【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 Volpe;
B.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.Kuleshov;
K.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.Masood;
W.Mitthumsiri;
T.Montaruli;
南云程;
庞彬宇;
P.Pattarakijwanich;
裴致远;
齐孟尧;
D.Ruffolo;
V.Rulev;
A.Sáiz;
邵琅;
O.Shchegolev;
盛祥东;
石京燕;
宋慧超;
Yu.V.Stenkin;
V.Stepanov;
孙秦宁;
孙晓娜;
孙志斌;
谭柏轩;
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;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;Hebei Normal University;School of Astronomy and Space Science, Nanjing University;Center for Astrophysics, Guangzhou University;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;School of Physics and Technology, Wuhan University;Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences;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, 24 Quai Ernest Ansermet;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;LHAASO Collaboration;
【机构】
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;
Hebei Normal University;
School of Astronomy and Space Science, Nanjing University;
Center for Astrophysics, Guangzhou University;
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;
School of Physics and Technology, Wuhan University;
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences;
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, 24 Quai Ernest Ansermet;
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;
LHAASO Collaboration;
【摘要】 A sub-array of the Large High Altitude Air Shower Observatory(LHAASO),KM2A is mainly designed to observe a large fraction of the northern sky to hunt for y-ray sources at energies above 10 TeV.Even though the detector construction is still underway,half of the KM2A array has been operating stably since the end of 2019.In this paper,we present the KM2A data analysis pipeline and the first observation of the Crab Nebula,a standard candle in very high energy y-ray astronomy.We detect y-ray signals from the Crab Nebula in both energy ranges of 10-100 TeV and> 100 TeV with high significance,by analyzing the KM2A data of 136 live days between December 2019 and May 2020.With the observations,we test the detector performance,including angular resolution,pointing accuracy and cosmic-ray background rejection power.The energy spectrum of the Crab Nebula in the energy range 10-250 TeV fits well with a single power-law function dN/dE=(1.13±0.05stat±0.08sys)×10-14·(E/20 TeV)-3.09±0.06stat±0.02sys cm-2 s-1 TeV-1.It is consistent with previous measurements by other experiments.This opens a new window of y-ray astronomy above 0.1 PeV through which new ultrahigh-energy γ-ray phenomena,such as cosmic PeVatrons,might be discovered.更多还原
【Abstract】 A sub-array of the Large High Altitude Air Shower Observatory(LHAASO),KM2A is mainly designed to observe a large fraction of the northern sky to hunt for y-ray sources at energies above 10 TeV.Even though the detector construction is still underway,half of the KM2A array has been operating stably since the end of 2019.In this paper,we present the KM2A data analysis pipeline and the first observation of the Crab Nebula,a standard candle in very high energy y-ray astronomy.We detect y-ray signals from the Crab Nebula in both energy ranges of 10-100 TeV and> 100 TeV with high significance,by analyzing the KM2A data of 136 live days between December 2019 and May 2020.With the observations,we test the detector performance,including angular resolution,pointing accuracy and cosmic-ray background rejection power.The energy spectrum of the Crab Nebula in the energy range 10-250 TeV fits well with a single power-law function dN/dE=(1.13±0.05stat±0.08sys)×10-14·(E/20 TeV)-3.09±0.06stat±0.02sys cm-2 s-1 TeV-1.It is consistent with previous measurements by other experiments.This opens a new window of y-ray astronomy above 0.1 PeV through which new ultrahigh-energy γ-ray phenomena,such as cosmic PeVatrons,might be discovered.更多还原
【基金】 Supported in China by National Key R&D program of China under the grants (2018YFA0404201,2018YFA0404202,2018YFA0404203);by NSFC (12022502,11905227,11635011,11761141001,U1931112,11775131,U1931201,11905043,U1931108);by NSFSPC (ZR2019MA014);in Thailand by RTA6280002 from Thailand Science Research and Innovation