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Proceedings Paper

Preliminary analysis of effect of random segment errors on coronagraph performance
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Paper Abstract

“Are we alone in the Universe?” is probably the most compelling science question of our generation. To answer it requires a large aperture telescope with extreme wavefront stability. To image and characterize Earth-like planets requires the ability to block 1010 of the host star’s light with a 10-11 stability. For an internal coronagraph, this requires correcting wavefront errors and keeping that correction stable to a few picometers rms for the duration of the science observation. This requirement places severe specifications upon the performance of the observatory, telescope and primary mirror. A key task of the AMTD project (initiated in FY12) is to define telescope level specifications traceable to science requirements and flow those specifications to the primary mirror. From a systems perspective, probably the most important question is: What is the telescope wavefront stability specification? Previously, we suggested this specification should be 10 picometers per 10 minutes; considered issues of how this specification relates to architecture, i.e. monolithic or segmented primary mirror; and asked whether it was better to have few or many segments. This paper reviews the 10 picometers per 10 minutes specification; provides analysis related to the application of this specification to segmented apertures; and suggests that a 3 or 4 ring segmented aperture is more sensitive to segment rigid body motion that an aperture with fewer or more segments.

Paper Details

Date Published: 24 September 2015
PDF: 14 pages
Proc. SPIE 9605, Techniques and Instrumentation for Detection of Exoplanets VII, 96050P (24 September 2015); doi: 10.1117/12.2190160
Show Author Affiliations
Mark T. Stahl, NASA Marshall Space Flight Ctr. (United States)
Stuart B. Shaklan, Jet Propulsion Lab. (United States)
H. Philip Stahl, NASA Marshall Space Flight Ctr. (United States)

Published in SPIE Proceedings Vol. 9605:
Techniques and Instrumentation for Detection of Exoplanets VII
Stuart Shaklan, Editor(s)

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