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arXiv · 2306.12134

4FGL J1844.4-0306: high-energy emission likely from the supernova remnant G29.37+0.1

D. Zheng·Z. Wang·X. Zhang·Y. Chen·Y. Xing
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Abstract

Very-high-energy (VHE) observations have revealed approximately 100 TeV sources in our Galaxy, and a significant fraction of them are under investigation for understanding their origin. We report our study of one of them, HESS~J1844$-$030. It is found possibly associated with the supernova remnant (SNR) candidate G29.37+0.1, and detailed studies of the source region at radio and X-ray frequencies have suggested that this SNR is a composite one, containing a pulsar wind nebula (PWN) powered by a candidate young pulsar. As the GeV source 4FGL~J1844.4$-$0306 is also located in the region with high positional coincidence, we analyze its $\gamma$-ray data obtained with the Large Area Telescope on-board the {\it Fermi Gamma-ray Space Telescope }. We determine the GeV $\gamma$-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 the properties and those from multi-frequency studies, we discuss the origin of the $\gamma$-ray emission by considering that the two \gr\ 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 the likely GeV counterpart to G29.37+0.1.

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D. Zheng, Z. Wang, X. Zhang, Y. Chen, Y. Xing. 2023-06-21. 4FGL J1844.4-0306: high-energy emission likely from the supernova remnant G29.37+0.1. https://doi.org/10.3847/1538-4357%2Face10b

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