Studying the TeV gamma-ray morphology of MSH 15-52
(Supervision: Markus Holler)


MSH 15-52 is a Pulsar Wind Nebula, consisting of highly relativistic electrons and positrons which radiate both synchrotron and Inverse Compton emission. Through these two non-thermal processes the source has been detected in X-rays and TeV gamma-rays. Although the respective photon energies differ by a factor of 1 million, they are both connected to the same particle population. In TeV gamma-rays, MSH 15-52 has been detected by the Imaging Atmospheric Cherenkov Telescopes of the H.E.S.S. array and is seen to be slightly extended with respect to the Point Spread Function (PSF). Within the last years, a new, more realistic simulation appraoch has been implemented in the H.E.S.S. software. This allows to simulate the PSF with an improved precision, in turn enabling to better investigate the gamma-ray morphology of slightly extended sources. The goal of this Bachelor Thesis is thus to study the TeV gamma-ray morphology of MSH 15-52 with the PSF from the new simulation approach. The better PSF will then allow a better comparison of the X-ray and TeV gamma-ray morphology of this source.


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