Revision of the GeV γ-Ray Emission in the Region of HESS J1813-178 with Fermi-LAT
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 analyzing the GeV γ -ray data in the field of HESS J1813-178 usin...
| Main Authors: | , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2024-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/ad2ae1 |
| _version_ | 1827297921910964224 |
|---|---|
| author | Xiaolei Guo Yuliang Xin |
| author_facet | Xiaolei Guo Yuliang Xin |
| author_sort | Xiaolei Guo |
| collection | DOAJ |
| description | 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 analyzing the GeV γ -ray data in the field of HESS J1813-178 using 14 yr 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 PL spectral index of 2.11 ± 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 ^−1 . The possible origins of the γ -ray emission from HESS J1813-178 are discussed, including SNR G12.820.02, 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 a promising PeVatron. A 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. |
| first_indexed | 2024-04-24T15:05:04Z |
| format | Article |
| id | doaj.art-5d8deb4e410f4f5098651687dfe7ec5e |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-04-24T15:05:04Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-5d8deb4e410f4f5098651687dfe7ec5e2024-04-02T13:33:18ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0196512810.3847/1538-4357/ad2ae1Revision of the GeV γ-Ray Emission in the Region of HESS J1813-178 with Fermi-LATXiaolei Guo0https://orcid.org/0009-0004-5450-8237Yuliang Xin1https://orcid.org/0000-0001-5135-5942School of Physical Science and Technology, Southwest Jiaotong University , Chengdu 610031, People's Republic of China ; xlguo@swjtu.edu.cn, ylxin@swjtu.edu.cnSchool of Physical Science and Technology, Southwest Jiaotong University , Chengdu 610031, People's Republic of China ; xlguo@swjtu.edu.cn, ylxin@swjtu.edu.cnHESS 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 analyzing the GeV γ -ray data in the field of HESS J1813-178 using 14 yr 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 PL spectral index of 2.11 ± 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 ^−1 . The possible origins of the γ -ray emission from HESS J1813-178 are discussed, including SNR G12.820.02, 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 a promising PeVatron. A 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.https://doi.org/10.3847/1538-4357/ad2ae1Gamma-ray sourcesSupernova remnantsPulsar wind nebulaeStar clustersMolecular clouds |
| spellingShingle | Xiaolei Guo Yuliang Xin Revision of the GeV γ-Ray Emission in the Region of HESS J1813-178 with Fermi-LAT The Astrophysical Journal Gamma-ray sources Supernova remnants Pulsar wind nebulae Star clusters Molecular clouds |
| title | Revision of the GeV γ-Ray Emission in the Region of HESS J1813-178 with Fermi-LAT |
| title_full | Revision of the GeV γ-Ray Emission in the Region of HESS J1813-178 with Fermi-LAT |
| title_fullStr | Revision of the GeV γ-Ray Emission in the Region of HESS J1813-178 with Fermi-LAT |
| title_full_unstemmed | Revision of the GeV γ-Ray Emission in the Region of HESS J1813-178 with Fermi-LAT |
| title_short | Revision of the GeV γ-Ray Emission in the Region of HESS J1813-178 with Fermi-LAT |
| title_sort | revision of the gev γ ray emission in the region of hess j1813 178 with fermi lat |
| topic | Gamma-ray sources Supernova remnants Pulsar wind nebulae Star clusters Molecular clouds |
| url | https://doi.org/10.3847/1538-4357/ad2ae1 |
| work_keys_str_mv | AT xiaoleiguo revisionofthegevgrayemissionintheregionofhessj1813178withfermilat AT yuliangxin revisionofthegevgrayemissionintheregionofhessj1813178withfermilat |