[en] Thinned CCD detectors display fringing which arises from the interference of multiply reflected light in the layers of the CCD. If the layer construction - the thicknesses and refractive indexes of the layers - is known, then the observed fringing can be accurately modelled and used to correct imaging and spectroscopic data for its effects. In practice the specifications on the actual deposited layer thicknesses may not be known to sufficient accuracy to predict the fringe behaviour. Thus calibration data, in the form of monochromatic flat fields, is required and can be modelled using the technique outlined by Malamuth et al. 2003, which has been applied to ACS CCDs.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Walsh, J. R.; ESA, Space Telescope European Co-ordinating Facility, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
Kuntschner, H.; ESO, Alonso de Cordóva 3107, Vitacura, Santiago, Chile
Jehin, Emmanuel ; Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Astrophysique et traitement de l'image
Kaufer, A.; ESO, Alonso de Cordóva 3107, Vitacura, Santiago, Chile
O'Brien, K.; ESO, Alonso de Cordóva 3107, Vitacura, Santiago, Chile
Riquelme, M.; ESO, Alonso de Cordóva 3107, Vitacura, Santiago, Chile
Smette, A.
Kerber, Florian
Language :
English
Title :
Modelling the Fringing of the FORS2 CCD
Publication date :
2008
Event name :
The 2007 ESO Instrument Calibration Workshop
Event organizer :
Andreas Kaufer, Florian Kerber, R Hanuschik, F Patat, M Peron, M Romaniello, M Sterzik
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