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Observations of the brightest UHE Gamma-Ray Sources With the LHAASO-KM2A
Wu, Sha1; Chen, SongZhan1; Liu, Ruo-Yu2; Cao, Zhen1,3,4; Aharonian, F.5,6; An, Q.7,8; Axikegu9; Bai, L. X.10; Bai, Y. X.1,4; Bao, Y. W.2; Bastieri, D.11; Bi, X. J.1,3,4; Bi, Y. J.1,4; Cai, H.12; Cai, J. T.11; Cao, Zhe7,8; Chang, J.13; Chang, J. F.1,4,7; Chen, B. M.14; Chen, E. S.1,3,4; Chen, J.10; Chen, Liang1,3,4,15; Chen, Long9; Chen, M. J.1,4; Chen, M. L.1,4,7; Chen, Q. H.9; Chen, S. H.1,3,4; Chen, S. Z.1,4; Chen, T. L.16; Chen, X. L.1,3,4; Chen, Y.2; Cheng, N.1,4; Cheng, Y. D.1,4; Cui, S. W.14; Cui, X. H.17; Cui, Y. D.18; D’Ettorre Piazzoli, B.19; Dai, B. Z.20; Dai, H. L.1,4,7; Dai, Z. G.8; Danzengluobu16; della Volpe, D.21; Dong, X. J.1,4; Duan, K. K.13; Fan, J. H.11; Fan, Y. Z.13; Fan, Z. X.1,4; Fang, J.20; Fang, K.1,4; Feng, C. F.22; Feng, L.13; Feng, S. H.1,4; Feng, Y. L.13; Gao, B.1,4; Gao, C. D.22; Gao, L. Q.1,3,4; Gao, Q.16; Gao, W.22; Ge, M. M.20; Geng, L. S.1,4; Gong, G. H.23; Gou, Q. B.1,4; Gu, M. H.1,4,7; Guo, F. L.15; Guo, J. G.1,3,4; Guo, X. L.9; Guo, Y. Q.1,4; Guo, Y. Y.1,3,4,13; Han, Y. A.24; He, H. H.1,3,4; He, H. N.13; He, J. C.1,3,4; He, S. L.11; He, X. B.18; He, Y.9; Heller, M.21; Hor, Y. K.18; Hou, C.1,4; Hu, H. B.1,3,4; Hu, S.10; Hu, S. C.1,3,4; Hu, X. J.23; Huang, D. H.9; Huang, Q. L.1,4; Huang, W. H.22; Huang, X. T.22; Huang, X. Y.13; Huang, Z. C.9; Ji, F.1,4; Ji, X. L.1,4,7; Jia, H. Y.9; Jiang, K.7,8; Jiang, Z. J.20; Jin, C.1,3,4; Ke, T.1,4; Kuleshov, D.25; Levochkin, K.25; Li, B. B.14; Li, Cheng7,8; Li, Cong1,4; Li, F.1,4,7; Li, H. B.1,4; Li, H. C.1,4; Li, H. Y.8,13; Li, J.1,4,7; Li, K.1,4; Li, W. L.22; Li, X. R.1,4; Li, Xin7,8,9; Li, Y.10; Li, Y. Z.1,3,4; Li, Zhe1,4; Li, Zhuo26; Liang, E. W.27; Liang, Y. F.27; Lin, S. J.18; Liu, B.8; Liu, C.1,4; Liu, D.22; Liu, H.9; Liu, H. D.24; Liu, J.1,4; Liu, J. L.28; Liu, J. S.18; Liu, J. Y.1,4; Liu, M. Y.16; Liu, R. Y.2; Liu, S. M.9; Liu, W.1,4; Liu, Y.11; Liu, Y. N.23; Liu, Z. X.10; Long, W. J.9; Lu, R.20; Lv, H. K.1,4; Ma, B. Q.26; Ma, L. L.1,4; Ma, X. H.1,4; Mao JR(毛基荣)29; Masood, A.9; Min, Z.1,4; Mitthumsiri, W.30; Montaruli, T.21; Nan, Y. C.22; Pang, B. Y.9; Pattarakijwanich, P.30; Pei, Z. Y.11; Qi, M. Y.1,4; Qi, Y. Q.14; Qiao, B. Q.1,4; Qin, J. J.8; Ruffolo, D.30; Rulev, V.25; Sáiz, A.30; Shao, L.14; Shchegolev, O.25,31; Sheng, X. D.1,4; Shi, J. Y.1,4; Song, H. C.26; Stenkin, Yu. V.25,31; Stepanov, V.25; Su, Y.32; Sun, Q. N.9; Sun, X. N.27; Sun, Z. B.33; Tam, P. H.18; Tang, Z. B.7,8; Tian, W. W.3,17; Wang, B. D.1,4; Wang, C.33; Wang, H.9; Wang, H. G.11
Source PublicationProceedings of Science
Contribution Rank第29完成单位
Indexed ByEI
Conference Name37th International Cosmic Ray Conference, ICRC 2021
Conference Date2021-07-12
Conference PlaceVirtual, Berlin, Germany

Cosmic rays are high-energy charged particles that come from outer space. They play an important role in the evolution of our Galaxy. Gamma-ray emission produced by cosmic rays is a direct probe of cosmic rays and their accelerators. As a key sub-array of the Large High Altitude Air Shower Observatory (LHAASO), KM2A is the most sensitive gamma-ray detector at ultra-high energy (UHE, >100 TeV) band. Here, we report four of the brightest UHE sources measured by LHAASO, LHAASO J1825-1326, LHAASO J1908+0621, LHAASO J2108+5157 and LHAASO J2226+6057. The morphology and spectral energy distribution of these sources are studied respectively using the KM2A data collected from December 2019 to December 2020. The origin of the UHE gamma-ray emission is also discussed taking into account the implications from multi-wavelength observations. © Copyright owned by the author(s).

Funding ProjectN/A
Funding OrganizationN/A
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 Number20230213354767
EI KeywordsCosmic rays
EI Classification Number657 Space Physics - 657.2 Extraterrestrial Physics and Stellar Phenomena - 931.3 Atomic and Molecular Physics - 932.1 High Energy Physics
Citation statistics
Document Type会议论文
Affiliation1.Key Laboratory of Particle Astrophyics, Experimental Physics Division, Computing Center, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, 100049, China;
2.School of Astronomy and Space Science, Nanjing University, Jiangsu, Nanjing, 210023, China;
3.University of Chinese Academy of Sciences, Beijing, 100049, China;
4.TIANFU Cosmic Ray Research Center, Sichuan, Chengdu, China;
5.Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, 2, Dublin, Ireland;
6.Max-Planck-Institut for Nuclear Physics, P.O. Box 103980, Heidelberg, 69029, Germany;
7.State Key Laboratory of Particle Detection and Electronics, China;
8.University of Science and Technology of China, Anhui, Hefei, 230026, China;
9.School of Physical Science and Technology, School of Information Science and Technology, Southwest Jiaotong University, Sichuan, Chengdu, 610031, China;
10.College of Physics, Sichuan University, Sichuan, Chengdu, 610065, China;
11.Center for Astrophysics, Guangzhou University, Guangdong, Guangzhou, 510006, China;
12.School of Physics and Technology, Wuhan University, Hubei, Wuhan, 430072, China;
13.Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Jiangsu, Nanjing, 210023, China;
14.Hebei Normal University, Hebei, Shijiazhuang, 050024, China;
15.Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, 200030, China;
16.Key Laboratory of Cosmic Rays, Tibet University, Ministry of Education, Tibet, Lhasa, 850000, China;
17.National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China;
18.School of Physics and Astronomy, School of Physics (Guangzhou), Sun Yat-Sen University, Guangdong, Zhuhai, 519000, China;
19.Dipartimento di Fisica, Università di Napoli `‘Federico II
20.School of Physics and Astronomy, Yunnan University, Yunnan, Kunming, 650091, China;
21.D’epartement de Physique Nucl’eaire et Corpusculaire, Facult’e de Sciences, Universit’e de Gen‘eve, 24 Quai Ernest Ansermet, Geneva, 1211, Switzerland;
22.Institute of Frontier and Interdisciplinary Science, Shandong University, Shandong, Qingdao, 266237, China;
23.Department of Engineering Physics, Tsinghua University, Beijing, 100084, China;
24.School of Physics and Microelectronics, Zhengzhou University, Henan, Zhengzhou, 450001, China;
25.Institute for Nuclear Research of Russian Academy of Sciences, Moscow, 117312, Russia;
26.School of Physics, Peking University, Beijing, 100871, China;
27.School of Physical Science and Technology, Guangxi University, Guangxi, Nanning, 530004, China;
28.Tsung-Dao Lee Institute, School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai, 200240, China;
29.Yunnan Observatories, Chinese Academy of Sciences, Yunnan, Kunming, 650216, China;
30.Department of Physics, Faculty of Science, Mahidol University, Bangkok, 10400, Thailand;
31.Moscow Institute of Physics and Technology, Moscow, 141700, Russia;
32.Key Laboratory of Radio Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Jiangsu, Nanjing, 210023, China;
33.National Space Science Center, Chinese Academy of Sciences, Beijing, 100190, China
Recommended Citation
GB/T 7714
Wu, Sha,Chen, SongZhan,Liu, Ruo-Yu,et al. Observations of the brightest UHE Gamma-Ray Sources With the LHAASO-KM2A[C]:Sissa Medialab Srl,2022.
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