Numerical simulation of observational telescope with the dynamic holographic correction

Abstract

Described are the methods of numerical design and simulation of observational telescopes, using the thin (plain) dynamic hologram as the corrector for image distortions, imposed by the primary mirror surface defects.Hologram application to compensation for distortions of the primary mirror of imaging telescope was first proposed and realised by Yu.N.Denisyuk and S.I.Soskin [1,2] (Fig. 1). In these works the conventional static hologram of distortions of primary mirror was registered on photoplate, using the auxiliary scheme, working from this mirror centre of curvature. This hologram was then processed and mounted in the focal unit of the telescope. Such a scheme did not cope for dynamic distortions and was rather hard to be aligned and adjusted. So until recently this approach was used in practice only for correction for the regular aberrations of the system of Zeidel kind.

<title>White light imaging using large-numerical-aperture telescope with dynamic holographic correction for primary mirror distortions</title>

“…Laser radiation enters the system as the beam with the plain wavefront through the beam splitting cube. Two component lens of special 1,22 (clear aperture 30 mm) focuses it to the PM center of curvature. The radiation, reflected by the PM, goes back through the lens.…”

<title>Large-numerical-aperture imaging bypass system with dynamic holographic correction for primary mirror distortions</title>

“…Two component lens of special 1,22 (clear aperture 30 mm) focuses it to the PM center of curvature. Laser radiation enters the system as the beam with the plain wavefront through the beam splitting cube.…”