期刊
OPTICS EXPRESS
卷 18, 期 2, 页码 1528-1552出版社
OPTICAL SOC AMER
DOI: 10.1364/OE.18.001528
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资金
- National Science Foundation [9 (AST-0551161), 1 (AST-0244680), AST-0132798]
- U.S. Department of Energy [DE-AC02-76SF00515, DE-AC02-98CH10886, W-7405-Eng-48, DE-AC52-07NA27344]
- LSSTC Institutional Members
- Lawrence Livermore National Laboratory
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1036980] Funding Source: National Science Foundation
The Large Synoptic Survey Telescope (LSST) uses a novel, three-mirror, modified Paul-Baker design, with an 8.4-meter primary mirror, a 3.4-m secondary, and a 5.0-m tertiary, along with three refractive corrector lenses to produce a flat focal plane with a field of view of 9.6 square degrees. In order to maintain image quality during operation, the deformations and rigid body motions of the three large mirrors must be actively controlled to minimize optical aberrations, which arise primarily from forces due to gravity and thermal expansion. We describe the methodology for measuring the telescope aberrations using a set of curvature wavefront sensors located in the four corners of the LSST camera focal plane. We present a comprehensive analysis of the wavefront sensing system, including the availability of reference stars, demonstrating that this system will perform to the specifications required to meet the LSST performance goals. (C) 2010 Optical Society of America
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