Eclipse telescope design factors

Tony Hull; John T. Trauger; Steven A. Macenka; Dwight Moody; Guillermo Olarte; Cesar Sepulveda; Walter Tsuha; David Cohen

doi:10.1117/12.457884

3 March 2003 Eclipse telescope design factors

Tony Hull, John T. Trauger, Steven A. Macenka, Dwight Moody, Guillermo Olarte, Cesar Sepulveda, Walter Tsuha, David Cohen

Author Affiliations +

Proceedings Volume 4860, High-Contrast Imaging for Exo-Planet Detection; (2003) https://doi.org/10.1117/12.457884
Event: Astronomical Telescopes and Instrumentation, 2002, Waikoloa, Hawai'i, United States

Abstract

Very high contrast imagery, required for exoplanet image acquisition, imposes significantly different criteria upon telescope architecture than do the requirements imposed upon most spaceborne telescopes. For the Eclipse Mission, the fundamental figure-of-merit is a stellar contrast, or brightness reduction ratio, reaching a factor of 10^-9 or better at star-planet distances as close as the 4th Airy ring. Factors necessary to achieve such contrast ratios are both irrelevant and largely ignored in contemporary telescope design. Although contemporary telescoeps now meet Hubble Space Telescope performance at substantially lower mass and cost than HST, control of mid-spatial-frequency (MSF) errors, crucial to coronagraphy, has not been emphasized. Accordingly, roughness at MSF has advanced little since HST. Fortunately, HST primary mirror smoothness would nearly satisfy Eclipse requirements, although other aspects of HST are undesirable for stellar coronagraphy. Conversely, the narrow field required for Eclipse eases other drivers of traditional telescope design. A systematic approach to telescope definition, with primary and sub-tier figures-of-merit, will be discussed in the context of the Eclipse Mission.

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Tony Hull, John T. Trauger, Steven A. Macenka, Dwight Moody, Guillermo Olarte, Cesar Sepulveda, Walter Tsuha, and David Cohen "Eclipse telescope design factors", Proc. SPIE 4860, High-Contrast Imaging for Exo-Planet Detection, (3 March 2003); https://doi.org/10.1117/12.457884

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