Revision of the GeV $γ$-ray Emission in the Region of HESS J1813-178 with Fermi-LAT
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arXiv
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| Autores principales: | , |
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| Formato: | Preprint |
| Publicado: |
2024
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| _version_ | 1866914684985147392 |
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| author | Guo, Xiaolei Xin, Yuliang |
| author_facet | Guo, Xiaolei Xin, Yuliang |
| contents | HESS J1813-178 is one of the brightest and most compact TeV $γ$-ray sources, and whether its $γ$-ray emission is associated with supernova remnant (SNR), pulsar wind nebula (PWN) or young stellar cluster (YSC) is still under debate. By analysing the GeV $γ$-ray data in the field of HESS J1813-178 using 14 years of PASS 8 data recorded by the Fermi Large Area Telescope (Fermi-LAT), we report the discovery of three different sources with different spectra in this region. The hard source with a power law spectral index of 2.11 $\pm$ 0.08 has a small size extension, which is spatially and spectrally coincident with the TeV $γ$-ray emission from HESS J1813-178. CO observations display the dense molecular clouds surrounding HESS J1813-178 in the velocity range of 45-60 km s$^{\rm -1}$. The possible origins of the $γ$-ray emission from HESS J1813-178 are discussed, including SNR G12.82-0.02, the PWN driven by the energetic X-ray pulsar PSR J1813-1749, and YSC Cl 1813-178. However, none of them can be ruled out clearly. Note that the maximum energy of protons in the hadronic model should exceed a few hundred TeV, which makes HESS J1813-178 to be a promising PeVatron. The detailed LHAASO data analysis about the morphology and spectrum would be helpful to investigate the origin of the $γ$-ray emission in this region and test its PeVatron nature. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2402_11880 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Revision of the GeV $γ$-ray Emission in the Region of HESS J1813-178 with Fermi-LAT Guo, Xiaolei Xin, Yuliang High Energy Astrophysical Phenomena HESS J1813-178 is one of the brightest and most compact TeV $γ$-ray sources, and whether its $γ$-ray emission is associated with supernova remnant (SNR), pulsar wind nebula (PWN) or young stellar cluster (YSC) is still under debate. By analysing the GeV $γ$-ray data in the field of HESS J1813-178 using 14 years of PASS 8 data recorded by the Fermi Large Area Telescope (Fermi-LAT), we report the discovery of three different sources with different spectra in this region. The hard source with a power law spectral index of 2.11 $\pm$ 0.08 has a small size extension, which is spatially and spectrally coincident with the TeV $γ$-ray emission from HESS J1813-178. CO observations display the dense molecular clouds surrounding HESS J1813-178 in the velocity range of 45-60 km s$^{\rm -1}$. The possible origins of the $γ$-ray emission from HESS J1813-178 are discussed, including SNR G12.82-0.02, the PWN driven by the energetic X-ray pulsar PSR J1813-1749, and YSC Cl 1813-178. However, none of them can be ruled out clearly. Note that the maximum energy of protons in the hadronic model should exceed a few hundred TeV, which makes HESS J1813-178 to be a promising PeVatron. The detailed LHAASO data analysis about the morphology and spectrum would be helpful to investigate the origin of the $γ$-ray emission in this region and test its PeVatron nature. |
| title | Revision of the GeV $γ$-ray Emission in the Region of HESS J1813-178 with Fermi-LAT |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2402.11880 |