A Fourier domain model for estimating astrometry errors due to static and quasi-static optical surface errors
A Fourier domain model for estimating astrometry errors due to static and quasi-static optical surface errors
复制标题
用于估计静态和准静态光学表面误差引起的天体测量误差的傅立叶域模型
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发表时间：
2013
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通讯作者：
B. Ellerbroek
中科院分区：
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作者：
B. Ellerbroek
上下文自适应光学系统和科学仪器中的光学面形误差引起的波前像差是高精度天体测量的重要误差源。目标。本文导出了这些误差的计算公式，这些公式在制定天体测量误差预算和光学表面质量规范时可能是有用的。方法.使用傅立叶域方法，并且每个光学表面上的误差被建模为“相位屏”，其在距光学系统光瞳的一个或多个共轭范围处具有静态统计。三类误差被认为是：（i）在初始校准的静态表面误差的影响的误差;（ii）光束平移的影响，或“漂移”，由于（例如）仪器的轴线校准误差的光学表面;和（iii）准静态的表面误差，从一个观察到下一个变化。结果对于每一个这些影响，我们开发的公式描述的位置估计误差在一个科学领域的一个单一的观察，以及两个单独的观察之间的差分误差。文中给出了三种误差的数值计算结果，包括对30米望远镜和NFIRAOS第一束光自适应光学系统的计算结果。
Context. The wavefront aberrations due to optical surface errors in adaptive optics systems and science instruments can be a significant error source for high precision astrometry. Aims. This report derives formulas for evaluating these errors which may be useful in developing astrometry error budgets and optical surface quality specifications. Methods. A Fourier domain approach is used, and the errors on each optical surface are modeled as “phase screens” with stationary statistics at one or several conjugate ranges from the optical system pupil. Three classes of error are considered: (i) errors in initially calibrating the effects of static surface errors; (ii) the effects of beam translation, or “wander,” across optical surfaces due to (for example) instrument boresighting error; and (iii) quasistatic surface errors which change from one observation to the next. Results. For each of these effects, we develop formulas describing the position estimation errors in a single observation of a science field, as well as the differential error between two separate observations. Sample numerical results are presented for the three classes of error, including some sample computations for the Thirty Meter Telescope and the NFIRAOS first-light adaptive optics system.