Photon-counting speckle masting

Karl-Heinz Hofmann; W. Mauder; Gerd Weigelt

doi:10.1117/12.34796

1 July 1990 Photon-counting speckle masting

Karl-Heinz Hofmann, W. Mauder, Gerd Weigelt

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Proceedings Volume 1319, Optics in Complex Systems; (1990) https://doi.org/10.1117/12.34796
Event: 15th International Optics in Complex Systems, 1990, Garmisch, Germany

Abstract

The resolution of conventional astronomical images made with large, ground-based telescopes is limited to about 0.3 to 1 arcsec by atmospheric turbulence. Much higher resolution can be obtained by the speckle masking method13 . Speckle masking yields images with diffraction-limited resolution, for example, 0.03 arcsec resolution for a 3.6-rn telescope. In speckle masking a large number of speckle interferograms (short-exposure photographs; exposure time 0.05 sec) has to be evaluated. The first image processing step is the calculation of the ensemble average bispectrum or the ensemble average triple correlation of all speckle interferograms. The speckle interferograms of faint astronomical objects consist of only a small number of photon events. For example in the NGC 1068 experiment described below, each of the 10 000 evaluated speckle interferograms consisted of about 400 photon events only. As described in the next section, triple correlation or bispectrum processing can be applied to the photon-counting speckle interferograms.

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Karl-Heinz Hofmann, W. Mauder, and Gerd Weigelt "Photon-counting speckle masting", Proc. SPIE 1319, Optics in Complex Systems, (1 July 1990); https://doi.org/10.1117/12.34796

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