Physics
Scientific paper
Jul 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010hstc.worke..52n&link_type=abstract
"2010 Space Telescope Science Institute Calibration Workshop - Hubble after SM4. Preparing JWST, held 21-23 July 2010 at Space T
Physics
Scientific paper
The Space Telescope Imaging Spectrograph (STIS) has two types of reference files that are related to flat-fielding. A low-order flat field (the so-called L-flat) consists of a map of the large scale (> 64 pixels) variations in the sensitivity across a detector and contains the wavelength-dependent, low spatial frequency information about the uniformity of the detector. A pixel-to-pixel flat field (the so-called P-flat) contains the high-frequency pixel-to-pixel variations and the small scale blemishes like dead and bright pixels, thinning differences, and dust motes. The main features of the P-flats are the high frequency odd-even pattern seen in the high-resolution multi-anode microchannel array exposures and the small scale blemishes from dead and bright pixels, dust motes, etc. seen in the charge-coupled device (CCD) images. The L-flats are not expected to change significantly as a function of time. We therefore concentrate on P-flats and describe the generation of new post Servicing Mission 4 (SM4) STIS P-flats. The programs for taking data and software used to generate P-flats are described briefly. Application and the effectiveness of the new P-flats are also discussed. New post-SM4 FUV P-flats do not show any structural changes, hence no new flats have been made available, while the analysis of post-SM4 NUV P-flats is underway. New post-SM4 P-flats for the STIS CCD were delivered in December 2009 for use in pipeline processing.
Ake Thomas B.
Lennon Daniel
Niemi Sami-Matias
Proffitt Charles R.
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