【作者】
曹臻;
F.Aharonian;
安琪;
阿西克古;
白云翔;
包逸炜;
D.Bastieri;
毕效军;
毕玉江;
蔡金庭;
曹晴;
曹文羽;
曹喆;
常进;
常劲帆;
陈尚明;
陈恩生;
陈亮;
陈林;
陈龙;
陈明君;
陈玛丽;
陈起辉;
陈素弘;
陈天禄;
陈阳;
程宁;
程耀东;
崔明阳;
崔树旺;
崔晓红;
崔昱东;
戴本忠;
代洪亮;
戴子高;
单增罗布;
D.della Volpe;
董绪强;
段凯凯;
樊军辉;
范一中;
方军;
方堃;
冯存峰;
封莉;
冯少辉;
丰晓婷;
冯有亮;
S.Gabici;
高博;
高川东;
高林青;
高启;
高卫;
高伟康;
葛茂茂;
耿利斯;
G.Giacinti;
龚光华;
苟全补;
顾旻皓;
郭福来;
郭晓磊;
郭义庆;
郭莹莹;
韩毅昂;
何会海;
贺昊宁;
何佳银;
何新波;
何钰;
M.Heller;
贺远强;
侯博文;
侯超;
侯贤;
胡红波;
胡铨;
胡世聪;
黄代绘;
黄天奇;
黄文俊;
黄性涛;
黄晓渊;
黄勇;
黄志成;
季筱璐;
贾焕玉;
贾康;
江琨;
姜晓巍;
姜泽军;
金敏;
康明铭;
柯通;
D.Kuleshov;
K.Kurinov;
李兵兵;
李澄;
李骢;
李丹;
李飞;
李海波;
李会财;
李华阳;
李军;
李剑;
李捷;
李凯;
李文龙;
李文莲;
李秀荣;
李昕;
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;
刘金艳;
刘茂元;
柳若愚;
刘四明;
刘伟;
刘怡;
刘以农;
鲁睿;
罗晴;
吕洪魁;
马伯强;
马玲玲;
马欣华;
毛基荣;
闵振;
W.Mitthumsiri;
穆慧君;
南云程;
A.Neronov;
区子维;
庞彬宇;
P.Pattarakijwanich;
裴致远;
齐孟尧;
祁业情;
乔冰强;
秦家军;
D.Ruffolo;
A.Sáiz;
D.Semikoz;
邵澄宇;
邵琅;
O.Shchegolev;
盛祥东;
舒富文;
宋慧超;
Yu.V.Stenkin;
V.Stepanov;
苏扬;
孙秦宁;
孙晓娜;
孙志斌;
谭柏轩;
唐庆文;
唐泽波;
田文武;
王超;
王昌贝;
王广威;
王洪光;
王惠惠;
王建成;
汪凯;
王利苹;
王玲玉;
王培汉;
王冉;
王为;
王祥高;
王祥玉;
王阳;
王玉东;
王岩谨;
王忠海;
王仲翔;
王振;
王铮;
韦大明;
魏俊杰;
魏永健;
文韬;
吴超勇;
吴含荣;
武莎;
吴雪峰;
吴雨生;
席邵强;
夏捷;
夏君集;
项光漫;
肖迪泫;
肖刚;
辛广广;
辛玉良;
邢祎;
熊峥;
徐东莲;
徐仁峰;
徐仁新;
徐伟立;
薛良;
闫大海;
颜景志;
颜田;
杨朝文;
杨帆;
杨冯帆;
杨何文;
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;
岳华;
曾厚敦;
曾婷轩;
曾玮;
查敏;
张彬彬;
张丰;
张海明;
张恒英;
张建立;
张丽霞;
张力;
张鹏飞;
张佩佩;
张瑞;
张少博;
张少如;
张寿山;
张潇;
张笑鹏;
张云峰;
张毅;
张勇;
赵兵;
赵静;
赵雷;
赵立志;
赵世平;
郑福;
周斌;
周浩;
周佳能;
周猛;
周平;
周荣;
周勋秀;
祝成光;
祝凤荣;
朱辉;
朱科军;
左雄;
LHAASO Collaboration;
【Author】
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;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;D.della Volpe;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;M.Heller;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.Wang;J.C.Wang;K.Wang;L.P.Wang;L.Y.Wang;P.H.Wang;R.Wang;W.Wang;X.G.Wang;X.Y.Wang;Y.Wang;Y.D.Wang;Y.J.Wang;Z.H.Wang;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.Zhang;S.R.Zhang;S.S.Zhang;X.Zhang;X.P.Zhang;Y.F.Zhang;Yi Zhang;Yong Zhang;B.Zhao;J.Zhao;L.Zhao;L.Z.Zhao;S.P.Zhao;F.Zheng;B.Zhou;H.Zhou;J.N.Zhou;M.Zhou;P.Zhou;R.Zhou;X.X.Zhou;C.G.Zhu;F.R.Zhu;H.Zhu;K.J.Zhu;X.Zuo;LHAASO Collaboration;Key Laboratory of Particle Astrophyics & Experimental Physics Division & Computing Center,Institute of High Energy Physics,Chinese Academy of Sciences;University of Chinese Academy of Sciences;Tianfu Cosmic Ray Research Center;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;School of Astronomy and Space Science,Nanjing University;Center for Astrophysics,Guangzhou University;Hebei Normal University;Key Laboratory of Dark Matter and Space Astronomy & Key Laboratory of Radio Astronomy,Purple Mountain Observatory,Chinese Academy of Sciences;Tsung-Dao Lee Institute & School of Physics and Astronomy,Shanghai Jiao Tong 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 (Zhuhai) & School of Physics (Guangzhou) & Sino-French Institute of Nuclear Engineering and Technology (Zhuhai),Sun Yat-sen University;School of Physics and Astronomy,Yunnan University;Département de Physique Nucléaire et Corpusculaire,Facultéde Sciences,Universitéde Genève;Institute of Frontier and Interdisciplinary Science,Shandong University;APC,Universit’e Paris Cit’e,CNRS/IN2P3,CEA/IRFU,Observatoire de Paris;Department of Engineering Physics,Tsinghua University;School of Physics and Microelectronics,Zhengzhou University;Yunnan Observatories,Chinese Academy of Sciences;School of Physics and Astronomy (Zhuhai) & School of Physics(Guangzhou) & Sino-French Institute of Nuclear Engineering and Technology (Zhuhai),Sun Yat-sen University;College of Physics,Sichuan University;Institute for Nuclear Research of Russian Academy of Sciences;Moscow Institute of Physics and Technology;School of Physics,Peking University;School of Physical Science and Technology,Guangxi University;Department of Physics,Faculty of Science,Mahidol University;Center for Relativistic Astrophysics and High Energy Physics,School of Physics and Materials Science & Institute of Space Science and Technology,Nanchang University;National Space Science Center,Chinese Academy of Sciences;
【机构】
Key Laboratory of Particle Astrophyics & Experimental Physics Division & Computing Center,Institute of High Energy Physics,Chinese Academy of Sciences;
University of Chinese Academy of Sciences;
Tianfu Cosmic Ray Research Center;
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;
School of Astronomy and Space Science,Nanjing University;
Center for Astrophysics,Guangzhou University;
Hebei Normal University;
Key Laboratory of Dark Matter and Space Astronomy & Key Laboratory of Radio Astronomy,Purple Mountain Observatory,Chinese Academy of Sciences;
Tsung-Dao Lee Institute & School of Physics and Astronomy,Shanghai Jiao Tong 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 (Zhuhai) & School of Physics (Guangzhou) & Sino-French Institute of Nuclear Engineering and Technology (Zhuhai),Sun Yat-sen University;
School of Physics and Astronomy,Yunnan University;
Département de Physique Nucléaire et Corpusculaire,Facultéde Sciences,Universitéde Genève;
Institute of Frontier and Interdisciplinary Science,Shandong University;
APC,Universit’e Paris Cit’e,CNRS/IN2P3,CEA/IRFU,Observatoire de Paris;
Department of Engineering Physics,Tsinghua University;
School of Physics and Microelectronics,Zhengzhou University;
Yunnan Observatories,Chinese Academy of Sciences;
School of Physics and Astronomy (Zhuhai) & School of Physics(Guangzhou) & Sino-French Institute of Nuclear Engineering and Technology (Zhuhai),Sun Yat-sen University;
College of Physics,Sichuan University;
Institute for Nuclear Research of Russian Academy of Sciences;
Moscow Institute of Physics and Technology;
School of Physics,Peking University;
School of Physical Science and Technology,Guangxi University;
Department of Physics,Faculty of Science,Mahidol University;
Center for Relativistic Astrophysics and High Energy Physics,School of Physics and Materials Science & Institute of Space Science and Technology,Nanchang University;
National Space Science Center,Chinese Academy of Sciences;
【摘要】 The full array of the Large High Altitude Air Shower Observatory(LHAASO) has been in operation since July 2021. For its kilometer-square array(KM2A), we optimized the selection criteria for very high and ultrahigh energy γ-rays using data collected from August 2021 to August 2022, resulting in an improvement in significance of the detection in the Crab Nebula of approximately 15%, compared with that of previous cuts. With the implementation of these new selection criteria, the angular resolution was also significantly improved by approximately 10% at tens of Te V. Other aspects of the full KM2A array performance, such as the pointing error, were also calibrated using the Crab Nebula. The resulting energy spectrum of the Crab Nebula in the energy range of 10-1000Te V are well fitted by a log-parabola model, which is consistent with the previous results from LHAASO and other experiments.更多还原
【Abstract】 The full array of the Large High Altitude Air Shower Observatory(LHAASO) has been in operation since July 2021. For its kilometer-square array(KM2A), we optimized the selection criteria for very high and ultrahigh energy γ-rays using data collected from August 2021 to August 2022, resulting in an improvement in significance of the detection in the Crab Nebula of approximately 15%, compared with that of previous cuts. With the implementation of these new selection criteria, the angular resolution was also significantly improved by approximately 10% at tens of Te V. Other aspects of the full KM2A array performance, such as the pointing error, were also calibrated using the Crab Nebula. The resulting energy spectrum of the Crab Nebula in the energy range of 10-1000Te V are well fitted by a log-parabola model, which is consistent with the previous results from LHAASO and other experiments.更多还原
【基金】 Supported by the National Key R&D Program of China (2018YFA0404201, 2018YFA0404202, 2018YFA0404203, 2018YFA0404204);the National Natural Science Foundation of China (12022502, 12205314, 12105301, 12261160362, 12105294, U1931201);the Youth Innovation Promotion Association CAS (2022010);in Thailand by the National Science and Technology Development Agency (NSTDA);the National Research Council of Thailand (NRCT):High-Potential Research Team Grant Program (N42A650868)