should now be included for all NICMOS data retrieved from the
HST
archive as of June 2005.
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