Accès ouvert déclaré
2025
article
Broadband γ-Ray Spectrum of Supernova Remnant Cassiopeia A
Z. Cao, F Aharonian, Y. Bai, Y. W. Bao, D. Bastieri, Xiao-Jun Bi, Y.J Bi, Weixin Bian, A.V Bukevich, Chufan Cai, Wenjing Cao, Zhe Cao, J. Chang, J. F. Chang, A. M. Chen, E. S. Chen, H. X. Chen, Liang Chen, Long Chen, M.J. Chen, M. L. Chen, Qingze Chen, S. Chen, Shaw H. Chen, S.Z. Chen, T. L. Chen, Xiang‐Bai Chen, X. J. Chen, Ye Chen, Ning Cheng, Y. D. Cheng, M. C. Chu, Maxwell Cui, S. W. Cui, X. H. Cui, B. Z. Dai, H. L. Dai, Z. G. Dai, Danzengluobu, Yingxue Diao, X.Q Dong, K. K. Duan, Junhui Fan, Y. Z. Fan, Jun Fang, J. H. Fang, Kun Fang, Chunsheng Feng, Haoran Feng, Li Feng, X.T Feng, Yuliang Feng, Y. L. Feng, S. Gabici, Bo Gao, Chuyue Gao, Qi Gao, Wei Gao, M.M Ge, Tingting Ge, Li‐Sheng Geng, Gwenael Giacinti, G.H Gong, Q. B. Gou, M. H. Gu, Fu-Ming Guo, J. Guo, Xu Guo, Y. Q. Guo, Yong Guo, Yunping Han, O. A. Hannuksela, M. Zahid Hasan, H.H He, Hongbin He, Jiangbiao He, Xiaoying He, Y. He, S. Hern ndez-Cadena, Y. K. Hor, Bowen Hou, Chao Hou, Xingsong Hou, H.B Hu, S. C. Hu, Chun-Hao P. Huang, D.H Huang, J. J. Huang, T. Q. Huang, Weidong Huang, X. T. Huang, X. Y. Huang, Yumin Huang, Y. Huang, Xiangdong Ji, HY Jia, Ke Jia, H. B. Jiang, K. Jiang, X. W. Jiang, Zhuo Jiang, Mingzhou Jin, Samy Kaci, M.M Kang, I. Karpikov, D. Khangulyan, D. Kuleshov, K. Kurinov, Bing Li, Cheng Li, Cong Li, Di Li, Fan Li, Haibo Li, Huicai Li, Jiandong Li, Jie Li, K. Li, Lu Li, R. L. Li, S. D. Li, Tianyu Li, W.L Li, X.R Li, Xin Li, Yang Li, Zhe Li, Zhuo Li, E.W Liang, Y. F. Liang, S.J Lin, B. Liu, C. Liu, D. Liu, D. B. Liu, Haichao Liu, H. D. Liu, J. Liu, J. L. Liu, Jiaren Liu, Manfei Liu, Ruo-Yu Liu, Siming Liu, W. Liu, Xin Liu, Yu‐Rong Liu, Y. N. Liu, Y.‐Q. Lou, Q. Luo, Yangping Luo, H.K Lv, B.Q Ma, L.L. Ma, X. H., J. R. Mao, W. Mitthumsiri, Guobin Mou, Haowei Mu, Y. C. Nan, A. Neronov, Kenny C. Y. Ng, Michael Y. Ni, L. S. Nie, Lijun Ou, P. Pattarakijwanich, Zhichao Pei, Jinfeng Qi, Ming Qi, J. J. Qin, Ali Raza, Chunying Ren, D. Ruffolo, A. Sáiz, M. A. Saeed, D. Semikoz, L. Shao, O. Shchegolev, Y. Z. Shen, X. D. Sheng, Fengchun Shu, H. C. Song, Yu.V Stenkin, V. Stepanov, Yang Su, Danfeng Sun, H. Sun, Q. N. Sun, X.N Sun, Zhaoyong Sun, N.H Tabasam, J. Takata, P. H. T. Tam, Hongbing Tan, Q.W Tang, Rujun Tang, Z. Tang, Tian Wu, Cunzhu Tong, L. H. Wan, C. Wang, G. W. Wang, Hui Wang, H.H Wang, Jianyuan Wang, K. Wang, Kai Wang, L. P. Wang, L. Y. Wang, R. Wang, Wei Wang, X. G. Wang, Xingjun Wang, X.Y Wang, Ying Wang, Y.D Wang, Z.H. Wang, Z. X. Wang, Zheng Wang, D. M. Wei, Jinjia Wei, Y. Wei, Tao Wen, Shanshan Weng, CY Wu, H. R. Wu, Q. W. Wu, Sha Sha Wu, X.F Wu, Yong Wu, Shichuan Xi, Jun Xia, Jingbo Xia, G. M. Xiang, D. X. Xiao, G. Xiao, Y. L. Xin, Y. Xing, D. R. Xiong, D.L Xu, Ruo-Jun Xu, Run Xu, W. L. Xu, L. Xue, D.H Yan, Jing‐Zhi Yan, Tong Yan, Chengfeng Yang, Cheng Yang, F.F Yang, Liuan Yang, Mingjie Yang, Rui Yang, Wen‐Xing Yang, Y. Yao, Z. G. Yao, Xinchen Ye, Lina Yin, N Yin, X. H. You, Zhanping You, Yi Yu, Qiong Yuan, Han Yue, Hui‐Yi Zeng, Tingxuan Zeng, W. Zeng, M. Zha, Bin‐Bin Zhang, B. T. Zhang, Fan Zhang, Hengyun Zhang, H. M. Zhang, H. Y. Zhang, J. L. Zhang, Li Zhang, P. F. Zhang, P. P. Zhang, Rui Zhang, S. R. Zhang, S. S. Zhang, W. Y. Zhang, Xiao Zhang, X. P. Zhang, Yi Zhang, Yong Zhang, Z. P. Zhang, J. Y. Zhao, Lei Zhao, Linlin Zhao, S. P. Zhao, X. Zhao, Z. H. Zhao, F. Zheng, W. J. Zhong, B. Zhou, H. Zhou, Jianhui Zhou, Menglei Zhou, Ping Zhou, Rong Zhou, Xu Zhou, Baohua Zhu, C. G. Zhu, F. R. Zhu, H. Zhu, K. J. Zhu, Y. C. Zou, X. Zuo
10Citations signalées — pas une note de qualité
0Institutions déclarées
0Pays d’affiliation déclarés
Résumé fourni par la source
Abstract The core-collapse supernova remnant (SNR) Cassiopeia A (Cas A) is one of the brightest galactic radio sources with an angular radius of ∼ 2 . ′ 5 . Although no extension of this source has been detected in the γ-ray band, using more than 1000 days of LHAASO data above ∼0.8 TeV, we find that its spectrum is significantly softer than those obtained with Imaging Air Cherenkov Telescopes (IACTs), and its flux near ∼1 TeV is about 2 times higher. In combination with analyses of more than 16 yr of Fermi-LAT data covering 0.1 GeV–1 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 ± 0.15stat (3.41 ± 0.19stat) below (above) a break energy of 0.63 ± 0.21stat 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 modeling can be used to constrain the acceleration processes of TeV particles in the early stage of SNR evolution.
Ce résumé expose les affirmations des auteurs. BNTIC ne l’interprète pas comme une validation indépendante des résultats.
Contrôle bibliographique ouvert
DOI retrouvé dans Crossref DOI retrouvé, mais le titre doit être comparé manuellement.
- Titre Crossref
- Broadband <i>γ</i>-Ray Spectrum of Supernova Remnant Cassiopeia A
- Date Crossref
- 20/03/2025
- 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.
Sujets associés
Astrophysics and Cosmic PhenomenaGamma-ray bursts and supernovaeRadio Astronomy Observations and Technology