4FGL J1844.4–0306: High-energy Emission Likely from the Supernova Remnant G29.37 + 0.1
Very-high-energy (VHE) observations have revealed approximately 100 TeV sources in our Galaxy, and a significant fraction of them are under investigation to understand their origin. We report our study of one of them, HESS J1844−030. It is found to be possibly associated with the supernova remnant (...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ace10b |
| _version_ | 1797695251496828928 |
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| author | Dong Zheng Zhongxiang Wang Xiao Zhang Yang Chen Yi Xing |
| author_facet | Dong Zheng Zhongxiang Wang Xiao Zhang Yang Chen Yi Xing |
| author_sort | Dong Zheng |
| collection | DOAJ |
| description | Very-high-energy (VHE) observations have revealed approximately 100 TeV sources in our Galaxy, and a significant fraction of them are under investigation to understand their origin. We report our study of one of them, HESS J1844−030. It is found to be possibly associated with the supernova remnant (SNR) candidate G29.37 + 0.1, and detailed studies of the source region at radio and X-ray frequencies have suggested that this SNR is a composite one, containing a pulsar wind nebula (PWN) powered by a candidate young pulsar. As the GeV source 4FGL J1844.4−0306 is also located in the region with high positional coincidence, we analyze its γ -ray data obtained with the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. We determine the GeV γ -ray emission is extended, described with a log-parabola function. The obtained spectrum can be connected to that of the VHE source HESS J1844−030. Given these properties and those from multifrequency studies, we discuss the origin of the γ -ray emission by considering that the two γ -ray sources are associated. Our modeling indicates that while the TeV part would have either a hadronic (from the SNR) or a leptonic origin (from the putative PWN), the GeV part would arise from a hadronic process. Thus we conclude that 4FGL J1844.4−0306 is likely the GeV counterpart to G29.37 + 0.1. |
| first_indexed | 2024-03-12T03:09:40Z |
| format | Article |
| id | doaj.art-d9a35b852e4f45129092b62eced6ce4f |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T03:09:40Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-d9a35b852e4f45129092b62eced6ce4f2023-09-03T14:29:08ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01952215810.3847/1538-4357/ace10b4FGL J1844.4–0306: High-energy Emission Likely from the Supernova Remnant G29.37 + 0.1Dong Zheng0Zhongxiang Wang1https://orcid.org/0000-0003-1984-3852Xiao Zhang2https://orcid.org/0000-0002-9392-547XYang Chen3https://orcid.org/0000-0002-4753-2798Yi Xing4https://orcid.org/0000-0002-5818-0732Department of Astronomy, School of Physics and Astronomy, Yunnan University , Kunming 650091, People's Republic of China ; wangzx20@ynu.edu.cnDepartment of Astronomy, School of Physics and Astronomy, Yunnan University , Kunming 650091, People's Republic of China ; wangzx20@ynu.edu.cn; Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People's Republic of China ; xiaozhang@nju.edu.cnSchool of Astronomy & Space Science, Nanjing University , 163 Xinlin Avenue, Nanjing 210023, People's Republic of China; Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University , Ministry of Education, People's Republic of ChinaSchool of Astronomy & Space Science, Nanjing University , 163 Xinlin Avenue, Nanjing 210023, People's Republic of China; Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University , Ministry of Education, People's Republic of ChinaShanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People's Republic of China ; xiaozhang@nju.edu.cnVery-high-energy (VHE) observations have revealed approximately 100 TeV sources in our Galaxy, and a significant fraction of them are under investigation to understand their origin. We report our study of one of them, HESS J1844−030. It is found to be possibly associated with the supernova remnant (SNR) candidate G29.37 + 0.1, and detailed studies of the source region at radio and X-ray frequencies have suggested that this SNR is a composite one, containing a pulsar wind nebula (PWN) powered by a candidate young pulsar. As the GeV source 4FGL J1844.4−0306 is also located in the region with high positional coincidence, we analyze its γ -ray data obtained with the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. We determine the GeV γ -ray emission is extended, described with a log-parabola function. The obtained spectrum can be connected to that of the VHE source HESS J1844−030. Given these properties and those from multifrequency studies, we discuss the origin of the γ -ray emission by considering that the two γ -ray sources are associated. Our modeling indicates that while the TeV part would have either a hadronic (from the SNR) or a leptonic origin (from the putative PWN), the GeV part would arise from a hadronic process. Thus we conclude that 4FGL J1844.4−0306 is likely the GeV counterpart to G29.37 + 0.1.https://doi.org/10.3847/1538-4357/ace10bSupernova remnantsPulsar wind nebulaeGamma-ray sources |
| spellingShingle | Dong Zheng Zhongxiang Wang Xiao Zhang Yang Chen Yi Xing 4FGL J1844.4–0306: High-energy Emission Likely from the Supernova Remnant G29.37 + 0.1 The Astrophysical Journal Supernova remnants Pulsar wind nebulae Gamma-ray sources |
| title | 4FGL J1844.4–0306: High-energy Emission Likely from the Supernova Remnant G29.37 + 0.1 |
| title_full | 4FGL J1844.4–0306: High-energy Emission Likely from the Supernova Remnant G29.37 + 0.1 |
| title_fullStr | 4FGL J1844.4–0306: High-energy Emission Likely from the Supernova Remnant G29.37 + 0.1 |
| title_full_unstemmed | 4FGL J1844.4–0306: High-energy Emission Likely from the Supernova Remnant G29.37 + 0.1 |
| title_short | 4FGL J1844.4–0306: High-energy Emission Likely from the Supernova Remnant G29.37 + 0.1 |
| title_sort | 4fgl j1844 4 0306 high energy emission likely from the supernova remnant g29 37 0 1 |
| topic | Supernova remnants Pulsar wind nebulae Gamma-ray sources |
| url | https://doi.org/10.3847/1538-4357/ace10b |
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