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Proceedings Paper

Coronagraph design for an extreme adaptive optics system with spatially filtered wavefront sensing on segmented telescopes
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Paper Abstract

High dynamic range coronagraphy targeted at discovering planets around nearby stars is often associated with monolithic, unobstructed aperture space telescopes. With the advent of extreme adaptive optics (ExAO) systems with thousands of sensing and correcting channels, the benefits of placing a near-infrared coronagraph on a large segmented mirror telescope become scientifically interesting. This is because increased aperture size produces a tremendous gain in achievable contrast at the same angular distance from a point source at Strehl ratios in excess of 90\% (and at lower Strehl ratios on future giant telescopes such as the Thirty Meter Telescope). We outline some of the design issues facing such a coronagraph, and model a band-limited coronagraph on an aperture with a Keck-like pupil. We examine the purely diffractive challenges facing the eXtreme AO Planetary Imager (XAOPI) given the Keck pupil geometry, notably its inter-segment gap spacing of 6~mm. Classical Lyot coronagraphs, with hard-edged occulting stops, are not efficient enough at suppressing diffracted light, given XAOPI's scientific goal of imaging a young Jupiter at a separation as close as 0.15 arcseconds (4λD at H on Keck) from its parent star. With a 4000 channel ExAO system using an anti-aliased spatially-filtered wavefront sensor planned for XAOPI, we wish to keep diffracted light due to coronagraphic design at least as low as the noise floor set by AO system limitations. We study the band-limited Lyot coronagraph (BLC) as a baseline design instead of the classical design because of its efficient light suppression, as well as its analytical simplicity. We also develop ways of investigating tolerancing coronagraphic mask fabrication by utilizing the BLC design's mathematical tractability.

Paper Details

Date Published: 25 October 2004
PDF: 10 pages
Proc. SPIE 5490, Advancements in Adaptive Optics, (25 October 2004); doi: 10.1117/12.551939
Show Author Affiliations
Anand Sivaramakrishnan, Space Telescope Science Institute (United States)
Univ. of California/Santa Cruz (United States)
Russell B. Makidon, Space Telescope Science Institute (United States)
Univ. of California/Santa Cruz (United States)
Remi Soummer, Space Telescope Science Institute (United States)
Univ. of California/Santa Cruz (United States)
Bruce A. Macintosh, Lawrence Livermore National Lab. (United States)
Univ. of California/Santa Cruz (United States)
Mitchell Troy, Jet Propulsion Lab. (United States)
Univ. of California/Santa Cruz (United States)
Gary A. Chanan, Univ. of California/Irvine (United States)
Univ. of California/Santa Cruz (United States)
James P. Lloyd, California Institute of Technology (United States)
Univ. of California/Santa Cruz (United States)
Marshall D. Perrin, Univ. of California/Berkeley (United States)
Univ. of California/Santa Cruz (United States)
James R. Graham, Univ. of California/Berkeley (United States)
Univ. of California/Santa Cruz (United States)
Lisa Poyneer, Lawrence Livermore National Lab. (United States)
Univ. of California/Santa Cruz (United States)
Andrew I. Sheinis, Univ. of California/Santa Cruz (United States)


Published in SPIE Proceedings Vol. 5490:
Advancements in Adaptive Optics
Domenico Bonaccini Calia; Brent L. Ellerbroek; Roberto Ragazzoni, Editor(s)

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