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Line-of-shower trigger method to lower energy threshold for GRB detection using LHAASO-WCDA
Aharonian, F.26,27; An, Q.4,5; Axikegu20; Bai, L. X.21; Bai, Y. X.1,3; Bao, Y. W.15; Bastieri, D.10; Bi, X. J.1,2,3; Bi, Y. J.1,3; Cai, H.23; Cai, J. T.10; Cao, Z.1,2,3; Cao, Z.4,5; Chang, J.16; Chang, J. F.1,3,4; Chang, X. C.1,3; Chen, B. M.13; Chen, J.21; Chen, L.1,2,3; Chen, L.18; Chen, L.20; Chen, M. J.1,3; Chen, M. L.1,3,4; Chen, Q. H.20; Chen, S. H.1,2,3; Chen, S. Z.1,3; Chen, T. L.22; Chen, X. L.1,2,3; Chen, Y.15; Cheng, N.1,3; Cheng, Y. D.1,3; Cui, S. W.13; Cui, X. H.7; Cui, Y. D.11; Dai, B. Z.24; Dai, H. L.1,3,4; Dai, Z. G.15; Danzengluobu22; Volpe, D. della31; Piazzoli, B. D’Ettorre28; Dong, X. J.1,3; Fan, J. H.10; Fan, Y. Z.16; Fan, Z. X.1,3; Fang, J.24; Fang, K.1,3; Feng, C. F.17; Feng, L.16; Feng, S. H.1,3; Feng, Y. L.16; Gao, B.1,3; Gao, C. D.17; Gao, Q.22; Gao, W.17; Ge, M. M.24; Geng, L. S.1,3; Gong, G. H.6; Gou, Q. B.1,3; Gu, M. H.1,3,4; Guo, J. G.1,2,3; Guo, X. L.20; Guo, Y. Q.1,3; Guo, Y. Y.1,2,3,16; Han, Y. A.14; He, H. H.1,2,3; He, H. N.16; He, J. C.1,2,3; He, S. L.10; He, X. B.11; He, Y.20; Heller, M.31; Hor, Y. K.11; Hou, C.1,3; Hou X(侯贤)25; Hu, H. B.1,2,3; Hu, S.21; Hu, S. C.1,2,3; Hu, X. J.6; Huang, D. H.20; Huang, Q. L.1,3; Huang, W. H.17; Huang, X. T.17; Huang, Z. C.20; Ji, F.1,3; Ji, X. L.1,3,4; Jia, H. Y.20; Jiang, K.4,5; Jiang, Z. J.24; Jin, C.1,2,3; Kuleshov, D.29; Levochkin, K.29; Li, B. B.13; Li, C.1,3; Li, C.4,5; Li, F.1,3,4; Li, H. B.1,3; Li, H. C.1,3; Li, H. Y.5,16; Li, J.1,3,4; Li, K.1,3; Li, W. L.17; Li, X.4,5; Li, X.20; Li, X. R.1,3; Li, Y.21; Li, Y. Z.1,2,3; Li, Z.1,3; Li, Z.9; Liang, E. W.12; Liang, Y. F.12; Lin, S. J.11; Liu, B.5; Liu, C.1,3; Liu, D.17; Liu, H.20; Liu, H. D.14; Liu, J.1,3; Liu, J. L.19; Liu, J. S.11; Liu, J. Y.1,3; Liu, M. Y.22; Liu, R. Y.15; Liu, S. M.16; Liu, W.1,3; Liu, Y. N.6; Liu, Z. X.21; Long, W. J.20; Lu, R.24; Lv, H. K.1,3; Ma, B. Q.9; Ma, L. L.1,3; Ma, X. H.1,3; Mao JR(毛基荣)25; Masood, A.20; Mitthumsiri, W.32; Montaruli, T.31; Nan, Y. C.17; Pang, B. Y.20; Pattarakijwanich, P.32; Pei, Z. Y.10; Qi, M. Y.1,3; Ruffolo, D.32; Rulev, V.29; Sáiz, A.32; Shao, L.13; Shchegolev, O.29,30; Sheng, X. D.1,3; Shi, J. R.1,3; Song, H. C.9; Stenkin, Yu. V.29,30; Stepanov, V.29; Sun, Q. N.20; Sun, X. N.12; Sun, Z. B.8; Tam, P. H. T.11; Tang, Z. B.4,5; Tian, W. W.2,7; Wang, B. D.1,3; Wang, C.8; Wang, H.20; Wang, H. G.10; Wang JC(王建成)25; Wang, J. S.19; Wang, L. P.17; Wang, L. Y.1,3; Wang, R. N.20; Wang, W.11; Wang, W.23; Wang, X. G.12; Wang, X. J.1,3; Wang, X. Y.15; Wang, Y. D.1,3; Wang, Y. J.1,3; Wang, Y. P.1,2,3; Wang, Z.1,3,4; Wang, Z.19; Wang, Z. H.21; Wang, Z. X.24; Wei, D. M.16; Wei, J. J.16; Wei, Y. J.1,2,3; Wen, T.24; Wu, C. Y.1,3; Wu, H. R.1,3; Wu, S.1,3; Wu, W. X.20; Wu, X. F.16; Xi, S. Q.20; Xia, J.5,16; Xia, J. J.20; Xiang, G. M.2,18; Xiao, G.1,3; Xiao, H. B.10; Xin, G. G.23; Xin, Y. L.20; Xing, Y.18; Xu, D. L.19; Xu, R. X.9; Xue, L.17; Yan DH(闫大海)25; Yang, C. W.21; Yang, F. F.1,3,4; Yang, J. Y.11; Yang, L. L.11; Yang, M. J.1,3; Yang, R. Z.5; Yang, S. B.24; Yao, Y. H.21; Yao, Z. G.1,3; Ye, Y. M.6; Yin, L. Q.1,3; Yin, N.17; You, X. H.1,3; You, Z. Y.1,2,3; Yu, Y. H.17; Yuan, Q.16; Zeng, H. D.16; Zeng, T. X.1,3,4; Zeng, W.24; Zeng, Z. K.1,2,3; Zha, M.1,3; Zhai, X. X.1,3; Zhang, B. B.15; Zhang, H. M.15; Zhang, H. Y.17; Zhang, J. L.7; Zhang, J. W.21; Zhang, L.13; Zhang, L.24; Zhang, L. X.10; Zhang, P. F.24; Zhang, P. P.13; Zhang, R.5,16; Zhang, S. R.13; Zhang, S. S.1,3; Zhang, X.15; Zhang, X. P.1,3; Zhang, Y.1,3; Zhang, Y.1,16; Zhang, Y. F.20; Zhang, Y. L.1,3; Zhao, B.20; Zhao, J.1,3; Zhao, L.4,5; Zhao, L. Z.13; Zhao, S. P.16,17; Zheng, F.8; Zheng, Y.20; Zhou, B.1,3; Zhou, H.19; Zhou, J. N.18; Zhou, P.15; Zhou, R.21; Zhou, X. X.20; Zhu, C. G.17; Zhu, F. R.20; Zhu, H.7; Zhu, K. J.1,2,3,4; Zuo, X.1,3
Contribution Rank第25完成单位
Indexed ByESCI

Purpose Observation of high energy and very high emission from Gamma Ray Bursts (GRBs) is crucial to study the gigantic explosion and the underline processes. With a large field-of-view and almost full duty cycle, the Water Cherenkov Detector Array (WCDA), a sub-array of the Large High Altitude Air Shower Observatory (LHAASO), is appropriate to monitor the very high energy emission from unpredictable transients such as GRBs. Method Nevertheless, the main issue for an extensive air shower array is the high energy threshold which limits the horizon of the detector. To address this issue a new trigger method is developed in this article to lower the energy threshold of WCDA for GRB observation. Result The proposed method significantly improves the detection efficiency of WCDA for gamma-rays around the GRB direction at 10-300 GeV. The sensitivity of the WCDA for GRB detection with the new trigger method is estimated. The achieved sensitivity of the quarter WCDA array above 10 GeV is comparable with that of Fermi-LAT. The data analysis process and corresponding fluence upper limit for GRB 190719C is presented as an example.

Funding ProjectNational Key R&D Program of China[2018YFA0404201] ; Natural Sciences Foundation of China[12022502] ; Natural Sciences Foundation of China[11635011] ; Key R&D Program of SiChuan Province[2019ZYZF0001]
Funding OrganizationNational Key R&D Program of China[2018YFA0404201] ; Natural Sciences Foundation of China[12022502, 11635011] ; Key R&D Program of SiChuan Province[2019ZYZF0001]
Subject Area天文学 ; 天体物理学 ; 高能天体物理学 ; 核科学技术
MOST Discipline Catalogue理学 ; 理学::天文学 ; 工学 ; 工学::核科学与技术
Publication Place#04-01 CENCON I, 1 TANNERY RD, SINGAPORE 347719, SINGAPORE
WOS IDWOS:000722123300002
WOS Research AreaNuclear Science & Technology
WOS SubjectNuclear Science & Technology
Citation statistics
Document Type期刊论文
Corresponding AuthorChen, B. M.
Affiliation1.Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, 100049, China;
2.University of Chinese Academy of Sciences, Beijing, 100049, China;
3.TIANFU Cosmic Ray Research Center, Chengdu, Sichuan, China;
4.State Key Laboratory of Particle Detection and Electronics, Beijing, China;
5.University of Science and Technology of China, Hefei, 230026, Anhui, China;
6.Department of Engineering Physics, Tsinghua University, Beijing, 100084, China;
7.National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China;
8.National Space Science Center, Chinese Academy of Sciences, Beijing, 100190, China;
9.School of Physics, Peking University, Beijing, 100871, China;
10.Center for Astrophysics, Guangzhou University, Guangzhou, 510006, Guangdong, China;
11.School of Physics and Astronomy & School of Physics (Guangzhou), Sun Yat-sen University, Zhuhai, 519000, Guangdong, China;
12.School of Physical Science and Technology, Guangxi University, Nanning, 530004, Guangxi, China;
13.Hebei Normal University, Shijiazhuang, 050024, Hebei, China;
14.School of Physics and Microelectronics, Zhengzhou University, Zhengzhou, 450001, Henan, China;
15.School of Astronomy and Space Science, Nanjing University, Nanjing, 210023, Jiangsu, China;
16.Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, 210023, Jiangsu, China;
17.Institute of Frontier and Interdisciplinary Science, Shandong University, Qingdao, 266237, Shandong, China;
18.Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, 200030, China;
19.Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai, 200240, China;
20.School of Physical Science and Technology & School of Information Science and Technology, Southwest Jiaotong University, Chengdu, 610031, Sichuan, China;
21.College of Physics, Sichuan University, Chengdu, 610065, Sichuan, China;
22.Key Laboratory of Cosmic Rays (Tibet University), Ministry of Education, Lhasa, 850000, Tibet, China;
23.School of Physics and Technology, Wuhan University, Wuhan, 430072, Hubei, China;
24.School of Physics and Astronomy, Yunnan University, Kunming, 650091, Yunnan, China;
25.Yunnan Observatories, Chinese Academy of Sciences, Kunming, 650216, Yunnan, China;
26.Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin, Ireland;
27.Max-Planck-Institut for Nuclear Physics, P.O. Box 103980, 69029, Heidelberg, Germany;
28.Dipartimento di Fisica dell’Università di Napoli “Federico II”, Complesso Universitario di Monte Sant’Angelo, via Cinthia, 80126, Napoli, Italy;
29.Institute for Nuclear Research of Russian Academy of Sciences, Moscow, Russia, 117312;
30.Moscow Institute of Physics and Technology, Moscow, Russia, 141700;
31.Département de Physique Nucléaire et Corpusculaire, Faculté de Sciences, Université de Genève, 24 Quai Ernest Ansermet, 1211, Geneva, Switzerland;
32.Department of Physics, Faculty of Science, Mahidol University, Bangkok, 10400, Thailand
Recommended Citation
GB/T 7714
Aharonian, F.,An, Q.,Axikegu,et al. Line-of-shower trigger method to lower energy threshold for GRB detection using LHAASO-WCDA[J]. RADIATION DETECTION TECHNOLOGY AND METHODS,2021,5(4):531-541.
APA Aharonian, F..,An, Q..,Axikegu.,Bai, L. X..,Bai, Y. X..,...&Zuo, X..(2021).Line-of-shower trigger method to lower energy threshold for GRB detection using LHAASO-WCDA.RADIATION DETECTION TECHNOLOGY AND METHODS,5(4),531-541.
MLA Aharonian, F.,et al."Line-of-shower trigger method to lower energy threshold for GRB detection using LHAASO-WCDA".RADIATION DETECTION TECHNOLOGY AND METHODS 5.4(2021):531-541.
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