Performance of LHAASO-WCDA and observation of the Crab Nebula as a standard candle *

作者：F. Aharonian, Q. An, 克古 Axikegu, Lixin Bai, Y. X. Bai, Yiwang Bao, D. Bastieri, Xiao-Jun Bi, Yu Bi, H. Cai, J. T. Cai, Z. Cao, Z. Cao, J. F. Chang, J. F. Chang, X. Chang, Bing Chen, J. Chen, Lei Chen, Lei Chen, Lei Chen, M.J. Chen, M.L. Chen, Qianyu Chen, S.H. Chen, S. Z. Chen, T. L. Chen, X.L. Chen, Y. Chen, N. Cheng, Y. D. Cheng, S. W. Cui, Xiaohong Cui, Y.D. Cui, BZ Dai, H. L. Dai, Zi-Gao Dai, 罗布 Danzengluobu, D. della Volpe, B. D′Ettorre Piazzoli, X. J. Dong, J. H. Fan, Y. Fan, Zhiguo Fan, J. Fang, Kai Fang, C. Feng, Li Feng, S.H. Feng, Yulong Feng, B. S. Gao, Chuyue Gao, Qing Gao, Wei Gao, M. M. Ge, Li‐Sheng Geng, G. Gong, Q. B. Gou, M. H. Gu, J. Guo, Xueling Guo, Yanjun Guo, Y. Y. Guo, Yunping Han, H. H. He, H. N. He, Jiale He, S. L. He, Xinyu He, Y. He, M. Heller, Y. K. Hor, C. Hou, Xianglin Hou, Haibing Hu, S. Hu, S. Hu, Xintian Hu, D.H. Huang, Q. Huang, Wenhao Huang, X. T. Huang, Zhongjie Huang, Feng Ji, X. L. Ji, H. Y. Jia, K. Jiang, Zhijie Jiang, Changqing Jin, D. Kuleshov, K. Levochkin, Bo Li, Cong Li, Cong Li, F. Li, H.B. Li, H.C. Li, H.Y. Li, J. Li, K. Li, W.L. Li, X. Li, Xin R Li, X.R. Li, Yujie Li, Y.Z. Li, Zhi Li, Zhenwang Li, En‐Wei Liang, Liang Yu, S. J. Lin, B. Liu, Chao Liu, D. Liu, H. Liu, H.D. Liu, Jing Liu, Junnan Liu, J.S. Liu, J.Y. Liu, M.Y. Liu, R.Y. Liu, Siming Liu, Weiwei Liu, Yongqi Liu, Z.X. Liu, W. J. Long, R. Lu, H. K. Lv, Bin Ma, Lingling Ma, Xinhua Ma, J. R. Mao, A. Masood, W. Mitthumsiri, T. Montaruli, Y. C. Nan, B. Y. Pang, P. Pattarakijwanich, Z. Y. Pei, M. Qi, Bing-Qiang Qiao, D. Ruffolo, V. Rulev, A. Sáiz, L. Shao, O. Shchegolev, X. D. Sheng, Jianrong Shi, H. C. Song, Yu. V. Stenkin, V. Stepanov, Q. N. Sun, X. N. Sun, Z. B. Sun, P. H. T. Tam, Z. Tang, W.W. Tian, B. D. Wang, C. Wang, H. Wang, H.G. Wang, Jincheng Wang, J. Wang, L.P. Wang, L.Y. Wang, R.N. Wang, W. Wang, W. Wang, Xiang-Gao Wang, Xianwen Wang, X.Y. Wang, Y.D Wang, Yuejun Wang, Ying‐Ping Wang, Z. Wang, Z. Wang, Z.H. Wang, Z.X. Wang, D. M. Wei, Jinjia Wei, Yujie Wei, T. Wen, C. Y. Wu, H. R. Wu, S. Wu, W. X. Wu, Xue-Feng Wu, Shichuan Xi, Jun‐Qing Xia, J. Xia, G. M. Xiang, Guoqing Xiao, H. Xiao, G. G. Xin, Y. Xin, Y. Xing, D. L. Xu, R. X. Xu, L. Xue, D. Yan, C. W. Yang, Fang Yang, Junyou Yang, Lili Yang, Mingjie Yang, Ruizhi Yang, S. B. Yang, Yuhua Yao, Z. G. Yao, Y.M. Ye, L. Q. Yin, N. Yin, X. H. You, Z. Y. You, Yi Yu, Q. Yuan, Houdun Zeng, T. X. Zeng, W. Zeng, Z.K. Zeng, M. Zha, X. X. Zhai, Bin‐Bin Zhang, H.M. Zhang, H.Y. Zhang, J.L. Zhang, J.W. Zhang, L. Zhang, L. Zhang, L.X. Zhang, P.F. Zhang, P.P. Zhang, Ruoyu Zhang, S.R. Zhang, Shoushan Zhang, Xiao Zhang, X. P. Zhang, Y. Zhang, Y. Zhang, Y.F. Zhang, Y.L. Zhang, Bowen Zhao, Jianling Zhao, Linlin Zhao, L.Z. Zhao, S. P. Zhao, Fa‐Kun Zheng, Y. G. Zheng, Bo Zhou, Hong‐Cai Zhou, Jingzhi Zhou, P. Zhou, Ruijie Zhou, X. X. Zhou, C. G. Zhu, F. R. Zhu, Haifeng Zhu, K. J. Zhu, X. Zuo · 发表于：Chinese Physics C · 年份：2021 · DOI：10.1088/1674-1137/ac041b · 被引用次数：66 · 研究领域：Astrophysics and Cosmic Phenomena、Gamma-ray bursts and supernovae、Geophysics and Gravity Measurements

Abstract The first Water Cherenkov detector of the LHAASO experiment (WCDA-1) has been operating since April 2019. The data for the first year have been analyzed to test its performance by observing the Crab Nebula as a standard candle. The WCDA-1 achieves a sensitivity of 65 mCU per year, with a statistical threshold of 5 . To accomplish this, a 97.7% cosmic-ray background rejection rate around 1 TeV and 99.8% around 6 TeV with an approximate photon acceptance of 50% is achieved after applying an algorithm to separate gamma-induced showers. The angular resolution is measured using the Crab Nebula as a point source to be approximately 0.45° at 1 TeV and better than 0.2° above 6 TeV, with a pointing accuracy better than 0.05°. These values all match the design specifications. The energy resolution is found to be 33% for gamma rays around 6 TeV. The spectral energy distribution of the Crab Nebula in the range from 500 GeV to 15.8 TeV is measured and found to be in agreement with the results from other TeV gamma ray observatories.