Image reduction pipeline for the detection of variable sources in highly crowded fields

Details Image reduction pipeline for the detection of variable sources in highly crowded fields Image reduction pipeline for the detection of variable sources in highly crowded fields

2001-10-31

arxiv.org/abs/astro-ph/0110704v1

Astron.Astrophys. 381 (2002) 1095-1109

Astronomy and Astrophysics

Astrophysics

15 pages, 4 figures, accepted by A&A

Scientific paper

10.1051/0004-6361:20011522

We present a reduction pipeline for CCD (charge-coupled device) images which was built to search for variable sources in highly crowded fields like the M31 bulge and to handle extensive databases due to large time series. We describe all steps of the standard reduction in detail with emphasis on the realisation of per pixel error propagation: Bias correction, treatment of bad pixels, flatfielding, and filtering of cosmic rays. The problems of conservation of PSF (point spread function) and error propagation in our image alignment procedure as well as the detection algorithm for variable sources are discussed: We build difference images via image convolution with a technique called OIS (Alard & Lupton, 1998), proceed with an automatic detection of variable sources in noise dominated images and finally apply a PSF-fitting, relative photometry to the sources found. For the WeCAPP project (Riffeser et al., 2001) we achieve 3 sigma detections for variable sources with an apparent brightness of e.g. m = 24.9 mag at their minimum and a variation of dm = 2.4 mag (or m = 21.9 mag brightness minimum and a variation of dm = 0.6 mag) on a background signal of 18.1 mag/arcsec^2 based on a 500 s exposure with 1.5 arcsec seeing at a 1.2 m telescope. The complete per pixel error propagation allows us to give accurate errors for each measurement.

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