sukye

jref

acs data handbook p154
———————————
In the Unix environment, we must specify the location of the ‘jref’
directory where the calibration reference files reside and then start
IRAF. We assume here that the user has requested calibration files as
part of the data archive request and stored these in their directory
‘/mydisk/myjref/’, where ‘/mydisk/’ specifies the directory containing
the pipeline data.

(Note: This setup must be done in the same window in which IRAF will be
used. Note also that setting ‘jref’ from within IRAF will not work even
though typing ‘show jref’ would suggest it might.)

unix> setenv jref /mydisk/myjref/
unix> cl
————————————————–
p182
The main calibration reference files required by MultiDrizzle are the
IDCTAB and DGEOFILE files discussed in Section 4.1.4. The IDCTAB
file describes the ACS distortion in terms of polynomial coefficients. The
appropriate reference file is recorded in the image header keyword
IDCTAB. This file should be obtained from the STScI archive (via
Starview) and placed in some local directory. Before starting MultiDrizzle
the environment variable “jref” must be set appropriately to point to this
directory (see Section 3.5 for more information). Once the FLT files have
been collected and the ‘jref’ environment established, PyRAF should be
started and the stsdas, analysis, and dither packages loaded.

————————————————–
Harry
The goods cluster does not have the jref directory installed.
What we typically do is identify the specific files needed by looking at the
FITS header keywords, and then we copy them individually over to the
goods cluster using
scp tib:/data/cdbs7/jref/filename.fits

I usually put them in /data/raid1/acs_archive/reffiles and then

setenv jref /data/raid1/acs_archive/reffiles/ (the last / is important),
before getting into iraf or pyraf.
————————————————–

Massimo
put Best Reference Files in /jref and set jref=/…/jref

works!

http://archive.stsci.edu/hst/search.php
sukye: Calibrated Science Files (usu only flt.fits are useful) could be
put in another file where multidrizzle is started.
–>epar mul

————————————————–

pyraf

http://www.stsci.edu/resources/software_hardware/pyraf

1. download
http://www.stsci.edu/resources/software_hardware/pyraf/stsci_python/current/download
yes, i need to have 7 additional softwares…

2. why pyraf
to replace iraf cl (no error or exception handling).
By developing a Python interface to IRAF tasks, we open up the IRAF system and make it possible to write scripts that combine IRAF tasks with the numerous other capabilities of Python.

3. python
http://www.python.org/
http://www.python.org/doc/tut/
http://www.woodpecker.org.cn:9081/doc/abyteofpython_cn/chinese/index.html

a. working in windows dos
set path=%path%;C:\python25
python

This week

0.
i,z images: done
acs wfc image F850LP
http://www.stsci.edu/hst/observatory/cdbs/SIfileInfo/ACS/WFCFlatImage?no_wrap=true
http://archive.stsci.edu/pointings/search.php
(i-z)_iso vs z_auto: done

1.
Keck, N (Bahram)
Gemini, N, S
http://www.gemini.edu/sciops/ObsProcess/ObsProcIntro.html
2007B Semester, 1 August 2007 - 31 January 2008, deadline is MONDAY APRIL 2nd, 2007
2007A semester, 1 February - 31 July 2007, deadline is around 30 September,2007
both North and South

VLT, S
http://www.eso.org/sci/observing/proposals/index.html
The next deadline (for Period 80, 1 October 2007 - 1 April 2008) is: 30 March 2007
You cannot submit proposals now.Please wait for the next announcement of observing time
which will be released at the beginning of September 2007.
Period 79 - current - (1 April 2007 - 30 September 2007)
Period 78 (1 October 2006 - 31 March 2007)

CDFs
HDFN

sept or apr?

2.
fan, sdss, how to discriminate stars frm qsos?
dwarfs and quasars…

3.
hst, data handbook acs section
http://www.stsci.edu/hst/HST_overview/documents/datahandbook
p13 wide field channel (WFC): 202*202 arcsec. 3700~11000 A
high resolution channel (HRC): 29*25. 2000~11000
solar blind channel (SBC): 35*31. 1150~1700.
p16 While there is no mechanical reason why the coronagraph could not be
used with the SBC, for health and safety reasons (due to brightness limits
of the MAMA detector) use of the coronagraph is forbidden with the SBC.
The ACS detectors exhibit significantly more distortion than previous
HST instruments. All ACS observations must be corrected for distortion
before any photometry or astrometry is derived.
p25 ACS WFC data come from two CCD chips and are treated as separate
observations, with a SCI, DQ and ERR array for each chip, and with both
chips being stored in the same FITS file. The result is a FITS file with 6
data extensions plus a global header for a single WFC exposure.
MultiDrizzle removes the effects of the geometric distortion and
produces a drizzled (DRZ) product which has the multi-extension FITS file
shown in Figure 2.1

4.
multidrizzle
acs manual chap 4

5.
sextractor, bertin & arnouts
or idiot’s guide

6.
iraf/pyraf user’s guide

7.
Keck LRIS spectra of late-M, L and T dwarfs
http://www-int.stsci.edu/~inr/ultracool.html