Abstract
HESS J1813-178 is one of the brightest and most compact objects detected by the HESS Galactic Plane Survey and MAGIC observations. A young supernova remnant (SNR) G12.8–0.0 locates within the TeV extent of HESS J1813-178. And a pulsar wind nebula (PWN) driven by an energetic X-ray pulsar PSR J1813-1749 is embedded in the SNR, together with a young stellar cluster, C1 1813-178, detected in this region. The origin of the gamma-ray emission from HESS J1813-178 is still not clear. Previous studies show that the GeV emission around HESS J1813-178 is much more extended than its TeV emission. With the Fermi-LAT data analysis, we did a detailed morphological and spectral analysis in the region of HESS J1813-178 and found that the GeV gamma-ray morphology above 20 GeV is much smaller, which is close to the TeV gamma-ray contours. Meanwhile, the GeV spectrum above 20 GeV is hard with an index of ~2.07, which connects smoothly with that of HESS J1813-178.
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