Accès ouvert déclaré
2025
article
An Enigmatic PeVatron in an Area around H ii Region G35.6−0.5
Z. Cao, F Aharonian, Axikegu, Yuting Bai, Yiwang Bao, D. Bastieri, Xiao-Jun Bi, Y.J Bi, W Bian, A.V Bukevich, Qin Cao, Weiling Cao, Zhe Cao, J. F. Chang, A.M Chen, Bingqiu Chen, E.S Chen, Hua-Xing Chen, Liang Chen, Lin Chen, Long Chen, M.J Chen, M.L Chen, Qin Chen, Shengyong Chen, Shaw H. Chen, S. Z. Chen, T. L. Chen, Yang Chen, Na Cheng, Y.D Cheng, Micheline C. Chu, Maxwell Cui, S. W. Cui, X.H Cui, Y. D. Cui, B. Z. Dai, Zi-Gao Dai, Danzengluobu Danzengluobu, X.Q Dong, K. K. Duan, Junhui Fan, Yi-Zhong Fan, Fang Ji, J. Fang, Kun Fang, C. Feng, Hua Feng, L. Feng, Shuo Feng, X.T Feng, Y. Feng, Y. L. Feng, S. Gabici, Bo Gao, C. D. Gao, Q. Gao, Wei Gao, M. M. Ge, T.T Ge, Li‐Sheng Geng, Gwenael Giacinti, G. Gong, Q. B. Gou, M. H. Gu, Fulai Guo, Jia Guo, Xu Guo, Y. Q. Guo, Yong Guo, Y. A. Han, O. A. Hannuksela, M Hasan, H. H. He, H. N. He, Jiangbiao He, Y. He, Y. K. Hor, Bowen Hou, Changbo Hou, X. T. Hou, H. B. Hu, Q. Hu, S. C. Hu, C. Huang, D.H Huang, T.Q Huang, Weidong Huang, X. T. Huang, X.Y Huang, Yongbo Huang, Yanyi Huang, X. L. Ji, H.Y Jia, Ke Jia, Hongbing Jiang, K. Jiang, Xiaojun Jiang, Z.J Jiang, Min Jin, M. M. Kang, I. Karpikov, D. Khangulyan, D. Kuleshov, K. Kurinov, Bing Li, C.M Li, Cheng Li, Cong Li, Duo Li, Li Fei, Haibo Li, Hancheng Li, Jian Li, Jie Li, Kai Li, Shaoquan Li, W.L Li, X.R. Li, Xin Li, Yuze Li, Zhe Li, Zhuo Li, En‐Wei Liang, Yun-Feng Liang, S.J Lin, Yun Liu, C Liu, Dantong Liu, D. Liu, Haiqing Liu, H.D Liu, Jie Liu, J.L Liu, M. Liu, Rui Liu, S.M Liu, Y. Liu, Yu‐Rong Liu, Quantian Luo, Yi Luo, H.K Lv, B.Q Ma, L.L Ma, Xinhua Ma, J. R. Mao, W. Mitthumsiri, Haowei Mu, Y. C. Nan, A. Neronov, K.C.Y Ng, L.J Ou, P. Pattarakijwanich, Z. Y. Pei, J.C Qi, Ming Qi, Bing-Qiang Qiao, J. J. Qin, Ahmed Raza, D. Ruffolo, A. Sáiz, M. A. Saeed, D. Semikoz, Lu Shao, O. Shchegolev, X.D Sheng, Fengchun Shu, H. C. Song, Yu.V Stenkin, V. I. Stepanov, Yanjing Su, D.X Sun, Q. N. Sun, X.N Sun, Zhifeng Sun, J. Takata, P. H. T. Tam, Q.W Tang, Ryan W. Tang, Z.B Tang, W. W. Tian, L.H Wan, C. Wang, C.B Wang, G.W Wang, Haigang Wang, H.H Wang, Jincheng Wang, Kai Wang, L.P Wang, L.Y Wang, Ping Wang, Ruikang K. Wang, Weiyang Wang, X.G. Wang, Xuefeng Wang, Yi Wang, Y.D Wang, Yun-Jiang Wang, Z.H. Wang, Z.X Wang, Zhen Wang, Z. Wang, D. M. Wei, Jun-Jie Wei, Yujie Wei, T. Wen, Chen Wu, H. R. Wu, Qi Wu, Sheng Wu, X.F Wu, Yong Wu, Shao-Qiang Xi, Jing Xia, G. M. Xiang, D. X. Xiao, G. Xiao, Y. Xin, Yi Xing, D.R Xiong, D.L Xu, R.F Xu, Rui Xu, Weiwei Xu, L. Xue, D.H Yan, Jing‐Zhi Yan, Ting Yan, Chul Woo Yang, C. Y. Yang, Fan Yang, Fang Yang, Lili Yang, Mo Yang, Ruizhi Yang, W.X Yang, Y. Yao, Z. G. Yao, L. Q. Yin, N. Yin, X. H. You, Z. Y. You, Yi Yu, Hui Yue, Houdun Zeng, T. X. Zeng, Wen Zeng, M. Zha, Bin‐Bin Zhang, Fengming Zhang, Hua Zhang, H.M Zhang, Hengyun Zhang, J.L Zhang, Li Zhang, Peng Zhang, P.P Zhang, Rui Zhang, Shengbai Zhang, S.R Zhang, S.S Zhang, Xiao Zhang, X.P Zhang, Y.F Zhang, Yi Zhang, Yong Zhang, Bo Zhao, J. Zhao, Lei Zhao, S. P. Zhao, Xinsheng Zhao, F. Zheng, Bo Zhou, H. Zhou, J. N. Zhou, Mingfei Zhou, Ping Zhou, Ruijie Zhou, X. X. Zhou, Baohua Zhu, C. G. Zhu, F. R. Zhu, Hao Zhu, Kejun Zhu, Yuan-Chuan Zou, X. Zuo
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Résumé fourni par la source
Abstract Identifying Galactic PeVatrons (PeV particle accelerators) from ultrahigh-energy (UHE, >100 TeV) γ-ray sources plays a crucial role in revealing the origin of Galactic cosmic rays. The UHE source 1LHAASO J1857+0203u is suggested to be associated with HESS J1858+020, which may be attributed to the possible PeVatron candidate supernova remnant (SNR) G35.6−0.4 or H ii region G35.6−0.5. We perform detailed analysis on the very-high-energy and UHE γ-ray emissions toward this region with data from the Large High Altitude Air Shower Observatory (LHAASO). 1LHAASO J1857+0203u is detected with a significance of 11.6σ above 100 TeV, indicating the presence of a PeVatron. It has an extent of ∼0 . ° 18 with a power-law (PL) spectral index of ∼2.5 at 1–25 TeV and pointlike emission with a PL spectral index of ∼3.2 above 25 TeV. Using archival CO and H i data, we identify some molecular and atomic clouds that may be associated with the TeV γ-ray emissions. Our modeling indicates that the TeV γ-ray emissions are unlikely to arise from clouds illuminated by the protons that escaped from SNR G35.6−0.4. In the scenario in which H ii region G35.6−0.5 could accelerate particles to the UHE band, the observed GeV–TeV γ-ray emission could be well explained by a hadronic model with a PL spectral index of ∼2.0 and cutoff energy of ∼450 TeV. However, an origin in an evolved pulsar wind nebula cannot be ruled out.
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Contrôle bibliographique ouvert
DOI retrouvé dans Crossref DOI retrouvé, mais le titre doit être comparé manuellement.
- Titre Crossref
- An Enigmatic PeVatron in an Area around H <scp>ii</scp> Region G35.6−0.5
- Date Crossref
- 17/01/2025
- Éditeur
- American Astronomical Society
- Type
- journal-article
Ce recoupement confirme des métadonnées liées au DOI. Il ne confirme ni la méthode ni les conclusions de l’étude et ne compte pas comme une seconde source scientifique indépendante.
Institutions déclarées
Une affiliation ne permet pas de déduire la nationalité d’un auteur.
Sujets associés
Astrophysics and Cosmic PhenomenaGamma-ray bursts and supernovaeNeutrino Physics Research