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Performance of LHAASO-WCDA and observation of the Crab Nebula as a standard candle

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【作者】 F.Aharonian安琪阿西克古白立新白云翔包逸炜D.Bastieri毕效军毕玉江蔡浩蔡金庭曹臻曹喆常进常劲帆常潇川陈宝民陈建陈良陈亮陈龙陈明君陈玛丽陈起辉陈素弘陈松战陈天禄陈秀林陈阳程宁程耀东崔树旺崔晓红崔昱东戴本忠代洪亮戴子高单增罗布D.della VolpeB.D’Ettorre Piazzoli董湘军樊军辉范一中范志香方军方堃冯存峰封莉冯少辉冯有亮高博高川东高启高卫葛茂茂耿利斯龚光华苟全补顾旻皓郭俊广郭晓磊郭义庆郭莹莹韩毅昂何会海贺昊宁何坚承何思乐何新波何钰M.Heller贺远强侯超侯贤胡红波胡森胡世聪呼晓军黄代绘黄秋兰黄文昊黄性涛黄志成纪方季筱璐贾焕玉江琨姜泽军靳超D.KuleshovK.Levochkin李兵兵李骢李澄李飞李海波李会财李华阳李捷李凯李文龙李昕李新李秀荣李尧李一卓李哲黎卓梁恩维梁云峰林苏杰刘冰刘成刘栋刘虎刘海东刘佳刘江来刘佳松刘金艳刘茂元柳若愚刘四明刘伟刘以农刘彰兴龙文杰鲁睿吕洪魁马伯强马玲玲马欣华毛基荣A.MasoodW.MitthumsiriT.Montaruli南云程庞彬宇P.Pattarakijwanich裴致远齐孟尧B.Q.QiaoD.RuffoloV.RulevA.Sáiz邵琅O.Shchegolev盛祥东石京燕宋慧超Yu.V.StenkinV.Stepanov孙秦宁孙晓娜孙志斌P.H.T.Tam唐泽波田文武王博东王超王辉王洪光王建成王界双王利苹王玲玉王润娜王为王伟王祥高王晓洁王祥玉王玉东王岩谨王亚平王铮王振王忠海王仲翔韦大明魏俊杰魏永健文韬吴超勇吴含荣武莎吴文雄吴雪峰席邵强夏捷夏君集项光漫肖刚肖胡兵辛广广辛玉良邢祎徐东莲徐仁新薛良闫大海杨朝文杨冯帆杨佳盈杨莉莉杨明洁杨睿智杨深邦姚玉华姚志国叶一锰尹丽巧尹娜游晓浩游智勇于艳红袁强曾厚敦曾婷轩曾玮曾宗康查敏翟徐徐张彬彬张海明张恒英张建立张进文张力张路张丽霞张鹏飞张佩佩张瑞张少如张寿山张潇张笑鹏张毅张勇张云峰张月雷赵兵赵静赵雷赵立志赵世平郑福郑应周斌周浩周佳能周平周荣周勋秀祝成光祝凤荣朱辉朱科军左雄

【Author】 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.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.Wang;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.Wang;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;P.Zhou;R.Zhou;X.X.Zhou;C.G.Zhu;F.R.Zhu;H.Zhu;K.J.Zhu;X.Zuo;Dublin Institute for Advanced Studies;Max-Planck-Institut for Nuclear Physics;State Key Laboratory of Particle Detection and Electronics;University of Science and Technology of China;School of Physical Science and Technology & School of Information Science and Technology, Southwest Jiaotong University;College of Physics, Sichuan University;Key Laboratory of Particle Astrophyics & Experimental Physics Division & Computing Center, Institute of High Energy Physics, Chinese Academy of Sciences;TIANFU Cosmic Ray Research Center;School of Astronomy and Space Science, Nanjing University;Center for Astrophysics, Guangzhou University;University of Chinese Academy of Sciences;School of Physics and Technology, Wuhan University;Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences;Hebei Normal University;Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences;Key Laboratory of Cosmic Rays (Tibet University), Ministry of Education;National Astronomical Observatories, Chinese Academy of Sciences;School of Physics and Astronomy & School of Physics (Guangzhou), Sun Yat-sen University;School of Physics and Astronomy, Yunnan University;Département de Physique Nucléaire et Corpusculaire, Faculté de Sciences, Université de Genève;Dipartimento di Fisica dell’Università di Napoli “Federico Ⅱ”, Complesso Universitario di Monte Sant’Angelo;Institute of Frontier and Interdisciplinary Science, Shandong University;Department of Engineering Physics, Tsinghua University;School of Physics and Microelectronics, Zhengzhou University;Yunnan Observatories, Chinese Academy of Sciences;Institute for Nuclear Research of Russian Academy of Sciences;School of Physics, Peking University;School of Physical Science and Technology, Guangxi University;Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University;Department of Physics, Faculty of Science, Mahidol University;Moscow Institute of Physics and Technology;National Space Science Center, Chinese Academy of Sciences;

【机构】 Dublin Institute for Advanced StudiesMax-Planck-Institut for Nuclear PhysicsState Key Laboratory of Particle Detection and ElectronicsUniversity of Science and Technology of ChinaSchool of Physical Science and Technology & School of Information Science and Technology, Southwest Jiaotong UniversityCollege of Physics, Sichuan UniversityKey Laboratory of Particle Astrophyics & Experimental Physics Division & Computing Center, Institute of High Energy Physics, Chinese Academy of SciencesTIANFU Cosmic Ray Research CenterSchool of Astronomy and Space Science, Nanjing UniversityCenter for Astrophysics, Guangzhou UniversityUniversity of Chinese Academy of SciencesSchool of Physics and Technology, Wuhan UniversityKey Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of SciencesHebei Normal UniversityKey Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of SciencesKey Laboratory of Cosmic Rays (Tibet University), Ministry of EducationNational Astronomical Observatories, Chinese Academy of SciencesSchool of Physics and Astronomy & School of Physics (Guangzhou), Sun Yat-sen UniversitySchool of Physics and Astronomy, Yunnan UniversityDépartement de Physique Nucléaire et Corpusculaire, Faculté de Sciences, Université de GenèveDipartimento di Fisica dell’Università di Napoli “Federico Ⅱ”, Complesso Universitario di Monte Sant’AngeloInstitute of Frontier and Interdisciplinary Science, Shandong UniversityDepartment of Engineering Physics, Tsinghua UniversitySchool of Physics and Microelectronics, Zhengzhou UniversityYunnan Observatories, Chinese Academy of SciencesInstitute for Nuclear Research of Russian Academy of SciencesSchool of Physics, Peking UniversitySchool of Physical Science and Technology, Guangxi UniversityTsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong UniversityDepartment of Physics, Faculty of Science, Mahidol UniversityMoscow Institute of Physics and TechnologyNational Space Science Center, Chinese Academy of Sciences

【摘要】 The first Water Cherenkov detector of the LHAASO experiment(WCDA-1) has been operating since April 2019.The data for the first year have been analyzed to test its performance by observing the Crab Nebula as a standard candle.The WCDA-1 achieves a sensitivity of 65 mCU per year,with a statistical threshold of 5 σ.To accomplish this,a 97.7% cosmic-ray background rejection rate around 1 TeV and 99.8% around 6 TeV with an approximate photon acceptance of 50% is achieved after applying an algorithm to separate gamma-induced showers.The angular resolution is measured using the Crab Nebula as a point source to be approximately 0.450 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 specifications.The energy resolution is found to be 33% for gamma rays around 6 TeV.The 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.

【Abstract】 The first Water Cherenkov detector of the LHAASO experiment(WCDA-1) has been operating since April 2019.The data for the first year have been analyzed to test its performance by observing the Crab Nebula as a standard candle.The WCDA-1 achieves a sensitivity of 65 mCU per year,with a statistical threshold of 5 σ.To accomplish this,a 97.7% cosmic-ray background rejection rate around 1 TeV and 99.8% around 6 TeV with an approximate photon acceptance of 50% is achieved after applying an algorithm to separate gamma-induced showers.The angular resolution is measured using the Crab Nebula as a point source to be approximately 0.450 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 specifications.The energy resolution is found to be 33% for gamma rays around 6 TeV.The 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.

【基金】 Supported by the following grants:the National Key R&D program of China (2018YFA0404201, 2018YFA0404202, 2018YFA0404203);the National Natural Science Foundation of China (12022502, 11905227, U1931112, 11635011, 11761141001, Y811A35, 11675187, U1831208, U1931111);in Thailand by RTA6280002 from Thailand Science Research and Innovation
  • 【文献出处】 Chinese Physics C ,中国物理C , 编辑部邮箱 ,2021年08期
  • 【分类号】P154.3
  • 【下载频次】100
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