3 November 1983 Reflecting Correctors For Large Spherical Primaries
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Two aspheric reflecting elements can correct exactly the spherical aberration and coma of a spherical primary mirror. The remaining off-axis aberrations depend mainly on the sizes of the secondary and tertiary mirrors. Two solutions are presented in which the secondary mirror is 1 meter in diameter. The first is for a 5-meter f/0.8 primary suitable for use as an optical Arecibo (fixed primary) telescope. The second is for a fully steerable telescope with a 12-meter f/1.33 primary. In both cases, 1 arcsecond images are formed at the edge of a field 4 arcminutes in diameter. The collimation tolerances for the corrector assemblies are stringent in comparison to most conventional telescopes, but modest in comparison to the precision required to maintain a segmented primary mirror.
© (1983) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Stephen A. Shectman, "Reflecting Correctors For Large Spherical Primaries", Proc. SPIE 0444, Advanced Technology Optical Telescopes II, (3 November 1983); doi: 10.1117/12.937964; https://doi.org/10.1117/12.937964

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