Measuring the direct sky brightness on CCD images

Details Measuring the direct sky brightness on CCD images Measuring the direct sky brightness on CCD images

Feb 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasp..103..243p&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 103, Feb. 1991, p. 243-252.

Astronomy and Astrophysics

Astronomy

16

Astronomical Photometry, Charge Coupled Devices, Sky Brightness, Error Analysis, Seeing (Astronomy), Stellar Magnitude

Scientific paper

A new method of determining the background sky brightness for stellar photometric measurements with CCDs is described. By fitting and subtracting stellar profiles from a CCD image, one can measure the sky brightness directly at the position of each star after subtraction. These sky values can then be used for the next round of profile fitting and subtraction. The 'direct sky' brightness for a star is the convergent value of the sky after a few such iterations and is the most direct measurement of the line-of-sight contribution of the background to the observed magnitude of a star. Using this method, a decrease of the random photometric errors by more than a factor of two over standard methods is possible, with the most significant improvements for stars in very crowded regions and areas of strong and highly variable nebulosity.

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