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Skymaps measured with imaging atmospheric Cherenkov telescopes (IACTs)represent the real source distribution convolved with the point spread functionof the observing instrument. Current IACTs have an angular resolution in theorder of 0.1$^\circ$ which is rather large for the study of morphologicalstructures and for comparing the morphology in $\gamma$-rays to measurements inother wavelengths where the instruments have better angular resolutions.  Serendipitously it is possible to approximate the underlying true sourcedistribution by applying a deconvolution algorithm to the observed skymap, thuseffectively improving the instruments angular resolution. From the multitude ofexisting deconvolution algorithms several are already used in astronomy, but inthe special case of $\gamma$-ray astronomy most of these algorithms arechallenged due to the high noise level within the measured data.  One promising algorithm for the application to $\gamma$-ray data is theMaximum Entropy Algorithm. The advantages of this algorithm are the possibilityto take a priori knowledge into account and that it is an independent approachto previous work, e.g., Heinz et al. (2012) who applied the Richardson LucyAlgorithm to $\gamma$-ray skymaps.  An implementation of the Maximum Entropy Algorithm is provided in the MemSys5software package by Gull and Skilling (1999). As this algorithm is verysensitive to various input parameters it is essential to understand theirinfluences. We present a study of the influences of these parameters in orderto investigate the applicability of the Maximum Entropy Algorithm for thedeconvolution of skymaps in $\gamma$-ray astronomy.

Application of Maximum Entropy Deconvolution to ${\gamma}$-ray Skymaps