14 September 2007 Stray light design and analysis of the SNAP Telescope
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Abstract
SNAP is a proposed space-based experiment designed to quantify dark energy by measuring the redshift-magnitude diagram of supernovae and to quantify the growth of structure in the universe by measuring weak gravitational lensing over cosmological distances. The baseline SNAP telescope is an ambient temperature three-mirror anastigmat (TMA). The goal of the stray light design is to ensure that stray light in the 0.4 to 1.7 micron wavelength range does not exceed a small fraction of Zodiacal radiation within the mission's target field near the North ecliptic pole. At visible wavelengths, we expect the primary source of stray light will be starlight scattered by the primary mirror. In our longest wavelength NIR band we expect thermal emission from the mirrors and structure will dominate. Scattered stray light is mitigated by an internal field stop, and a cold (140K) internal aperture stop. Stray light scattered by mirror roughness and particulate contamination, as well as scattering from the telescope baffles are modeled and quantified. The baseline design and analyses contained herein ensure that stray light will be less than 10% of Zodiacal in all bands.
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M. J. Sholl, F. S. Grochocki, J. C. Fleming, R. W. Besuner, P. Jelinsky, M. L. Lampton, "Stray light design and analysis of the SNAP Telescope", Proc. SPIE 6675, Optical Modeling and Performance Predictions III, 66750C (14 September 2007); doi: 10.1117/12.732517; https://doi.org/10.1117/12.732517
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