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Simulation Study on Scaler Mode in LHAASO-KM2A
Huang, Zhicheng1; Huang, Daihui1; Zhou, Xunxiu1; Zhao, Jing2; He, Huihai2; Chen, Songzhan2; Ma, Xinhua2; Liu, Dong3; Axi, Kegu1; Zhao, Bing1; Cao, Zhen4,5,6; Aharonian, F.7,8; An, Q.9,10; Axikegu11; Bai, L. X.12; Bai, Y. X.4,6; Bao, Y. W.4; Bastieri, D.4; Bi, X. J.4,5,6; Bi, Y. J.4,6; Cai, H.4,5; Cai, J. T.4; Cao, Zhe9,10; Chang, J.4,6; Chang, J. F.4,6,9; Chen, B. M.4,7; 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; Saiz, 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
会议录名称Proceedings of Science
2022-03-18
卷号395
DOI10.22323/1.395.0365
产权排序第32完成单位
收录类别EI
会议名称37th International Cosmic Ray Conference, ICRC 2021
会议日期2021-07-12
会议地点Virtual, Berlin, Germany
关键词Scaler mode Shower mode LHAASO KM2A Monte Carlo simulations Cosmic rays
摘要

LHAASO, located at Daocheng in Sichuan province of China with an altitude up to 4410 m above the sea level, takes the function of hybrid technology to detect cosmic rays. As the major array of LHAASO, KM2A is composed of 5195 electromagnetic particle detectors (EDs) and 1188 muon detectors (MDs). In the ground-based experiments, there are two common independent data acquisition systems, corresponding to the scaler and shower operation modes. In order to learn more about the scaler mode in LHAASO-KM2A, we adopt the CORSIKA to study the shower development and employ the G4KM2A (based on Geant4) to simulate the detector responses. For one cluster (composed of 64 EDs) in the array of KM2A-ED, the event rates of showers having a number of fired EDs ≥ 1, 2, 3 and 4 (in a time coincidence of 100 ns) are recorded. The average rates of the four multiplicities are ∼ 88 kHz, ∼ 1.4 kHz, ∼ 210 Hz and ∼ 110 Hz, respectively. For the array of KM2A-MD, there are 16 MDs in one cluster. The average rates with multiplicities ≥ 1 and 2 are ∼ 84 kHz and ∼ 890 Hz, respectively. The corresponding primary energies are also given. According to our simulations, the energy threshold of the scaler mode can be lowered to ∼ 100 GeV. At the same time, the energy threshold of LHAASO-KM2A in shower mode is presented for comparison. The simulation results in this work are beneficial for the online trigger with scaler mode, and also be useful in understanding the experiment results in LHAASO-KM2A. © Copyright owned by the author(s).

资助项目National Natural Science Foundation of China[11475141] ; National Natural Science Foundation of China[12047576] ; National Natural Science Foundation of China[U2031101]
项目资助者National Natural Science Foundation of China[11475141, 12047576, U2031101]
语种英语
学科领域天文学 ; 天体物理学 ; 高能天体物理学 ; 核科学技术
学科门类理学 ; 理学::天文学 ; 工学 ; 工学::核科学与技术
文章类型Conference article (CA)
出版者Sissa Medialab Srl
URL查看原文
EI入藏号20230113325067
EI主题词Cosmic rays
EI分类号471.1 Oceanography, General - 657 Space Physics - 657.2 Extraterrestrial Physics and Stellar Phenomena - 723.2 Data Processing and Image Processing - 723.4 Artificial Intelligence - 922.2 Mathematical Statistics - 944.7 Radiation Measuring Instruments
引用统计
文献类型会议论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/25725
专题星系类星体研究组
作者单位1.School of Physical Science and Technology, Southwest Jiaotong University, Chengdu, 610031, China;
2.Institute of High Energy Physics, CAS, Beijing, 100049, China;
3.Institute of Frontier and Interdisciplinary Science, Shandong University, Qingdao, 266237, 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, Universit‘a di Napoli
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, 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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Huang, Zhicheng,Huang, Daihui,Zhou, Xunxiu,et al. Simulation Study on Scaler Mode in LHAASO-KM2A[C]:Sissa Medialab Srl,2022.
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