Accurate physical model for direct modeling of point source transients for ISOCAM LW detector

Details Accurate physical model for direct modeling of point source transients for ISOCAM LW detector Accurate physical model for direct modeling of point source transients for ISOCAM LW detector

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003esasp.511..343f&link_type=abstract

Exploiting the ISO Data Archive. Infrared Astronomy in the Internet Age, held in Siguenza, Spain 24-27 June, 2002. Edited by

Astronomy and Astrophysics

Astronomy

Scientific paper

Under quasi uniform illumination, the transient response of individual pixel of Si:Ga LW ISOCAM detector is described with high accuracy by one of the Fouks' models, called as Fouks-Schubert model. But this model fails its accuracy if the gradient of illumination between adjacent pixels is high.
We present here a general 3D physical model which allows to describe with a high accuracy most of the cases we have with ISOCAM. Besides the case of quasi uniform illumination it is applicable also to the case of point sources. For the last case, the narrower the source PSF, the higher the accuracy of the 3D model.
This model still uses the (β,λ) parameters which were used for the uniform illumination case. No supplementary parameters are required. But in 3D case, where the exact topology of the detector array should be involved in the account, these two parameters describing the transient properties of each pixel are directly expressed through the parameters characterizing the technological quality of the detector bulk and its contacts. This fact gave the way to optimize future Si:Ga photodetectors.
We present here the direct model and also a preliminary inversion method. We discuss the limitations in the theory, the direct model and the correction method. This new physical model can now be used to reconsider the point source photometry and to remove all the artifact following observation of point sources in the raster maps. It is still important since the LW CAM wavelengths (˜5-18 μ m) will not be covered by SIRTF and ASTRO-F.

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