Wavefront Amplitude and Phase Correction Using Pupil Shape Diversity

Details Wavefront Amplitude and Phase Correction Using Pupil Shape Diversity Wavefront Amplitude and Phase Correction Using Pupil Shape Diversity

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...20715303g&link_type=abstract

American Astronomical Society Meeting 207, #153.03; Bulletin of the American Astronomical Society, Vol. 37, p.1413

Astronomy and Astrophysics

Astronomy

Scientific paper

High contrast imaging from space must overcome photon noise of the diffracted star light and scattered light from optical components defects. The very high contrast required (up to 10-10 for terrestrial planets) puts severe requirements on the wavefront control system, as the achievable contrast is limited by the quality of the wavefront. In this paper we present an iterative method for the shaped pupil coronagraph to minimize the energy in a pre-defined region in the image where terrestrial planets would be found. The method uses three intensity measurements in the image plane with a pinhole added to the shaped pupil for diversity. This method has been shown in simulations to be effective in the presence of photon noise, deformable mirror modeling errors and overcoming defective actuators in the deformable mirror.

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