5 October 2005 Wavefront amplitude variation of TPF's high-contrast imaging testbed: modeling and experiment
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Proceedings Volume 5905, Techniques and Instrumentation for Detection of Exoplanets II; 59051L (2005); doi: 10.1117/12.618574
Event: Optics and Photonics 2005, 2005, San Diego, California, United States
Abstract
Knowledge of wavefront amplitude is as important as the knowledge of phase for a coronagraphic high contrast imaging system. Efforts have been made to understand various contributions to the amplitude variation in Terrestrial Planet Finder's (TPF) High Contrast Imaging Testbed (HCIT). Modeling of HCIT with as-built mirror surfaces has shown an amplitude variation of 1.3% due to the phase-amplitude mixing for the testbed's front-end optics. Experimental measurements on the testbed have shown the amplitude variation is about 2.5% with the testbed's illumination pattern having a major contribution to the low order amplitude variation.
© (2005) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Fang Shi, Andrew E. Lowman, Dwight C. Moody, Albert F. Niessner, John T. Trauger, "Wavefront amplitude variation of TPF's high-contrast imaging testbed: modeling and experiment", Proc. SPIE 5905, Techniques and Instrumentation for Detection of Exoplanets II, 59051L (5 October 2005); doi: 10.1117/12.618574; https://doi.org/10.1117/12.618574
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KEYWORDS
Mirrors

Wavefronts

Cameras

Near field optics

Imaging systems

Stars

Optical testing

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