Wavefront reconstruction algorithms for astronomical adaptive optics systems

Details Wavefront reconstruction algorithms for astronomical adaptive optics systems Wavefront reconstruction algorithms for astronomical adaptive optics systems

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994spie.2201..655s&link_type=abstract

Proc. SPIE Vol. 2201, p. 655-662, Adaptive Optics in Astronomy, Mark A. Ealey; Fritz Merkle; Eds.

Physics

Optics

Scientific paper

The requirements of wavefront reconstruction algorithm for use in astronomical adaptive optics systems are discussed. We present the results of realistic numerical simulations of the closed-loop performance of a Shack-Hartmann wavefront sensor used in conjunction with a high-order segmented mirror suitable for adaptive correction on a 4 m telescope at visible wavelengths. Iterative over-relaxation methods are used to derive the segment piston values, and we investigate the behavior of these techniques in the presence of photon and detector noise. We also discuss the use of non variance-minimizing techniques to optimize the point- spread function for particular astronomical applications.

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