Accès ouvert déclaré
2025
preprint
Broadband $γ$-ray spectrum of supernova remnant Cassiopeia A
Z. Cao, F. Aharonian, Y.X Bai, Yiwang Bao, D. Bastieri, Xiao-Jun Bi, Y. J. Bi, W. H. Bian, A.V Bukevich, Chufan Cai, W.Y Cao, Zhe Cao, J. Chang, J. F. Chang, A. M. Chen, E. S. Chen, Hua-Xing Chen, Liang Chen, Long Chen, M.J Chen, M. L. Chen, Qin Chen, S. Chen, Shaw H. Chen, S.Z. Chen, T. L. Chen, Xiang‐Bai Chen, Y Chen, N. Cheng, Y.D Cheng, M. C. Chu, Maxwell Cui, S. W. Cui, X.H Cui, B. Z. Dai, Z. G. Dai, Danzengluobu Danzengluobu, Y.X Diao, X. Q. Dong, K. K. Duan, Y. Z. Fan, Jun Fang, J. Fang, Ke Fang, Chunsheng Feng, Hao Feng, Feng Lu, X.T Feng, Yuliang Feng, Y. L. Feng, S. Gabici, Bo Gao, Chuyue Gao, Q. Gao, W. Gao, W. K. Gao, M.M Ge, Tingting Ge, Li‐Sheng Geng, Gwenael Giacinti, G.H Gong, Q. B. Gou, M. H. Gu, Fu-Ming Guo, Jincheng Guo, X. L. Guo, Yi-Qing Guo, Y. Y. Guo, Yunping Han, O. A. Hannuksela, M Hasan, H. H. He, Hongbin He, Jiawei He, Xiaoying He, Yang He, S. Hernández-Cadena, Y. K. Hor, Bowen Hou, C. Hou, Xingsong Hou, H.B Hu, S. C. Hu, Cong Huang, D.H Huang, J. J. Huang, T. Q. Huang, Weidong Huang, X. T. Huang, X.Y Huang, Yi‐Wen Huang, Y. Huang, X. L. Ji, HY Jia, K. Jia, H. B. Jiang, Kuan Jiang, X. W. Jiang, Z. J. Jiang, Ming Jin, S Kaci, M. M. Kang, I. Karpikov, D. Khangulyan, D. Kuleshov, K. Kurinov, Bing Li, Cheng Li, Cong Li, Di Li, Fan Li, H. B. Li, H.C Li, Jiandong Li, Jie Li, Keran Li, Lu Li, R. L. Li, S. D. Li, T.Y Li, Weimin Li, X. R. Li, Xin Li, Y. Z. Li, Zhe Li, Zhuo Li, E.W Liang, Y. F. Liang, S. J. Lin, B. Liu, Cheng Liu, Daizhong Liu, Dong Liu, H. Liu, H.D. Liu, J. Liu, J.L Liu, Jiaren Liu, Mingyi Liu, Ruo-Yu Liu, S.M Liu, Wenzhao Liu, Xiangkun Liu, Yang Liu, Yafei Liu, Y.‐Q. Lou, Q. Luo, Yu Luo, H.K Lv, B.Q Ma, L.L. Ma, Xinhua Ma, J. R. Mao, W. Mitthumsiri, Guobin Mou, Haowei Mu, Y. C. Nan, A. Neronov, K.C.Y Ng, Michael Y. Ni, L. S. Nie, L.J Ou, P. Pattarakijwanich, Zhichao Pei, J.C Qi, M. Qi, Jiajun Qin, Ahmed Raza, Chongyang Ren, D. Ruffolo, A. Sáiz, M. A. Saeed, D. Semikoz, L. Shao, O. Shchegolev, Ya-Ching Shen, X.D Sheng, Fengchun Shu, H. C. Song, Yu.V Stenkin, V. Stepanov, Yi Su, Danfeng Sun, Hui Sun, Q. N. Sun, X.N Sun, Zhifeng Sun, N.H Tabasam, J. Takata, P. H. T. Tam, H. Tan, Q.W Tang, R. C. Tang, Z.B Tang, Tian Wu, Cunzhu Tong, L.H Wan, Cong Wang, G. W. Wang, H.G Wang, H.H Wang, Jianyuan Wang, K. Wang, Kai Wang, L.P Wang, L. Y. Wang, L.Y Wang, Rui Wang, Wei Wang, X.G Wang, Xingjun Wang, X.Y Wang, Y. Wang, Y.D Wang, Z.H Wang, Z. X. Wang, Zheng Wang, D. M. Wei, Jiaju Wei, Yifan Wei, Tao Wen, S.S Weng, C. Y. Wu, H. R. Wu, Qinmu Wu, Yongcheng Wu, X.F Wu, Yuping Wu, S. Q. Xi, J. Xia, Junji Xia, G. M. Xiang, D. X. Xiao, G. Q. Xiao, Y. L. Xin, Y. Xing, D.R Xiong, Z. Xiong, D.L Xu, R.F Xu, R. X. Xu, W. L. Xu, L. Xue, Dahai Yan, J. Z. Yan, T Yan, Chul Woo Yang, Cheng Yang, Fang Yang, Liuan Yang, Mo Yang, Rui Yang, W.X Yang, Yuhua Yao, Z. G. Yao, X.A Ye, L. Q. Yin, N. Yin, X. H. You, Z. Y. You, Y.H. Yu, Qiang Yuan, Han Yue, Hui‐Yi Zeng, T. X. Zeng, W. Zeng, M. Zha, Bin‐Bin Zhang, B. T. Zhang, Fan Zhang, Hongwei Zhang, H.M Zhang, H. Y. Zhang, J. L. Zhang, Li Zhang, Peng Zhang, P.P Zhang, R. Zhang, S.R Zhang, S.S Zhang, W.Y Zhang, Xiong Zhang, X.P Zhang, Yi Zhang, Yong Zhang, Z. P. Zhang, Jie Zhao, Q. Zhao, Linlin Zhao, S. P. Zhao, X. Zhao, Z. H. Zhao, Fan Zheng, W. J. Zhong, Banghao Zhou, H. Zhou, Jianhui Zhou, Mingfei Zhou, Pei Zhou, Rong Zhou, Xu Zhou, Baohua Zhu, C. G. Zhu, F.R Zhu, Hui Zhu, K. J. Zhu, Y. C. Zou, X. Zuo
0Citations signalées, ce qui n’est pas une note de qualité
2Institutions déclarées
2Pays d’affiliation déclarés
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Le résumé fourni par la source
The core-collapse supernova remnant (SNR) Cassiopeia A (Cas A) is one of the brightest galactic radio sources with an angular radius of $\sim$ 2.5 $\arcmin$. Although no extension of this source has been detected in the $γ$-ray band, using more than 1000 days of LHAASO data above $\sim 0.8$ TeV, we find that its spectrum is significantly softer than those obtained with Imaging Air Cherenkov Telescopes (IACTs) and its flux near $\sim 1$ TeV is about two times higher. In combination with analyses of more than 16 years of \textit{Fermi}-LAT data covering $0.1 \, \mathrm{GeV} - 1 \, \mathrm{TeV}$, we find that the spectrum above 30 GeV deviates significantly from a single power-law, and is best described by a smoothly broken power-law with a spectral index of $1.90 \pm 0.15_\mathrm{stat}$ ($3.41 \pm 0.19_\mathrm{stat}$) below (above) a break energy of $0.63 \pm 0.21_\mathrm{stat} \, \mathrm{TeV}$. Given differences in the angular resolution of LHAASO-WCDA and IACTs, TeV $γ$-ray emission detected with LHAASO may have a significant contribution from regions surrounding the SNR illuminated by particles accelerated earlier, which, however, are treated as background by IACTs. Detailed modelling can be used to constrain acceleration processes of TeV particles in the early stage of SNR evolution.
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Les sujets associés
Astrophysics and Cosmic PhenomenaNeutrino Physics ResearchDark Matter and Cosmic Phenomena