Optical aperture synthesis wave-front sensing

Details Optical aperture synthesis wave-front sensing Optical aperture synthesis wave-front sensing

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...256..715t&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 256, no. 2, p. 715-722.

Astronomy and Astrophysics

Astronomy

Apertures, Image Processing, Interferometry, Wave Fronts, Seeing (Astronomy), Signal To Noise Ratios, Transfer Functions

Scientific paper

To apply phase closure with an array of optical telescopes, each aperture must be phased. This sets an upper limit on the size of each aperture equal to the coherence area of the wave fronts (if no adaptive optics is used). By recording the wave-front on each aperture and by post-processing, it is possible to apply phase closure algorithms with apertures sustaining an arbitrary high number of coherence areas, as far as the combination remains coherent. This procedure increases substantially the signal-to-noise ratio in the visible and stands as a complement when adaptive optics only provides a partial correction of wave-fronts.

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