Reconstruction of Cherenkov image bymultiple telescopes of LHAASO-WFCTA  

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 

机构地区：[1]Key Laboratory of Particle Astrophyics&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]Dublin Institute for Advanced Studies,31 Fitzwilliam Place,2,Dublin,Ireland [5]Max-Planck-Institut for Nuclear Physics,P.O.Box 103980,69029 Heidelberg,Germany [6]State Key Laboratory of Particle Detection and Electronics,Beijing,China [7]University of Science and Technology of China,Hefei 230026,Anhui,China [8]School of Physical Science and Technology&School of Information Science and Technology,Southwest Jiaotong University,Chengdu 610031,Sichuan,China [9]College of Physics,Sichuan University,Chengdu 610065,Sichuan,China [10]School of Astronomy and Space Science,Nanjing University,Nanjing 210023,Jiangsu,China [11]Center for Astrophysics,Guangzhou University,Guangzhou 510006,Guangdong,China [12]Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy,Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210023,Jiangsu,China [13]Key Laboratory for Research in Galaxies and Cosmology,Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China [14]Key Laboratory of Cosmic Rays(Tibet University),Ministry of Education,Lhasa 850000,Tibet,China [15]National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China [16]Hebei Normal University,Shijiazhuang 050024,Hebei,China [17]School of Physics and Astronomy(Zhuhai)&Sino-French Institute of Nuclear Engineering and Technology(Zhuhai),Sun Yat-sen University,Zhuhai 519000,China [18]School of Physics(Guangzhou),Sun Yat-sen University,Guangzhou 510275,Guangdong,China [19]Dipartimento di Fisica dell’Universitàdi Napoli“Federico II”,Complesso Universitario di Monte Sant’Angelo,via Cinthia,80126 Napoli,Italy [20]School of Physics and Astronomy,Yunnan University,Kunming 650091,Yunnan,China [21]Dépar

出　　处：《Radiation Detection Technology and Methods》2022年第4期544-557,共14页辐射探测技术与方法（英文）

基　　金：supported by the National Key R&D program of China under grants 2018YFA0404201;This research work is also supported by the National Natural Science Foundation of China,with NSFC Grants No.11635011,No.11761141001,No.11905240,No.12105293,No.12105294,No.U2031103,No.U1831208,No.11503021,No.11205126,No.11947404,and No.11675187;by IHEP innovation project No.E25451U2;by the Science and Technology Department of Sichuan Province 2021YFSY0031;by the Xiejialin Foundation of IHEP No.E2546IU2,by RTA6280002 from Thailand Science Research and Innovation in Thailand.

摘　　要：Introduction One of main scientific goals of the Large High Altitude Air Shower Observatory(LHAASO)is to accurately measure the energy spectra of different cosmic ray compositions around the‘knee’region.The 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 goal.Multiple telescopes are put together and point to connected directions for a larger FoV.Method Telescopes are deployed spatially as close as possible,but due to their own size,the distance between two adjacent telescopes is about 10 m.Therefore,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 telescopes.An event building method for Cherenkov images measured by multiple telescopes of WFCTA is developed.The performance of the shower measurements using the combined images is evaluated by comparing with showers that are fully contained by a virtual telescope in simulation.Results 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 

分 类 号：O57[理学—粒子物理与原子核物理]