Wavefront sensor optimization in astronomical applications

Details Wavefront sensor optimization in astronomical applications Wavefront sensor optimization in astronomical applications

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993spie.1781..224l&link_type=abstract

Proc. SPIE Vol. 1781, p. 224-231, Specification and Measurement of Optical Systems, Lionel R. Baker; Ed.

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Microlens arrays made by engraving photoresist coatings are suitable for astronomical applications, especially in the Shack-Hartmann type of wavefront sensor. Their characteristics have to be carefully chosen to fit the turbulence strength. Our instrument, composed of a photon-counting device and a Shack-Hartmann sensor, allows synchronous recordings of short-exposure images and their corresponding wavefronts. In post-processing, the point spread functions (PSF) are calculated and used to deconvolve the direct images. A new real- time centroiding device transforms this experiment into a quasi real-time imaging corrective system.

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