Abstract
This paper discusses the results of a study of the optical systems of two types of earth-based wide-angle telescopes intended for monitoring celestial objects. The first type is a two-mirror system with a two-lens afocal corrector that contains aspheric surfaces, installed in convergent pencils of rays between the secondary mirror and the image plane. The second type is a Cassegrain system with a prefocal meniscus corrector and a focal-length converter installed in convergent beams between the corrector and the image plane. Design parameters are given for systems with a 1-m effective aperture, a 3-m focal length, and a 2°–2.5° angular field. Their advantages and disadvantages are discussed.
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