Kavli Affiliate: Steven Kahn
| First 5 Authors: Andrew Rasmussen, Pierre Antilogus, Pierre Astier, Chuck Claver, Peter Doherty
| Summary:
Near-future astronomical survey experiments, such as LSST, possess system
requirements of unprecedented fidelity that span photometry, astrometry and
shape transfer. Some of these requirements flow directly to the array of
science imaging sensors at the focal plane. Availability of high quality
characterization data acquired in the course of our sensor development program
has given us an opportunity to develop and test a framework for simulation and
modeling that is based on a limited set of physical and geometric effects. In
this paper we describe those models, provide quantitative comparisons between
data and modeled response, and extrapolate the response model to predict
imaging array response to astronomical exposure. The emergent picture departs
from the notion of a fixed, rectilinear grid that maps photo-conversions to the
potential well of the channel. In place of that, we have a situation where
structures from device fabrication, local silicon bulk resistivity variations
and photo-converted carrier patterns still accumulating at the channel,
together influence and distort positions within the photosensitive volume that
map to pixel boundaries. Strategies for efficient extraction of modeling
parameters from routinely acquired characterization data are described. Methods
for high fidelity illumination/image distribution parameter retrieval, in the
presence of such distortions, are also discussed.
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