WFC3 UVIS and IR Flat Fields

Details WFC3 UVIS and IR Flat Fields WFC3 UVIS and IR Flat Fields

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21725439p&link_type=abstract

American Astronomical Society, AAS Meeting #217, #254.39; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

The WFC3 flat field program for both the UVIS and IR channels consists of ground flats, LP flats, sky flats and earth flats. Creation of the WFC3 LP flats starts with the ground flats (pixel-to-pixel variation) and are combined with on-orbit observations of stellar fields (low frequency modulation). The ground flat field accuracy is +/-3% peak-to-peak for the IR and 1.5 to 4.5% in the UVIS. Assessment of the flats is done by identifying the peak-to-peak and RMS variations. As we continue to refine these flats and test them for inclusion in CDBS and the WFC3 pipeline we are in parallel executing both a sky flats and an earth flats program to use as secondary confirmation of the flat field program. In addition, internal flats are used to monitor flat field stability.

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