HESS J1813-178 is one of the brightest sources detected during the first HESS
Galactic Plane survey. The compact source, also detected by MAGIC, is believed
to be a pulsar wind nebula powered by one of the most powerful pulsars known in
the Galaxy, PSR J1813-1749 with a spin-down luminosity of EΛ=5.6β 1037ergsβ1. With its extreme physical
properties, as well as the pulsar's young age of 5.6 kyrs, the Ξ³-rays
detected in this region allow us to study the evolution of a highly atypical
system. Previous studies of the region in the GeV energy range show emission
extended beyond the size of the compact H.E.S.S. source. Using the archival
H.E.S.S. data with improved background methods, we perform a detailed
morphological and spectral analysis of the region. Additionally to the compact,
bright emission component, we find significantly extended emission, whose
position is coincident with HESS J1813-178. We reanalyse the region in GeV and
derive a joint-model in order to find a continuous description of the emission
in the region from GeV to TeV. Using the results derived in this analysis, as
well as X-ray and radio data of the region, we perform multi-wavelength
spectral modeling. Possible hadronic or leptonic origins of the Ξ³-ray
emission are investigated, and the diffusion parameters necessary to explain
the extended emission are examined.Comment: 8 pages, 4 figures, 1 table, In proceedings of ICRC202