Telescope to Observe Planetary Systems (TOPS): a high throughput 1.2-m visible telescope with a small inner working angle

The Telescope to Observe Planetary Systems (TOPS) is a proposed space mission to image in the visible (0.4-0.9 micron) planetary systems of nearby stars simultaneously in 16 spectral bands (resolution R~20). For the ~10 most favorable stars, it will have the sensitivity to discover 2 R_E rocky plane...

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Bibliographic Details
Published in:arXiv.org 2006-06
Main Authors: Guyon, Olivier, Angel, James R P, Bowers, Charles, Burge, James, Burrows, Adam, Codona, Johanan, Greene, Thomas, Iye, Masanori, Kasting, James, Martin, Hubert, McCarthy, Donald W, Jr, Meadows, Victoria, Meyer, Michael, Pluzhnik, Eugene A, Sleep, Norman, Spears, Tony, Tamura, Motohide, Tenerelli, Domenick, Vanderbei, Robert, Woodgate, Bruce, Woodruff, Robert A, Woolf, Neville J, /
Format: Article
Language:English
Subjects:
Active mirrors
Angular resolution
Apodization
Chromaticity
Coronagraphs
Focal plane
Planet detection
Planetary atmospheres
Planetary systems
Robust control
Spectral bands
Spectrophotometry
Terrestrial planets
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Summary:The Telescope to Observe Planetary Systems (TOPS) is a proposed space mission to image in the visible (0.4-0.9 micron) planetary systems of nearby stars simultaneously in 16 spectral bands (resolution R~20). For the ~10 most favorable stars, it will have the sensitivity to discover 2 R_E rocky planets within habitable zones and characterize their surfaces or atmospheres through spectrophotometry. Many more massive planets and debris discs will be imaged and characterized for the first time. With a 1.2m visible telescope, the proposed mission achieves its power by exploiting the most efficient and robust coronagraphic and wavefront control techniques. The Phase-Induced Amplitude Apodization (PIAA) coronagraph used by TOPS allows planet detection at 2 lambda/d with nearly 100% throughput and preserves the telescope angular resolution. An efficient focal plane wavefront sensing scheme accurately measures wavefront aberrations which are fed back to the telescope active primary mirror. Fine wavefront control is also performed independently in each of 4 spectral channels, resulting in a system that is robust to wavefront chromaticity.
ISSN:2331-8422
DOI:10.48550/arxiv.0606397