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Search for very high energy γ-ray emission from GRB 190829A with LHAASO-WCDA triggerless data
Yao, Yuhua1,2; Liu, Wei1; Qiao, Bingqiang1; Guo, Yiqing1; Hu, Hongbo1,3; Yang, Chaowen2; Yao, Zhiguo1; Cao, Zhen4,5,6; Aharonian, F.7,8; An, Q.9,10; Axikegu11; Bai, L. X.12; Bai, Y. X.4,6; Bai, L. X.12; Bai, Y. X.4,6; Bao, Y. W.13; Bastieri, D.14; Bi, X. J.4,5,6; Bi, Y. J.4,6; Cai, H.15; Cai, J. T.14; Cao, Zhe9,10; Chang, J.16; Chang, J. F.4,6,9; Chen, B. M.17; Chen, E. S.4,5,6; Chen, J.12; Chen, Liang4,5,6; Chen, Liang18; Chen, Long11; Chen, M. J.4,6; Chen, M. L.4,6,9; Chen, Q. H.11; Chen, S. H.4,5,6; Chen, S. Z.4,6; Chen, T. L.19; Chen, X. L.4,5,6; Chen, Y.13; Cheng, N.4,6; Cheng, Y. D.4,6; Cui, S. W.17; Cui, X. H.20; Cui, Y. D.21; D’Ettorre Piazzoli, B.22; Dai, B. Z.23; Dai, H. L.4,6,9; Dai, Z. G.10; Danzengluobu19; della Volpe, D.24; Dong, X. J.4,6; Duan, K. K.16; Fan, J. H.14; Fan, Y. Z.16; Fan, Z. X.4,6; Fang, J.23; Fang, K.4,6; Feng, C. F.25; Feng, L.16; Feng, S. H.4,6; Feng, Y. L.16; Gao, B.4,6; Gao, C. D.25; Gao, L. Q.4,5,6; Gao, Q.19; Gao, W.25; Ge, M. M.23; Geng, L. S.4,6; Gong, G. H.26; Gou, Q. B.4,6; Gu, M. H.4,6,9; Guo, F. L.18; Guo, J. G.4,5,6; Guo, X. L.11; Guo, Y. Q.4,6; Guo, Y. Y.4,5,6,16; Han, Y. A.27; He, H. H.4,5,6; He, H. N.16; He, J. C.4,5,6; He, S. L.14; He, X. B.21; He, Y.11; Heller, M.24; Hor, Y. K.21; Hou, C.4,6; Hu, H. B.4,5,6; Hu, S.12; Hu, S. C.4,5,6; Hu, X. J.26; Huang, D. H.11; Huang, Q. L.4,6; Huang, W. H.25; Huang, X. T.25; Huang, X. Y.16; Huang, Z. C.11; Ji, F.4,6; Ji, X. L.4,6,9; Jia, H. Y.11; Jiang, K.9,10; Jiang, Z. J.23; Jin, C.4,5,6; Ke, T.4,6; Kuleshov, D.28; Levochkin, K.28; Li, B. B.17; Li, Cheng9,10; Li, Cong4,6; Li, F.4,6,9; Li, H. B.4,6; Li, H. C.4,6; Li, H. Y.10,16; Li, J.4,6,9; Li, K.4,6; Li, W. L.25; Li, X. R.4,6; Li, Xin9,10; Li, Xin11; Li, Y.12; Li, Y. Z.4,5,6; Li, Zhe4,6; Li, Zhuo29; Liang, E. W.30; Liang, Y. F.30; Lin, S. J.21; Liu, B.10; Liu, C.4,6; Liu, D.25; Liu, H.11; Liu, H. D.27; Liu, J.4,6; Liu, J. L.31; Liu, J. S.21; Liu, J. Y.4,6; Liu, M. Y.19; Liu, R. Y.13; Liu, S. M.11; Liu, W.4,6; Liu, Y.14; Liu, Y. N.26; Liu, Z. X.12; Long, W. J.11; Lu, R.23; Lv, H. K.4,6; Ma, B. Q.29; Ma, L. L.4,6; Ma, X. H.4,6; Mao JR(毛基荣)32; Masood, A.11; Min, Z.4,6; Mitthumsiri, W.33; Montaruli, T.24; Nan, Y. C.25; Pang, B. Y.11; Pattarakijwanich, P.33; Pei, Z. Y.14; Qi, M. Y.4,6; Qi, Y. Q.17; Qiao, B. Q.4,6; Qin, J. J.10; Ruffolo, D.33; Rulev, V.28; Sáiz, A.33; Shao, L.17; Shchegolev, O.28,34; Sheng, X. D.4,6; Shi, J. Y.4,6; Song, H. C.29; Stenkin, Yu. V.28,34; Stepanov, V.28; Su, Y.35; Sun, Q. N.11; Sun, X. N.30
Source PublicationProceedings of Science
Contribution Rank第32完成单位
Indexed ByEI
Conference Name37th International Cosmic Ray Conference, ICRC 2021
Conference Date2021-07-12
Conference PlaceVirtual, Berlin, Germany

The observation of very high energy (VHE, > 100GeV) photon from γ-ray bursts (GRBs) can advance our understanding of their radiation mechanism, the evolution of host-galaxies, violations of Lorentz invariance, extragalactic background light, and intergalactic magnetic field. Recently the measurements on VHE emission from afterglow phase have blossomed and borne fruit while detection of the prompt emission is rare. It’s important to observe prompt emissions by ground-based instruments which take advantage of wide field of view and high duty cycle. Up to now, of the total six GRBs reported with VHE γ-ray emissions, GRB 190829A is the nearest one. The detection of its VHE emission was announced by H.E.S.S. at about 4h 20m after the burst. While during its prompt phase, GRB 190829A was at the edge of the field of view of LHAASO. Benefiting by the high altitude of 4410 m and the triggerless observation mode, the energy threshold of LHAASO is largely reduced to tens of GeV. This work presents the search for VHE γ-ray emission from GRB 190829A with the triggerless data taken by the first pond of LHAASO-WCDA. The analysis shows no indication of VHE emission neither in the prompt nor in the first 2 hours of afterglow phase, thus 95% upper limits are yielded. Furthermore, the upper limits of prompt phase was used to constrain the spectral parameter space of VHE extra component based on a phenomenological model. © Copyright owned by the author(s).

Funding ProjectNational Natural Science Foundation of China[11635011] ; National Natural Science Foundation of China[U1831208]
Funding OrganizationNational Natural Science Foundation of China[11635011, U1831208]
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
SubtypeConference article (CA)
PublisherSissa Medialab Srl
EI Accession Number20230113326408
EI KeywordsGamma rays
EI Classification Number931.3 Atomic and Molecular Physics - 932.1 High Energy Physics
Citation statistics
Document Type会议论文
Affiliation1.College of Physical Science and Technology, Sichuan University, N.29 Wangjiang Road, Jiuyanqiao, Wuhou District, Sichuan Province, Chengdu City, 610064, China;
2.Institute of High Energy Physics, Chinese Academy of Sciences, No.19B Yuquan Road, Shijingshan District, Beijing, 100049, China;
3.University of Chinese Academy of Sciences, 19 A Yuquan Rd, Shijingshan District, Beijing, 100049, China;
4.Key Laboratory of Particle Astrophyics, Experimental Physics Division, Computing Center, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, 100049, China;
5.University of Chinese Academy of Sciences, Beijing, 100049, China;
6.TIANFU Cosmic Ray Research Center, Sichuan, Chengdu, China;
7.Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, 2, Dublin, Ireland;
8.Max-Planck-Institut for Nuclear Physics, P.O. Box 103980, Heidelberg, 69029, Germany;
9.State Key Laboratory of Particle Detection and Electronics, China;
10.University of Science and Technology of China, Anhui, Hefei, 230026, China;
11.School of Physical Science and Technology, School of Information Science and Technology, Southwest Jiaotong University, Sichuan, Chengdu, 610031, China;
12.College of Physics, Sichuan University, Sichuan, Chengdu, 610065, China;
13.School of Astronomy and Space Science, Nanjing University, Jiangsu, Nanjing, 210023, China;
14.Center for Astrophysics, Guangzhou University, Guangdong, Guangzhou, 510006, China;
15.School of Physics and Technology, Wuhan University, Hubei, Wuhan, 430072, China;
16.Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Jiangsu, Nanjing, 210023, China;
17.Hebei Normal University, Hebei, Shijiazhuang, 050024, China;
18.Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, 200030, China;
19.Key Laboratory of Cosmic Rays, Tibet University, Ministry of Education, Tibet, Lhasa, 850000, China;
20.National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China;
21.School of Physics and Astronomy, School of Physics (Guangzhou), Sun Yat-Sen University, Guangdong, Zhuhai, 519000, China;
22.Dipartimento di Fisica, Università di Napoli `‘Federico II
23.School of Physics and Astronomy, Yunnan University, Yunnan, Kunming, 650091, China;
24.D’epartement de Physique Nucl’eaire et Corpusculaire, Facult’e de Sciences, Universit’e de Gen‘eve, 24 Quai Ernest Ansermet, Geneva, 1211, Switzerland;
25.Institute of Frontier and Interdisciplinary Science, Shandong University, Shandong, Qingdao, 266237, China;
26.Department of Engineering Physics, Tsinghua University, Beijing, 100084, China;
27.School of Physics and Microelectronics, Zhengzhou University, Henan, Zhengzhou, 450001, China;
28.Institute for Nuclear Research of Russian Academy of Sciences, Moscow, 117312, Russia;
29.School of Physics, Peking University, Beijing, 100871, China;
30.School of Physical Science and Technology, Guangxi University, Guangxi, Nanning, 530004, China;
31.Tsung-Dao Lee Institute, School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai, 200240, China;
32.Yunnan Observatories, Chinese Academy of Sciences, Yunnan, Kunming, 650216, China;
33.Department of Physics, Faculty of Science, Mahidol University, Bangkok, 10400, Thailand;
34.Moscow Institute of Physics and Technology, Moscow, 141700, Russia;
35.Key Laboratory of Radio Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Jiangsu, Nanjing, 210023, China;
36.National Space Science Center, Chinese Academy of Sciences, Beijing, 100190, China
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Yao, Yuhua,Liu, Wei,Qiao, Bingqiang,et al. Search for very high energy γ-ray emission from GRB 190829A with LHAASO-WCDA triggerless data[C]:Sissa Medialab Srl,2022.
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