Abstract
Not all pixels on a CCD chip are created equal. To make accurate photometric measurements, the differences in sensitivity and average noise must be taken into account. This is done through the use of master flat fields, dark frames, and bias frames. This chapter describes each type of master and how to create them.
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References
R. Berry, J. Burnell, The Handbook of Astronomical Image Processing (Willmann-Bell, Richmond, 2000)
R. Crisp, Residual bulk image: Cause and cure. Sky Telescope 121(5), 72–75 (2011)
S. Howell, Handbook of CCD Astronomy (Cambridge University Press, New York, 2000)
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Warner, B.D. (2016). Mastering the Masters. In: A Practical Guide to Lightcurve Photometry and Analysis. The Patrick Moore Practical Astronomy Series. Springer, Cham. https://doi.org/10.1007/978-3-319-32750-1_9
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DOI: https://doi.org/10.1007/978-3-319-32750-1_9
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