Effect of noise in image restoration of multi-aperture telescope

Details Effect of noise in image restoration of multi-aperture telescope Effect of noise in image restoration of multi-aperture telescope

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010spie.7740e.126z&link_type=abstract

Software and Cyberinfrastructure for Astronomy. Edited by Radziwill, Nicole M.; Bridger, Alan. Proceedings of the SPIE, Volume 7

Astronomy and Astrophysics

Astronomy

Scientific paper

Multi-aperture telescope is proposed to achieve high angular resolution without fabricating a large diameter monolithic primary mirror. Due to the array structure, the multi-aperture telescope has almost the same cut-off frequency as an equivalent diameter telescope, but decrease in the area of light collecting, which is the reason that the direct output image of multi-aperture telescope is blurred and low contrast. The additive noise level is another reason for low image quality. The Wiener filter is sensitive to noise because of the zero value out of the cut-off frequency in optical transfer function. An alternative image deblurring method is total variation (TV) blind deconvolution. The TV method is an iterative algorithm and preserves the edge information well. The most important characteristic of TV blind deconvolution is that the algorithm is still working with high noise level and produces reasonable result.

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