Broadband <i>γ</i>-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, Y. D. 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, S. H. Feng, X.T Feng, Yuliang Feng, Y. L. Feng, S. Gabici, Bo Gao, Chuyue Gao, Qi Gao, Wei 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
Abstract
Abstract The core-collapse supernova remnant (SNR) Cassiopeia A (Cas A) is one of the brightest galactic radio sources with an angular radius of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>∼</mml:mo> <mml:mn>2</mml:mn> <mml:mover accent="true"> <mml:mrow> <mml:mi>.</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>′</mml:mi> </mml:mrow> </mml:mover> <mml:mn>5</mml:mn> </mml:math> . 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 ± 0.15 stat (3.41 ± 0.19 stat ) below (above) a break energy of 0.63 ± 0.21 stat 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.