Speaker
Description
Supernova remnants (SNRs) are widely believed to be the dominant accelerators of Galactic cosmic rays (CRs) with energies up to the knee. The electrons and protons can be accelerated to be the ultra-relativistic particles by the shock of SNRs via the diffusive shock acceleration (DSA) mechanism. HESS J1813-178 is one of the brightest and most compact objects detected by the HESS Galactic Plane Survey and MAGIC observations. A young 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. Previous studies show that the GeV emission around HESS J1813-178 is much more extended than its TeV emission. With the Fermi-LAT analysis, we did a detailed morphological and spectral analysis in the region of HESS J1813-178 and found that the GeV gamma-ray morphology is consistent with the TeV contours of MAGIC. Meanwhile, the GeV spectrum is hard with index of ~2.0, which connects smoothly with that of HESS J1813-178. The possible origins of the gamma-ray emission from HESS J1813-178 are discussed.
| Subcategory | Experimental Results |
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