Iterative method of baffle design for modified Ritchey–Chretien telescope

Abstract

We developed a baffle design method based on a combination of the results of optical design software and analytical relations formulated herein. The method finds the exact solution for baffle parameters of a modified Ritchey-Chretien telescope by iteratively solving the analytical relations using the actual ray coordinates of the telescope computed with the aid of optical design software. The baffle system so designed not only blocks the direct rays of stray light reaching the image plane but also provides minimum obscuration to imaging light. Based on the iterative method, we proposed a baffle design approach for a rectangular-image-format telescope.

Stray light control for the space-agile optical system with a pointing mirror

“…Baffles are employed to eliminate the direct light that can reach the detector without any scattering. For a two-mirror optical system, the most common baffles are external baffle and the internal baffles near the mirrors [17][18], as shown in Fig. 5.…”

A high accuracy assembling method of R-C system based on reverse optimization method

“…Reflective system, with its noticeable advantages such as large aperture, long focal length, no chromatic aberration, and wide operating band compared with the refractive system, has been one of the widely applied optical system in the space exploration of space telescope [1,2]. Various reflective systems have been proposed in telescope, for example, Newtonian reflective system [3], Gregorian reflective system [3], Ritchey-Chré tien optical system [4][5][6] (R-C optical system) and Cassegrain optical system [7][8][9]. R-C optical systems are commonly used in long focal length imaging, which have the characteristics such as the compact structure, excellent imaging in the paraxial field of view, easy implementation of heat free, and suitable for lightweight, and the R-C optical systems have been widely used in long focal length imaging and long-distance detection fields such as aerospace, remote sensing, exploration, and space optical communication [10][11][12].…”

Analysis and calculation of the veiling glare index in optical systems

“…Moreover, it is important to measure the level of stray light in the designed optical system [9]. The veiling glare index (VGI) and point source transmittance (PST) are two parameters that are used to evaluate the stray light in an optical system [10][11][12][13]. The PST is used mainly for strong light sources such as the sun.…”