Abstract
The use of speckle imaging techniques for planetary research is discussed. Data are gathered with a video camera system. Image reconstruction uses a division algorithm for Fourier amplitudes and the Knox-Thompson algorithm for Fouroer phases. Bias correction techniques for arbitrary “photon shapes” have been developed. Results have been obtained with a laboratory optical simulator and on Io, Titan, Pallas, Jupiter, and Uranus using the 2.24-m telescope on Mauna Kea. All evidence indicates that spatial resolutions less than the seing limit by a factor of about 4 can be obtained. This applies to objects brighter than Uranus. For fainter objectsbias correction is inadequate and images cannot be recovered. Resolutions obtained are well above the diffraction limit. The reasons for this performance are understood in terms of inadequacies in the video camera. A photon-counting camera has been developed which should eliminate these problems. If so, it should be possible to obtain diffraction-limited resolution on objects as faint as Charon.
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