CCD Flatfield Correction by Differential Stellar Photometry: Automated Methods

Details CCD Flatfield Correction by Differential Stellar Photometry: Automated Methods CCD Flatfield Correction by Differential Stellar Photometry: Automated Methods

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...203.0402b&link_type=abstract

American Astronomical Society Meeting 203, #04.02; Bulletin of the American Astronomical Society, Vol. 35, p.1207

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Calibrating CCD stellar fields to derive precise, one percent, photometry requires corresponding validity in the assumption of unit input sent through the telescope optical system for making the initial flat. Twilight or nighttime sky or even dome light might make the initial flat. Scattered light can compromise the applicability of the flat for quality photometry. Test exposures on a rich star field can provide data to reveal the error of the flat, and also may be used to correct the initial flat. We have developed automated methods for tuning the initial flat so as to confidently apply the corrected flat to other stellar fields having just single exposures in an observing run.

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