E. Hege, M. Cheselka, M. Lloyd-Hart, P. Hinz, W. Hoffmann, J. Christou, S. Jefferies
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Astronomical Results using Physically-Constrained Iterative Deconvolution
Iterative physical deconvolution is used for point spread function (psf) calibration of a wide range of astronomical imagery obtained in visible (CCD) through near- and mid-infrared (NICMOS and MIRAC) wavelengths. Psf complications, ranging from those of uncorrected speckle images at large telescopes to those of contemporary high-performance adaptive optics, are accomodated by this algorithm which makes use of a priori physical information about the imaging system. Examples of diffraction-limited and “super-resolved” results are presented for a variety of different astronomical objects.
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