Manuel Anastacia M, Phillion Donald W, Olivier Scot S, Baker Kevin L, Cannon Brice
Lawrence Livermore National Laboratory, Livermore, CA 94550, USA.
Opt Express. 2010 Jan 18;18(2):1528-52. doi: 10.1364/OE.18.001528.
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.
大型综合巡天望远镜（LSST）采用了一种新颖的三镜、改进型保罗-贝克设计，主镜直径8.4米，副镜直径3.4米，三镜直径5.0米，还有三个折射校正透镜，以产生一个视场为9.6平方度的平 focal平面。为了在运行过程中保持图像质量，必须主动控制三块大镜子的变形和刚体运动，以尽量减少主要由重力和热膨胀引起的力所导致的光学像差。我们描述了使用位于LSST相机焦平面四个角的一组曲率波前传感器测量望远镜像差的方法。我们对波前传感系统进行了全面分析，包括参考星的可用性，证明该系统将达到满足LSST性能目标所需的规格要求。
