Restoration of Astronomical Images by Blind Iterative Deconvolution

Details Restoration of Astronomical Images by Blind Iterative Deconvolution Restoration of Astronomical Images by Blind Iterative Deconvolution

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.1308j&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #13.08; Bulletin of the American Astronomical Society, Vol. 24, p.1140

Physics

Optics

2

Scientific paper

Image degradation, whether due to turbulent atmospheric motion and/or inherent defects in imaging optics, causes attenuation and/or loss of the high-spatial frequency content of astronomical images. Knowledge of a point spread function (Psf) permits restoration of these spatial frequencies. However, not all Psf's are well behaved and can vary both in time and also location across the image. Thus optimal image restoration requires both the object and Psf to be restored from a ``blurred'' image. This is known as blind deconvolution. In this paper we describe an algorithm that incorporates a priori image information as constraints for deconvolution by error metric minimization using a conjugate gradient technique. We demonstrate the effectiveness of this algorithm to recover a complex object and Psf using simulated speckle interferometric data under different signal-to-noise conditions for both single and multiple frame input. We present astronomical results using both speckle interferometric data, e.g. near-infrared images of 4 Vesta, and direct near-infrared images of the Galactic Center obtained using an adaptive tip-tilt secondary. This work was supported by the NSF through grants DPP 89-17626, AST 88-22465 and AST 92-03336.

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