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A dynamic range extension system for LhAASOwCdA-1

Radiation detection Technology and Methods 2021年第4期5卷 520-530页

作者： F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.w.Bao d.Bastieri X.J.Bi Y.J.Bi h.Cai J.T.Cai z.Cao z.Cao J.Chang J.F.Chang X.C.Chang B.M.Chen J.Chen L.Chen L.Chen L.Chen M.J.Chen M.L.Chen Q.h.Chen S.h.Chen S.z.Chen T.L.Chen X.L.Chen Y.Chen N.Cheng Y.d.Cheng S.w.Cui X.h.Cui Y.d.Cui B.z.dai h.L.dai z.G.dai danzengluobu d.della Volpe B.d’Ettorre piazzoli X.J.dong J.h.Fan Y.z.Fan z.X.Fan J.Fang K.Fang C.F.Feng L.Feng S.h.Feng Y.L.Feng B.Gao C.d.Gao Q.Gao w.Gao M.M.Ge L.S.Geng G.h.Gong Q.B.Gou M.h.Gu J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.han h.h.he h.N.he J.C.he S.L.he X.B.he Y.he M.heller Y.K.hor C.hou X.hou h.B.hu S.hu S.C.hu X.J.hu d.h.huang Q.L.huang w.h.huang X.T.huang Y.huang z.C.huang F.Ji X.L.Ji h.Y.Jia K.Jiang z.J.Jiang C.Jin d.Kuleshov K.Levochkin B.B.Li C.Li C.Li F.Li h.B.Li h.C.Li h.Y.Li J.Li K.Li w.L.Li X.Li X.Li X.R.Li Y.Li Y.z.Li z.Li z.Li E.w.Liang Y.F.Liang S.J.Lin B.Liu C.Liu d.Liu h.Liu h.d.Liu J.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu w.Liu Y.N.Liu z.X.Liu w.J.Long R.Lu h.K.Lv B.Q.Ma L.L.Ma X.h.Ma J.R.Mao A.Masood w.Mitthumsiri T.Montaruli Y.C.Nan B.Y.pang p.pattarakijwanich z.Y.pei M.Y.Qi d.Ruffolo V.Rulev A.Sáiz L.Shao O.Shchegolev X.d.Sheng J.R.Shi h.C.Song Yu.V.Stenkin V.Stepanov Q.N.Sun X.N.Sun z.B.Sun p.h.T.Tam z.B.Tang w.w.Tian B.d.wang C.wang h.w.ng h.G.wang J.C.wang J.S.wang L.p.wang L.Y.wang R.N.wang w.wang w.wang X.G.wang X.J.wang X.Y.wang Y.d.wang Y.J.wang Y.p.wang z.wang z.wang z.h.w.ng z.X.wang d.M.wei J.J.wei Y.J.wei T.wen C.Y.wu h.R.wu S.wu w.X.wu X.F.wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang G.Xiao h.B.Xiao G.G.Xin Y.L.Xin Y.Xing d.L.Xu R.X.Xu L.Xue d.h.Yan C.w.yang F.F.yang J.Y.yang L.L.yang M.J.yang R.z.yang S.B.yang Y.h.Yao z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.h.You z.Y.You Y.h.Yu Q.Yuan h.d.zeng T.X.zeng w.zeng z.K.zeng M.zha X.X.zhai B.B.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 R.zhang S.R.zhang S.S.zhang X.zhang X.p.zhang Y.zhang Y.zhang Y.F.zhang Y.L.zhang B.zhao J.zhao L.zhao L.z.zhao S.p.zhao F.zheng Y.zheng B.zhou h.zhou J.N.zhou Key Laboratory of particle Astrophyics&Experimental physics division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of particle detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina d.p.rtment of Engineering physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of physics and Astronomy&School of physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina School of physical Science and Technology Guangxi UniversityNanning 530004GuangxiChina hebei Normal University Shijiazhuang 050024HebeiChina School of physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Key Laboratory of dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-dao Lee Institute&School of physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of physics Sichuan UniversityChengdu 610065SichuanChina Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina School of physics

purpose The main scientific goal of LhAASO-wCdA is to survey gamma-ray sources with energy from 100 GeV to 30 *** observe high-energy sh.w.r events,especially to measure the energy spectrum of cosmic rays from 100 TeV to 10 peV,a dynamic range extension system(wCdA++)is designed to use a 1.5-inch pMT with a dynamic range of four orders of magnitude for each cell in *** The dynamic range is extended by using these pMTs to measure the effective charge density in the core region of air sh.w.r events,which is an important parameter for identifying the composition of primary *** and Conclusion The system has been running for more than one *** this paper,the details of the design and.p.rformance of wCdA++are presented.

关键词： LhAASO-wCdA wCdA++ water Cherenkov detector performance

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LhAASO-KM2A detector simulation using Geant4

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Radiation detection Technology and Methods 2024年第3期8卷 1437-1447页

作者： zhen Cao F.Aharonian Q.An Axikegu Y.X.Bai Y.w.Bao d.Bastieri X.J.Bi Y.J.Bi J.T.Cai Q.Cao w.Y.Cao zhe Cao J.Chang J.F.Chang A.M.Chen E.S.Chen Liang Chen Lin Chen Long Chen M.J.Chen M.L.Chen Q.h.Chen S.h.Chen S.z.Chen T.L.Chen Y.Chen N.Cheng Y.d.Cheng M.Y.Cui S.w.Cui X.h.Cui Y.d.Cui B.z.dai h.L.dai z.G.dai danzengluobu X.Q.dong K.K.duan J.h.Fan Y.z.Fan J.Fang K.Fang C.F.Feng L.Feng S.h.Feng X.T.Feng Y.L.Feng S.Gabici B.Gao C.d.Gao L.Q.Gao Q.Gao w.Gao w.K.Gao M.M.Ge L.S.Geng G.Giacinti G.h.Gong Q.B.Gou M.h.Gu F.L.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.han h.h.he h.N.he J.Y.he X.B.he Y.he Y.K.hor B.w.hou C.hou X.hou h.B.hu Q.hu S.C.hu d.h.huang T.Q.huang w.J.huang X.T.huang X.Y.huang Y.huang z.C.huang X.L.Ji h.Y.Jia K.Jia K.Jiang X.w.Jiang z.J.Jiang M.Jin M.M.Kang T.Ke d.Kuleshov K.Kurinov B.B.Li Cheng Li Cong Li d.Li F.Li h.B.Li h.C.Li h.Y.Li J.Li Jian Li Jie Li K.Li w.L.Li w.L.Li X.R.Li Xin Li Y.z.Li zhe Li zhuo Li E.w.Liang Y.F.Liang S.J.Lin B.Liu C.Liu d.Liu h.Liu h.d.Liu J.Liu J.L.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu w.Liu Y.Liu Y.N.Liu R.Lu Q.Luo h.K.Lv B.Q.Ma L.L.Ma X.h.Ma J.R.Mao z.Min w.Mitthumsiri h.J.Mu Y.C.Nan A.Neronov z.w.Ou B.Y.pang p.pattarakijwanich z.Y.pei M.Y.Qi Y.Q.Qi B.Q.Qiao J.J.Qin d.Ruffolo A.Sáiz d.Semikoz C.Y.Shao L.Shao O.Shchegolev X.d.Sheng F.w.Shu h.C.Song Yu.V.Stenkin V.Stepanov Y.Su Q.N.Sun X.N.Sun z.B.Sun p.h.T.Tam Q.w.Tang z.B.Tang w.w.Tian C.wang C.B.wang G.w.wang h.G.wang h.h.w.ng J.C.wang K.wang L.p.wang L.Y.wang p.h.w.ng R.wang w.wang X.G.wang X.Y.wang Y.wang Y.d.wang Y.J.wang z.h.w.ng z.X.wang zhen wang zheng wang d.M.wei J.J.wei Y.J.wei T.wen C.Y.wu h.R.wu S.wu X.F.wu Y.S.wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang d.X.Xiao G.Xiao G.G.Xin Y.L.Xin Y.Xing z.Xiong d.L.Xu R.F.Xu R.X.Xu w.L.Xu L.Xue d.h.Yan J.z.Yan T.Yan C.w.yang F.yang F.F.yang h.w.yang J.Y.yang L.L.yang M.J.yang R.z.yang S.B.yang Y.h.Yao z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.h.You z.Y.You Y.h.Yu Q.Yuan h.Yue h.d.zeng T.X.zeng w.zeng M.zha B.B.zhang F.zhang h.M.zhang h.Y.zhang J.L.zhang L.X.zhang Li zhang p.F.zhang p.p.zhang R.zhang S.B.zh Key Laboratory of particle Astrophysics&Experimental physics division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing100049China University of Chinese Academy of Sciences Beijing100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-planck-Institute for Nuclear physics 69029Heidelberg103980Germany State Key Laboratory of particle detection and Electronics BeijingChina University of Science and Technology of China Hefei230026AnhuiChina School of physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu610031SichuanChina School of Astronomy and Space Science Nanjing UniversityNanjing210023JiangsuChina Center for Astrophysics Guangzhou UniversityGuangzhou510006GuangdongChina hebei Normal University Shijiazhuang050024HebeiChina Key Laboratory of dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Tsung-dao Lee Institute&School of physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of physics and Astronomy(zhuhai)&School of physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(zhuhai) Sun Yat-sen UniversityGuangzhouZhuhai 510275519000GuangdongChina School of physics and Astronomy Yunnan UniversityKunming 650091YunnanChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina ApC UniversitéParis CitéCNRS/IN2P3CEA/IRFUObservatoire de ParisParis 11975205France d.p.rtment of Engineering phys

KM2A is one of the main sub-arrays of LhAASO,working on gamma ray astronomy and cosmic ray physics at energies above 10 *** simulation is the important foundation for estimating detector performance and data *** is a big challenge to simulate the KM2A detector in the framework of Geant4 due to the need to track numerous photons from a large number of detector units(>6000)with large altitude difference(30)and huge coverage(1.3).In this paper,the design of the KM2A simulation code G4KM2A based on Geant4 is *** process of G4KM2A is optimized mainly in memory consumption to avoid memory *** simplifications are used to significantly speed up the execution of *** running time is reduced by at least 30 times compared to full detector *** particle distributions and the core/angle resolution comparison between simulation and experimental data of the full KM2A array are also presented,which sh.w.good agreement.

关键词： LhAASO KM2A Simulation GEANT4

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Line-of-sh.w.r trigger method to lower energy threshold for GRB detection using LhAASO-wCdA

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Radiation detection Technology and Methods 2021年第4期5卷 531-541页

作者： F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.w.Bao d.Bastieri X.J.Bi Y.J.Bi h.Cai J.T.Cai z.Cao z.Cao J.Chang J.F.Chang X.C.Chan B.M.Chen J.Chen L.Chen L.Chen L.Chen M.J.Chen M.L.Chen Q.h.Chen S.h.Chen S.z.Chen T.L.Chen X.L.Chen Y.Chen N.Chen Y.d.Chen S.w.Cui X.h.Cui Y.d.Cui B.z.dai h.L.dai z.G.dai danzengluobu d.della Volpe B.d’Ettorre piazzoli X.J.don J.h.Fan Y.z.Fan z.X.Fan J.Fang K.Fan C.F.Feng L.Feng S.h.Fen Y.L.Feng B.Gao C.d.Gao Q.Gao w.Gao M.M.Ge L.S.Gen G.h.Gong Q.B.Gou M.h.Gu J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.han h.h.he h.N.he J.C.he S.L.he X.B.he Y.he M.heller Y.K.hor C.hou X.hou h.B.hu S.hu S.C.hu X.J.hu d.h.huang Q.L.huan w.h.huang X.T.huang z.C.huang F.Ji X.L.Ji h.Y.Jia K.Jiang z.J.Jiang C.Jin d.Kuleshov K.Levochkin B.B.Li C.Li C.Li F.Li h.B.Li h.C.Li h.Y.Li J.Li K.Li w.L.Li X.Li X.Li X.R.Li Y.Li Y.z.Li z.Li z.Li E.w.Liang Y.F.Liang S.J.Lin B.Liu C.Liu d.Liu h.Liu h.d.Liu J.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu w.Liu Y.N.Liu z.X.Liu w.J.Long R.Lu h.K.Lv B.Q.Ma L.L.Ma X.h.Ma J.R.Mao A.Masood w.Mitthumsiri T.Montaruli Y.C.Nan B.Y.pang p.pattarakijwanich z.Y.pei M.Y.Qi d.Ruffolo V.Rulev A.Sáiz L.Shao O.Shchegolev X.d.Shen J.R.Shi h.C.Song Yu.V.Stenkin V.Stepanov Q.N.Sun X.N.Sun z.B.Sun p.h.T.Tam z.B.Tang w.w.Tian B.d.wan C.wang h.w.ng h.G.wang J.C.wang J.S.wang L.p.wang L.Y.wan R.N.wang w.wang w.wang X.G.wang X.J.wan X.Y.wang Y.d.wan Y.J.wan Y.p.wang z.wang z.wang z.h.w.ng z.X.wang d.M.wei J.J.wei Y.J.wei T.wen C.Y.wu h.R.wu S.wu w.X.wu X.F.wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang G.Xiao h.B.Xiao G.G.Xin Y.L.Xin Y.Xing d.L.Xu R.X.Xu L.Xue d.h.Yan C.w.yang F.F.yang J.Y.yang L.L.yang M.J.Yan R.z.yang S.B.yang Y.h.Yao z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.h.You z.Y.You Y.h.Yu Q.Yuan h.d.zeng T.X.zeng w.zeng z.K.zeng M.zha X.X.zhai B.B.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 R.zhang S.R.zhang S.S.zhan X.zhang X.p.zhan Y.zhan Y.zhang Y.F.zhang Y.L.zhan B.zhao J.zhao L.zhao L.z.zhao S.p.zhao F.zheng Y.zheng B.zhou h.zhou J.N.zhou p.zhou R.zhou X.X.zhou C.G. Key Laboratory of particle Astrophysics&Experimental physics division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of particle detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina d.p.rtment of Engineering physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of physics and Astronomy&School of physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina School of physical Science and Technology Guangxi UniversityNanning 530004GuangxiChina hebei Normal University Shijiazhuang 050024HebeiChina School of physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Key Laboratory of dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-dao Lee Institute&School of physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of physics Sichuan UniversityChengdu 610065SichuanChina Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina School of physic

purpose Observation of high energy and very high emission from Gamma Ray Bursts(GRBs)is crucial to study the gigantic explosion and the underline *** 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 Sh.w.r Observatory(LhAASO),is appropriate to monitor the very high energy emission from unpredictable transients such as *** Nevertheless,the main issue for an extensive air sh.w.r array is the high energy threshold which limits the horizon of the *** address this issue a new trigger method is developed in this article to lower the energy threshold of wCdA for GRB *** The proposed method significantly improves the detection efficiency of wCdA for gamma-rays around the GRB direction at 10-300 *** sensitivity of the wCdA for GRB detection with the new trigger method is *** achieved sensitivity of the quarter wCdA array above 10 GeV is comparable with that of *** data analysis process and corresponding fluence upper limit for GRB 190719C is presented as an example.

关键词： LhAASO wCdA GRB

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Copper-catalyzed synthesis of phenols from aryl halides and 4-methoxylbenzyl alcohol

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Chinese Chemical Letters 2009年第10期20卷 1170-1174页

作者： Chuan zhou tao wei wei Lu Ji You Sun d.p.rtment of Chemical Engineering Huaihai Institute of Technology Lianyungang 222005 China Jiangsu Marine Resou-rces R & d Institute Lianyungang 222005 China

A catalytic method was developed to synthesize substituted.p.enols from the corresponding aryl bromides and chlorides under mild conditions （yields = 34-92%）. 4-Methoxylbenzyl alcohol was used as water surrogate and... 详细信息

关键词： Copper catalysis water surrogate Cross-coupling phenols

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A New Organic-inorganic hybrid Arsenatotungstate[{Cu(phen)(en)}{Cu(phen)}{Cu_3(phen)_3(α-Asw_9O_(33))}](Oh)·3h_2O

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Chinese Journal of Structural Chemistry 2015年第8期34卷 1247-1252页

作者： LI Jie TIAN Shu-Fang zhou hui MA peng-tao Key Laboratory of polyoxometalate Chemistry of henan province Institute of Molecular and Crystal Engineering College of Chemistry and Chemical Engineering Henan University

A new organic-inorganic hybrid copper-substituted arsenatotungstate complex formulated as [{Cu（phen）（en）} {Cu（phen）} {Cu3（phen）3（α-Asw9033）}]（Oh）·3h2O （1, en = ethylene-diamine, 1,10-phen = 1,10-phenanthroline） has been synthesized by controlling the reaction process and characterized by infrared （IR） spectroscopy, elemental analysis, and thermogravimetric （TG） analysis. Crystal data for 1： C62h56AsCusN12O37w9, Mr=3608.46, monoclinic, space group p21/n, a = 13.245（4）, b = 25.692（9）, c = 24.670（8） A, fl = 99.251（6）°, V= 8286（5） A3, z = 4, GOOF = 1.103, R = 0.0560, wR = 0.1285. In 1, the vacant sites of the trivacant Keggin anion [α-Asw9O33]9- are occupied by three same copper coordination cations [Cu（phen）]2＋. Meanwhile, the lacunary anion [α-AswgO33]9-, is capped by two kinds of copper coordination cations [Cu（phen）]2＋ and [Cu（dhen）（en）]2＋, resulting in an unorecedented dolvcation structure with Cs svmmetrv.

关键词： tungstoarsenate, hydrothermal, crystal structure

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Synthesis, Crystal Structure and Luminescence property of [Ag_2(d.p.)_2(NMp)_2](SbF_6)_2·4h_2O·3Ch_2Cl_2

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Chinese Journal of Structural Chemistry 2005年第12期24卷 1363-1368页

作者： wEI Yong-Qin wU Ke-Chen zhUANG Bo-tao zhou zhang-Feng State Key Laboratory of Structural Chemistry Fujian Instituteof Research on the Structure of MatterThe Chinese Academy of Sciences Fuzhou Fujian 350002 China

The silver-d.p. complex, [Ag2（d.p.）2（NMp）2]（SbF6）2-4h2O-3Ch2Cl2 1 （NMp = 2- （4-dimethylaminophenyl）imidazo（4,5-f）（1,10）phenanthroline, d.p. = d.p.enylphosphinomethane）, was synthesized and its structure was determined by X-ray diffraction. The crystal belongs to monoclinic, space group C2/c, Mr = 2461.61, a = 21.57（10）, b = 22.48（6）, c = 22.53（6）A, β= 101.29（2）°, V= 10713（64）A^3, z= 4, dc= 1.526 g/cm^3,μ= 1.141mm^-1, F（000） = 4920, R =0.0664 and wR = 0.1774 for 8524 observed reflections （1 〉 2σ（I））. Complex 1 exists as a centrosymmetric dimmer. The two d.p. molecules bridge two AgNMp moieties to form an eight-membered Ag2p4C2 metallacyclic ring with ligand NMp chelating to each Ag. It appears photoluminescence （λmax = 625 nm） at room temperature and makes red shift compared with free ligand NMp （λmax = 522 nm）. dFF calculation indicates that the emission of 1 originates from singlet metal-perturbed ILCT excited state.

关键词： silver-d.p. luminescence dFT molecular obital charge-transfer

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Reconstruction of Cherenkov image bymultiple telescopes of LhAASO-wFCTA

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Radiation detection Technology and Methods 2022年第4期6卷 544-557页

作者： F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.w.Bao d.Bastieri X.J.Bi Y.J.Bi J.T.Cai zhe Cao zhen Cao J.Chang J.F.Chang E.S.Chen Liang Chen Liang Chen Long Chen M.J.Chen M.L.Chen Q.h.Chen S.h.Chen S.z.Chen T.L.Chen Y.Chen h.L.Cheng N.Cheng Y.d.Cheng S.w.Cui X.h.Cui Y.d.Cui B.d’Ettorre piazzoli B.z.dai h.L.dai z.G.dai danzengluobu ddella Volpe K.K.duan J.h.Fan Y.z.Fan z.X.Fan J.Fang K.Fang C.F.Feng L.Feng S.h.Feng X.T.Feng Y.L.Feng B.Gao C.d.Gao L.Q.Gao Q.Gao w.Gao w.K.Gao M.M.Ge L.S.Geng G.h.Gong Q.B.Gou M.h.Gu F.L.Guo J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.han h.h.he h.N.he S.L.he X.B.he Y.he M.heller Y.K.hor C.hou X.hou h.B.hu Q.hu S.hu S.C.hu X.J.hu d.h.huang w.h.huang X.T.huang X.Y.huang Y.huang z.C.huang X.L.Ji h.Y.Jia K.Jia K.Jiang z.J.Jiang M.Jin M.M.Kang T.Ke d.Kuleshov K.Levochkin B.B.Li Cheng Li Cong Li F.Li h.B.Li h.C.Li h.Y.Li J.Li Jian Li Jie Li K.Li wLLi XRLi Xin Li Xin Li YzLi zhe Li zhuo Li E.w.Liang Y.F.Liang S.J.Lin B.Liu C.Liu d.Liu h.Liu h.d.Liu J.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu w.Liu Y.Liu Y.N.Liu w.J.Long R.Lu Q.Luo h.K.Lv B.Q.Ma L.L.Ma X.h.Ma J.R.Mao A.Masood z.Min w.Mitthumsiri Y.C.Nan z.w.Ou B.Y.pang p.pattarakijwanich z.Y.pei M.Y.Qi Y.Q.Qi B.Q.Qiao J.J.Qin d.Ruffolo A.Sáiz C.Y.Shao L.Shao O.Shchegolev X.d.Sheng J.Y.Shi h.C.Song Yu.V.Stenkin V.Stepanov Y.Su Q.N.Sun X.N.Sun z.B.Sun p.h.T.Tam z.B.Tang w.w.Tian B.d.wang C.wang h.w.ng h.G.wang J.C.wang J.S.wang L.p.wang L.Y.wang R.wang R.N.wang w.wang X.G.wang X.Y.wang Y.wang Y.d.wang Y.J.wang Y.p.wang z.h.w.ng z.X.wang zhen wang zheng wang d.M.wei J.J.wei Y.J.wei T.wen C.Y.wu h.R.wu S.wu X.F.wu Y.S.wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang d.X.Xiao G.Xiao G.G.Xin Y.L.Xin Y.Xing z.Xiong d.L.Xu R.X.Xu L.Xue d.h.Yan J.z.Yan C.w.yang F.F.yang h.w.yang J.Y.yang L.L.yang M.J.yang R.z.yang S.B.yang Y.h.Yao z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.h.You z.Y.You Y.h.Yu Q.Yuan h.Yue h.d.zeng T.X.zeng w.zeng z.K.zeng M.zha X.X.zhai B.B.zhang F.zhang h.M.zhang h.Y.zhang J.L.zhang L.X.zhang Li zhang Lu zhang p.F.zhang p.p.zhang R.zhang S.B.zhang S.R.zhang S. Key Laboratory of particle Astrophyics&Experimental physics division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina dublin Institute for Advanced Studies 31 Fitzwilliam Place2DublinIreland Max-planck-Institut for Nuclear physics P.O.Box 10398069029 HeidelbergGermany State Key Laboratory of particle detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina School of physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of physics Sichuan UniversityChengdu 610065SichuanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina Key Laboratory of dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China hebei Normal University Shijiazhuang 050024HebeiChina School of physics and Astronomy(zhuhai)&Sino-French Institute of Nuclear Engineering and Technology(zhuhai) Sun Yat-sen UniversityZhuhai 519000China School of physics(Guangzhou) Sun Yat-sen UniversityGuangzhou 510275GuangdongChina d.p.rtimento di Fisica dell’Universitàdi Napoli“Federico II” Complesso Universitario di Monte Sant’Angelovia Cinthia80126 NapoliItaly School of physics and Astronomy Yunnan UniversityKunming 650091YunnanChina d.p.rtement de physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève

Introduction One of main scientiﬁc goals of the Large high Altitude Air Sh.w.r Observatory(LhAASO)is to accurately measure the energy spectra of different cosmic ray compositions around the‘knee’*** wide Field-of-View(FoV)Cherenkov Telescope Array(wFCTA),which is one of the main detectors of LhAASO and has 18 telescopes,is built to achieve this *** telescopes are put together and.p.int to connected directions for a larger *** Telescopes are d.p.oyed spatially as close as possible,but due to their own size,the distance between two adjacent telescopes is about 10 ***,the Cherenkov lateral distribution and the parallax between the two telescopes should be considered in the event building process for images crossing over the boundaries of FoVs of the *** event building method for Cherenkov images measured by multiple telescopes of wFCTA is *** performance of the sh.w.r measurements using the combined images is evaluated by comparing with sh.w.rs that are fully contained by a virtual telescope in *** and conclusion It is proved that the developed event building process can help to increase the FoV of wFCTA by 30%while maintaining the same reconstruction quality,compared to the separate telescope reconstruction method.

关键词： method directions conclusion

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performance of LhAASO-wCdA and observation of the Crab Nebula as a standard candle

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Chinese physics C 2021年第8期45卷 166-181页

作者： F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.w.Bao d.Bastieri X.J.Bi Y.J.Bi h.Cai J.T.Cai z.Cao z.Cao J.Chang J.F.Chang X.C.Chang B.M.Chen J.Chen L.Chen L.Chen L.Chen M.J.Chen M.L.Chen Q.h.Chen S.h.Chen S.z.Chen T.L.Chen X.L.Chen Y.Chen N.Cheng Y.d.Cheng S.w.Cui X.h.Cui Y.d.Cui B.z.dai h.L.dai z.G.dai danzengluobu d.della Volpe B.d'Ettorre piazzoli X.J.dong J.h.Fan Y.z.Fan z.X.Fan J.Fang K.Fang C.F.Feng L.Feng S.h.Feng Y.L.Feng B.Gao C.d.Gao Q.Gao w.Gao M.M.Ge L.S.Geng G.h.Gong Q.B.Gou M.h.Gu J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.han h.h.he h.N.he J.C.he S.L.he X.B.he Y.he M.heller Y.K.hor C.hou X.hou h.B.hu S.hu S.C.hu X.J.hu d.h.huang Q.L.huang w.h.huang X.T.huang z.C.huang F.Ji X.L.Ji h.Y.Jia K.Jiang z.J.Jiang C.Jin d.Kuleshov K.Levochkin B.B.Li C.Li C.Li F.Li h.B.Li h.C.Li h.Y.Li J.Li K.Li w.L.Li X.Li X.Li X.R.Li Y.Li Y.z.Li z.Li z.Li E.w.Liang Y.F.Liang S.J.Lin B.Liu C.Liu d.Liu h.Liu h.d.Liu J.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu w.Liu Y.N.Liu z.X.Liu w.J.Long R.Lu h.K.Lv B.Q.Ma L.L.Ma X.h.Ma J.R.Mao A.Masood w.Mitthumsiri T.Montaruli Y.C.Nan B.Y.pang p.pattarakijwanich z.Y.pei M.Y.Qi B.Q.Qiao d.Ruffolo V.Rulev A.Saiz L.Shao O.Shchegolev X.d.Sheng J.R.Shi h.C.Song Yu.V.Stenkin V.Stepanov Q.N.Sun X.N.Sun z.B.Sun p.h.T.Tam z.B.Tang w.w.Tian B.d.wang C.wang h.w.ng h.G.wang J.C.wang J.S.wang L.p.wang L.Y.wang R.N.wang w.wang w.wang X.G.wang X.J.wang X.Y.wang Y.d.wang Y.J.wang Y.p.wang z.wang z.wang z.h.w.ng z.X.wang d.M.wei J.J.wei Y.J.wei T.wen C.Y.wu h.R.wu S.wu w.X.wu X.F.wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang G.Xiao h.B.Xiao G.G.Xin Y.L.Xin Y.Xing d.L.Xu R.X.Xu L.Xue d.h.Yan C.w.yang F.F.yang J.Y.yang L.L.yang M.J.yang R.z.yang S.B.yang Y.h.Yao z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.h.You z.Y.You Y.h.Yu Q.Yuan h.d.zeng T.X.zeng w.zeng z.K.zeng M.zha X.X.zhai B.B.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 R.zhang S.R.zhang S.S.zhang X.zhang X.p.zhang Y.zhang Y.zhang Y.F.zhang Y.L.zhang B.zhao J.zhao L.zhao L.z.zhao S.p.zhao F.zheng Y.zheng B.zhou h.zhou J.N.zhou Key Laboratory of particle Astrophyics&Experimental physics division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of particle detection and Electronics China University of Science and Technology of China Hefei 230026China d.p.rtment of Engineering physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China School of physics and Astronomy&School of physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519082China School of physical Science and Technology Guangxi UniversityNanning 530004China hebei Normal University Shijiazhuang 050024China School of physics and Microelectronics Zhengzhou UniversityZhengzhou 450001China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Key Laboratory of dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-dao Lee Institute&School of physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China College of physics Sichuan UniversityChengdu 610065China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China School of physics and Technology Wuhan UniversityWuhan 430072China School of physics and Astronomy Yunnan University

The first water Cherenkov detector of the LhAASO experiment(wCdA-1)has been operating since April *** data for the first year have been analyzed to test its performance by observing the Crab Nebula as a standard *** wCdA-1 achieves a sensitivity of 65 mCU per year,with a statistical threshold of 5 *** accomplish this,a 97.7%cosmic-ray background rejection rate around 1 TeV and 99.8%around 6 TeV with an ap proximate photon acceptance of 50%is achieved after applying an algorithm to separate gamma-induced *** 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 *** energy resolution is found to be 33%for gamma rays around 6 *** 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.

关键词： LhAASO-wCdA Crab Nebula angular resolution spectral energy distribution

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Microstructural evolution and mechanical properties of in situ nano Ta_(4)hfC_(5) reinforced SiBCN composite ceramics

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Journal of Advanced Ceramics 2020年第6期9卷 739-748页

作者： Bingzhu wANG daxin LI zhihua yang dechang JIA Jingyi GUAN hao pENG delong CAI peigang hE Xiaoming dUAN Yu zhou tao zhANG Chenguang GAO Institute for Advanced Ceramics School of Materials Science and EngineeringHarbin Institute of TechnologyHarbin 150001China Key Laboratory of Advanced Structural-Functional Integration Materials&Green Manufacturing Technology Harbin Institute of TechnologyHarbin 150001China State Key Laboratory of Advanced welding and Joining Harbin Institute of TechnologyHarbin 150001China Beijing Institute of Control Engineering Beijing 100080China

The in situ nano Ta_(4)hfC_(5) reinforced SiBCN-Ta_(4)hfC_(5) composite ceramics were prepared by a combination of two-step mechanical alloying and reactive hot-pressing *** microstructural evolution and mechanical properties of the resulting SiBCN-Ta_(4)hfC_(5) were *** the first-step milling of 30 h,the raw materials of TaC and hfC underwent crushing,cold sintering,and short-range interdiffusion to finally obtain the high pure nano Ta_(4)hfC_(5).A hybrid structure of amorphous SiBCN and nano Ta_(4)hfC_(5) was obtained by ad.p.ing a second-step *** reactive hot-pressing sintering,amorphous SiBCN has crystallized to 3C-SiC,6h-SiC,and turbostratic BN(C)phases and Ta_(4)hfC_(5) retained the form of the *** the in situ generations of 2.5 wt% Ta_(4)hfC_(5),Ta_(4)hfC_(5) is preferentially distributed within the turbostratic BN(C);h.w.ver,as Ta_(4)hfC_(5) content further raised to 10 wt%,it mainly distributed in the grain-boundary of BN(C) and *** introduction of Ta_(4)hfC_(5) nanocrystals can effectively improve the flexural strength and fracture toughness of SiBCN ceramics,reaching to 344.1 Mpa and 4.52 Mpa·m^(1/2),*** work has solved the problems of uneven distribution of ultra-high temperature phases in the ceramic matrix,which is beneficial to the real applications of SiBCN ceramics.

关键词： Ta_(4)hfC_(5) SiBCN microstructure evolution mechanical properties

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Morphology prediction of dihydroxylammonium 5,5'-bistetrazole-1,1'-diolate (TKX-50) crystal in different solvent systems using modified attachment energy model

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Chinese Journal of Chemical Engineering 2023年第1期53卷 181-193页

作者： Fang Chen tao zhou Lijie Li Chongwei An Jun Li duanlin Cao Jianlong wang School of Chemical Engineering and Technology North University of ChinaTaiyuan 030051China School of Material Science and Engineering Beijing Institute of TechnologyBeijing 100081China School of Environmental and Safety Engineering North University of ChinaTaiyuan 030051China

In order to theoretically study the growth morphology of dihydroxylammonium 5,5’-bistetrazole-1,1’-dio late(TKX-50)crystal in different solvent systems,crystal–solvent models were established,and then molecular dynamics(Md)methods were ad.p.ed as a means to simulate particle *** attachment energy(MAE)model was employed to calculate the growth morphology of *** simulation results demonstrate that COMpASS force field and RESp charge are suitable for molecular dynamics simulation of *** morphologically dominant growth surfaces of TKX-50 in vacuum are(020),(011),(11–1),(100)and(120),*** water(h_(2)O)and N,N-dimethylformamide(dMF)solvents,the(11–1)face is the largest in the habit face,the growth rate of(020)face becomes *** the increase of temperature,the aspect ratios of TKX-50 crystal in dMF solvent increase,and the areas of the(120)faces *** ethylene glycol/h_(2)O mixed solvent system with volume ratio of 1/1,aspect ratio of TKX-50 is relatively *** formic acid/h_(2)O mixed solvents with different volume ratios(1/4,1/3,1/2,1/1 and 2/1),aspect ratio of TKX-50 is relatively small when volume ratio is 1/2.

关键词： TKX-50 Crystal morphology Solvents Modified attachment energy model Molecular dynamics simulation

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