Chipman R A, Brown D M, McGuire J P
Appl Opt. 1992 May 1;31(13):2301-13. doi: 10.1364/AO.31.002301.
The advanced x-ray astrophysics facility (AXAF) telescope consists of six concentric paraboloid-hyperboloid pairs of mirrors that operate near grazing incidence. Because of the substantial polarization effects at large angles of incidence there has been concern regarding the feasibility of doing polarimetry near the telescope focal plane. The primary mirror is shown to act as a tangentially directed half-wave linear retarder and to almost completely depolarize the linearly polarized component of the light. The secondary mirror introduces an additional half-wave of linear retardance. The two-mirror telescope assembly acts as a tangentially directed one-wave linear retarder. Each mirror depolarizes alone but together the two-mirror assembly preserves the polarization state. The net instrumental polarization effects are small and polarimetry is feasible with AXAF.
The polarization aberration function for the telescope is derived by using Jones calculus. Polarization aberration functions are used to calculte the effect of instrumental polarization on the transmitted wave front and the polarization state that is due to the primary mirror and the telescope assembly.
高级X射线天体物理设施（AXAF）望远镜由六对同心抛物面-双曲面镜组成，这些镜子在掠入射附近工作。由于在大入射角时存在显著的偏振效应，人们一直关注在望远镜焦平面附近进行偏振测量的可行性。结果表明，主镜起到切向半波线性延迟器的作用，几乎完全使光的线偏振分量退偏振。副镜引入了额外的半波线性延迟。双镜望远镜组件起到切向单波线性延迟器的作用。每个镜子单独使光退偏振，但双镜组件一起保留了偏振态。仪器的净偏振效应很小，AXAF进行偏振测量是可行的。
通过使用琼斯计算法推导出望远镜的偏振像差函数。偏振像差函数用于计算仪器偏振对透射波前以及由主镜和望远镜组件引起的偏振态的影响。
