Does or Did the Supernova Remnant Cassiopeia A Operate as a PeVatron?

作者：Z. Cao, F. Aharonian, Q. An, Axikegu, Y.X Bai, Yiwang Bao, D. Bastieri, Xiao-Jun Bi, Y.J Bi, J. T. Cai, Qing Cao, W.Y Cao, Zhe Cao, J. Chang, J. F. Chang, A.M Chen, E. S. Chen, Liang Chen, Lin Chen, Long Chen, M.J Chen, M.L Chen, Qin Chen, Shaw H. Chen, S. Z. Chen, T. L. Chen, Yang Chen, Ning Cheng, Y.D Cheng, Maxwell Cui, S. W. Cui, X.H Cui, Y. D. Cui, B. Z. Dai, H. L. Dai, Z. G. Dai, Danzengluobu Danzengluobu, D. della Volpe, X.Q Dong, K. K. Duan, Junhui Fan, Yi-Zhong Fan, Jun Fang, Kun Fang, C.F Feng, Li Feng, S. H. Feng, X.T Feng, Yulong Feng, S. Gabici, Bo Gao, Chuyue Gao, L. Q. Gao, Qi Gao, Wei Gao, Wei Gao, M.M Ge, Li‐Sheng Geng, Gwenael Giacinti, G. Gong, Q. B. Gou, M. H. Gu, Fulai Guo, Xu Guo, Yi-Qing Guo, Yong Guo, Y.A Han, H.H He, Hongbin He, Jiangbiao He, Xiao-Rong He, Y. He, Matthieu Heller, Y. K. Hor, Bowen Hou, C. Hou, X. T. Hou, H.B Hu, Qiang Hu, S. C. Hu, D.H Huang, T.Q Huang, Weidong Huang, X. T. Huang, X.Y Huang, Yumin Huang, Zhongjie Huang, X. L. Ji, H.Y Jia, Ke Jia, K. Jiang, Xiaojun Jiang, Z.J Jiang, Mingzhou Jin, M. M. Kang, T. Ke, D. Kuleshov, K. Kurinov, Bing Li, Cheng Li, Cong Li, Di Li, Li Fei, Haibo Li, H.C Li, H.Y Li, J. Li, Jian Li, Jie Li, Keran Li, W.L Li, W.L Li, X.R Li, Xin Li, Yang Li, Zhe Li, Zhuo Li, E.W Liang, Yun-Feng Liang, S.J Lin, B. Liu, Cuiping Liu, Dawei Liu, Haichao Liu, H.D Liu, J. Liu, J.L Liu, Jinxiang Liu, Mingyi Liu, Rui Liu, S.M Liu, W. Liu, Yi Liu, Yu‐Rong Liu, R. Lu, Q. Luo, H.K Lv, B.Q Ma, L.L. Ma, Xinhua Ma, J. R. Mao, Z. Min, W. Mitthumsiri, Haowei Mu, Y. C. Nan, A. Neronov, Z. W. Ou, B. Y. Pang, P. Pattarakijwanich, Z. Y. Pei, Ming Qi, Yuning Qi, Bing-Qiang Qiao, J. J. Qin, D. Ruffolo, A. Sáiz, D. Semikoz, Changhui Shao, L. Shao, O. Shchegolev, X. D. Sheng, Fengchun Shu, H. C. Song, Yu.V Stenkin, V. Stepanov, Yang Su, Q. N. Sun, X.N Sun, Zhifeng Sun, P. H. T. Tam, Q.W Tang, Z.B Tang, W. W. Tian, C. Wang, C.B Wang, G.W Wang, Hui Wang, H.H Wang, J. Wang, K Wang, L.P Wang, L.Y Wang, Ping Wang, R. Wang, Wei Wang, X.G Wang, X.Y Wang, Ying Wang, Y.D Wang, Y.J Wang, Z.H Wang, Z.X Wang, Zhen Wang, Zheng Wang, D. M. Wei, Jinjia Wei, Y. Wei, Tao Wen, Chen Wu, H. R. Wu, Sha Sha Wu, X.F Wu, Yong Wu, Shichuan Xi, J. Xia, Junji Xia, G. M. Xiang, Dong Xiao, G. Xiao, G. G. Xin, Y. Xin, Y. Xing, Z. Xiong, D.L Xu, Ruo-Jun Xu, Run Xu, W. L. Xu, L. Xue, D.H Yan, Jing‐Zhi Yan, Tong Yan, Chul Woo Yang, Fang Yang, F.F Yang, H. W. Yang, Junyou Yang, Lili Yang, Mo Yang, Ruizhi Yang, S. B. Yang, Y. Yao, Z. G. Yao, Y. M. Ye, Lina Yin, N. Yin, X. H. You, Z. Y. You, Yi Yu, Qiang Yuan, Han Yue, Houdun Zeng, T. X. Zeng, W. Zeng, M. Zha, Bin‐Bin Zhang, Fan Zhang, H.M Zhang, Hengyun Zhang, J.L Zhang, L.X Zhang, Li Zhang, Peng Zhang, P. Zhang, Rui Zhang, Shengbai Zhang, S.R Zhang, S.S Zhang, Xiong Zhang, X.P Zhang, Y.F Zhang, Yi Zhang, Yong Zhang, Bing Zhao, J. Y. Zhao, Lei Zhao, Lei Zhao, Shujie Zhao, F. Zheng, B. Zhou, H. Zhou, Jianhui Zhou, Meng Zhou, Ping Zhou, Rong Zhou, Xiaoxin Zhou, C. G. Zhu, F.R Zhu, H. Zhu, K. J. Zhu, X. Zuo · 发表于：The Astrophysical Journal Letters · 年份：2024 · DOI：10.3847/2041-8213/ad1d62 · 被引用次数：10 · 研究领域：Astrophysics and Cosmic Phenomena、Gamma-ray bursts and supernovae、Neutrino Physics Research

Abstract For decades, supernova remnants (SNRs) have been considered the prime sources of Galactic cosmic rays (CRs). But whether SNRs can accelerate CR protons to PeV energies and thus dominate CR flux up to the knee is currently under intensive theoretical and phenomenological debate. The direct test of the ability of SNRs to operate as CR PeVatrons can be provided by ultrahigh-energy (UHE; E γ ≥ 100 TeV) γ -rays. In this context, the historical SNR Cassiopeia A (Cas A) is considered one of the most promising targets for UHE observations. This paper presents the observation of Cas A and its vicinity by the LHAASO KM2A detector. The exceptional sensitivity of LHAASO KM2A in the UHE band, combined with the young age of Cas A, enabled us to derive stringent model-independent limits on the energy budget of UHE protons and nuclei accelerated by Cas A at any epoch after the explosion. The results challenge the prevailing paradigm that Cas A–type SNRs are major suppliers of PeV CRs in the Milky Way.