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Proceedings Paper

Pupil mapping Exoplanet Coronagraphic Observer (PECO)
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Paper Abstract

The Pupil mapping Exoplanet Coronagraphic Observer (PECO) mission concept is a 1.4-m telescope aimed at imaging and characterizing extra-solar planetary systems at optical wavelengths. The coronagraphic method employed, Phase-Induced Amplitude Apodization or PIAA (a.k.a. pupil mapping) can deliver 1e-10 contrast at 2 lambda/D and uses almost all the starlight that passes through the aperture to maintain higher throughput and higher angular resolution than any other coronagraph or nuller, making PECO the theoretically most efficient existing approach for imaging extra-solar planetary systems. PECO's instrument also incorporates deformable mirrors for high accuracy wavefront control. Our studies show that a probe-scale PECO mission with 1.4 m aperture is extremely powerful, with the capability of imaging at spectral resolution R≈∠15 the habitable zones of already known F, G, K stars with sensitivity sufficient to detect planets down to Earth size, and to map dust clouds down to a fraction of our zodiacal cloud dust brightness. PECO will acquire narrow field images simultaneously in 10 to 20 spectral bands covering wavelengths from 0.4 to 1.0 μm and will utilize all available photons for maximum wavefront sensing and imaging/spectroscopy sensitivity. This approach is well suited for low-resolution spectral characterization of both planets and dust clouds with a moderately sized telescope. We also report on recent results obtained with the laboratory prototype of a coronagraphic low order wavefront sensor (CLOWFS) for PIAA coronagraph. The CLOWFS is a key part of PECO's design and will enable high contrast at the very small PECO inner working angle.

Paper Details

Date Published: 12 July 2008
PDF: 9 pages
Proc. SPIE 7010, Space Telescopes and Instrumentation 2008: Optical, Infrared, and Millimeter, 70101Y (12 July 2008); doi: 10.1117/12.790080
Show Author Affiliations
Olivier Guyon, Steward Observatory, The Univ. of Arizona (United States)
Subaru Telescope, NAOJ (United States)
James R. P. Angel, Steward Observatory, The Univ. of Arizona (United States)
Dana Backman, NASA Ames Research Ctr. (United States)
Ruslan Belikov, NASA Ames Research Ctr. (United States)
Donald Gavel, Univ. of California, Santa Cruz (United States)
Amir Giveon, Jet Propulsion Lab. (United States)
Thomas Greene, NASA Ames Research Ctr. (United States)
Jeremy Kasdin, Princeton Univ. (United States)
James Kasting, Pennsylvania State Univ. (United States)
Marie Levine, Jet Propulsion Lab. (United States)
Mark Marley, NASA Ames Research Ctr. (United States)
Michael Meyer, Steward Observatory, The Univ. of Arizona (United States)
Glenn Schneider, Steward Observatory, The Univ. of Arizona (United States)
Gene Serabyn, Jet Propulsion Lab. (United States)
Stuart Shaklan, Jet Propulsion Lab. (United States)
Michael Shao, Jet Propulsion Lab. (United States)
Motohide Tamura, National Astronomical Observatory of Japan (United States)
Domenick Tenerelli, Lockheed Martin Space Corp. (United States)
Wesley Traub, Jet Propulsion Lab. (United States)
John Trauger, Jet Propulsion Lab. (United States)
Robert Vanderbei, Princeton Univ. (United States)
Robert A. Woodruff, Lockheed Martin Space Corp. (United States)
Neville J. Woolf, Steward Observatory, The Univ. of Arizona (United States)
Jeffrey Wynn, ITT Industries (United States)


Published in SPIE Proceedings Vol. 7010:
Space Telescopes and Instrumentation 2008: Optical, Infrared, and Millimeter
Jacobus M. Oschmann; Mattheus W. M. de Graauw; Howard A. MacEwen, Editor(s)

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