The major goals of adaptive optics for astronomy are two-fold; firstly to improve the image quality by reducing the atmospherically-induced wavefront aberrations and secondly to provide a stable point spread function. However, the quality of compensation depends upon a number of factors so that a point source reference does not necessarily have the same point spread function as that used for the target of interest. Thus, standard deconvolution techniques are limited. The application of a general myopic/blind deconvolution technique to astronomical adaptive optics data will be discussed with an emphasis on the ability to obtain quantitative measurements from deconvolved images.
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