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STSDAS
STSDAS Version 3.15 Release Notes

STSDAS Version 3.15 Release Notes

June 2012

This release of STSDAS contains changes to the pipeline code for many
HST instruments; primarily, ACS, STIS, WFC3 and COS. 

The final software used by the ST-ECF to calibrate FOS data has been
included strictly as a record of the processing performed to generate
the FOS products available from the HST archive. 

The specific changes are detailed in the following sections.


HSTCAL and Future STSDAS Releases
=================================
The code for CALACS has been removed entirely from STSDAS as it has
been replaced by the HSTCAL version.  Any user loading the acs package
under STSDAS will be directed to the HSTCAL version which now has
a Python-based TEAL interface as well as the standard command-line
executable interface. 

The STSDAS versions of CALWF3 and CALSTIS will also be removed in
future releases as they get replaced by HSTCAL versions of the code.


Platform Support
================
Binaries for this release were built on Red Hat Enterprise Linux 4
and Mac OS X 10.5.  Binaries were built with IRAF 2.14.  Binaries
for newer versions of IRAF or operating systems may be built as
needed, and users can check the STSDAS web pages for more 
details.
  
IRAF is available separately from http://iraf.net.

No Solaris Support
------------------
This release has NOT been tested on the Solaris platform.  We no longer
build Solaris binaries for STSDAS, although the source code can always
be downloaded and compiled locally as needed.


64-bit IRAF Support
--------------------
IRAF 2.15 includes support for 64-bit systems. The changes necessary to
support 64-bits generally require applications to be modified. We will
only release 32-bit binaries of the Tables and STSDAS packages for use
with IRAF 2.15. Support for 32-bit binaries will continue as long as
there are sufficient platforms that such binaries will run on. We may
only convert some packages in Tables and STSDAS to 64-bit version when
the 32-bit versions are no longer viable and if created will be released
as a separate package with a different name. When the 32-bit versions
of TABLES and STSDAS are no longer viable, support for any tasks within
those packages not ported to 64-bits will end.  The full description of
this policy can be found online at:

http://www.stsci.edu/resources/software_hardware/stsdas/iraf64


STECF Software
==============
This release contains the latest version of the stecf IRAF package for
supporting HST data that had been developed by members of the Space
Telescope European Coordinating Facility (ST-ECF) which closed on 31
December 2010.

The packages included in stecf are:

imres - Tasks used for photometric image restoration with unconstrained star
        positions, simulating images with ground-based seeing and making
        apodizing mask images.

impol - A package for imaging linear polarization mapping for data taken
        using the polarimetry modes of HST instruments.  An overview and 
        access to demos and help files is available at:
                http://www.eso.org/~jwalsh/softpol/

specres - A package for point source extraction and background decomposition
          of 2-D (longslit) spectra. An oThe wf3rej task was upgraded to read and save the BUNIT keyword value from the
[sci,1] extension of each input image and to then check those values each time
input sci data arrays are loaded in the various subroutines. If the input data
are in units of rates (either DN/sec or electrons/sec), the data are
immediately scaled up by the exposure time of the particular image to turn them
back into units of counts, which is the expected working units within wf3rej.verview is provided at:
                http://www.eso.org/~jwalsh/specres/

Support for these packages may be obtained by contacting the STScI Help
Desk at 'help@stsci.edu'. These questions will then be forwarded to the
package authors at ESO as required.

HST_CALIB
==========

calstis
-------
These are the major changes from calstis 2.36 to 2.40.

The values in the FLUX and ERROR columns for echelle data will be set to
zero if the spectral order does not have flux calibration information in
the PHOTTAB.  A new NET_ERROR column has been added to the x1d table to
give the error estimate for the net count rate.

The buffer size for an individual file name has been increased to 1024
characters.  The length of a string of input or output file names for
calstis, basic2d, or ocrreject is limited by the operating system.

Calstis now recognizes the command-line option -r, which will print the
full version string and exit with a status of 0.  There is also a --version
option that prints just the version number.

calwf3
------
These are the major changes for calwf3  from v 2.4.1 to  v2.7

The calwf3 IR ramp fitting routine (cridcalc step) adds up the total integration 
time of all unrejected samples for each pixel and stores that value in the output 
FLT file TIME extension. In some unusual circumstances involving the rejection of 
either the 1st or 2nd sample as bad or containing a CR hit, the total integration 
time was not coming out correctly, due to either a single valid sample in the 1st 
read or the valid part of the ramp starting in the 2nd read. The error was such 
that the reported total time is an overestimate, because the time associated with 
the rejected samples is not being removed properly. The fitsamps routine in cridcalc
was modified to correctly initialize the total integration time counter with the 
sample time of the first unrejected sample.

When calwf3 was executed for an association that contained repeat-obs (RPT) members 
it ignored the setting of the RPTCORR calibration switch in the image headers and 
always applies RPTCORR processing, which consists of calling the wf3rej task to 
combine the images. This made it impossible to control the application of RPTCORR 
processing via the OPUS keyword rules that set the RPTCORR switch. The high-level 
logic of calwf3 association processing was modified so that it only applies 
the wf3rej step when RPTCORR=PERFORM in the image headers. In association with this,
the calwf3 routines that build the association-level trailer file have been modified 
so that when a sub-product has not been created (i.e. wf3rej is not run) they use the 
trailer files of the individual association members, instead of trying to use the 
trailer file(s) of the crj sub-product.

The wf3rej task was upgraded to read and save the BUNIT keyword value from the
[sci,1] extension of each input image and to then check those values each time
input sci data arrays are loaded in the various subroutines. If the input data
are in units of rates (either DN/sec or electrons/sec), the data are
immediately scaled up by the exposure time of the particular image to turn them
back into units of counts, which is the expected working units within wf3rej.

Negative cosmic rays are now accounted for in IR WFC3 images during cosmic ray rejection.

The zero-read pixel value is now used for ramp-fitting when the pixel is already saturated
in the zeroth read of the ramp. The behavior has been modified such that pixel which are 
saturated in the zeroth read or in the first read are handled the same way. 
In both cases the output value is set to the value in the zeroth read. In the case 
where the zeroth read value is already saturated, a dq=256 flag will be added to the 
DQ array of the flt file. In the case where saturation does not occur until the 
first read, no saturation flag will be added to the flt DQ array. This eliminates blank pixels
in the output FLT image.

The IR cridcalc handling of pixels detected to contain spikes was modified so that
pixels flagged as bad from the static DQ mask still go through the process of CR
detection, in order to produce cleaner output FLT images.


new option added "-r" to calwf3 to print the current verison and exit 

aXe - stsdas.analysis.slitless
------------------------------

The test of the width parameter in the OAF file was updated to specify that it's the half-width
and not the width. Similarly, the AWIDTH1A BWIFTH1A and AORIENT1A are copied of the Sextractor parameters 
A_IMAGE, B_IMAGE and THETA_IMAGE. They therefore refer to the semi major axis, semi minor 
axis and orientation to the semi major axis wrt to the horizontal.



synphot
-------
Updated the synphot calcband and calcspec help files to contain more
useful information on how to use the thru() function to read ASCII
passband files.