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Deterministic reversal of single magnetic vortex circulation by an electric field

Science Bulletin 2020年第15期65卷 1260-1267,M0003页

作者： Yuelin Zhang Chuanshou wang Houbing Huang Jingdi Lu Renrong liang Jian Liu Renci Peng Qintong Zhang Qinghua Zhang Jing wang Lin Gu Xiu-Feng Han Long-Qing Chen Ramamoorthy Ramesh Ce-Wen nan Jinxing Zhang department of physics Beijing Normal UniversityBeijing 100875China Advanced Research Institute of Multidisciplinary Science Beijing Institute of TechnologyBeijing 100081China tsinghua National Laboratory for Information Science and Technology Institute of MicroelectronicsTsinghua UniversityBeijing 100084China department of Materials Science and Engineering and department of physics University of CaliforniaBerkeley and Materials Science DivisionLawrence Berkeley National LaboratoryBerkeleyCA 94720USA State Key Laboratory of New Ceramics and Fine Processing School of Materials Science and EngineeringTsinghua UniversityBeijing 100084China beijing National Laboratory of Condensed Matter physics Institute of PhysicsChinese Academy of SciencesBeijing 100190China department of Materials Science and Engineering The Pennsylvania State UniversityUniversity ParkPA 16802USA

The ability to control magnetic vortex is critical for their potential applications in spintronic *** methods including magnetic field,spin-polarized current *** been used to flip the core and/or reverse circulation of ***,it is challenging for deterministic electric-field control of the single magnetic vortex textures with time-reversal broken symmetry and no planar magnetic *** it is reported that a deterministic reversal of single magnetic vortex circulation can be driven back and forth by a space-varying strain in multiferroic heterostructures,which is controlled by using a bi-axial pulsed electric ***-field simulation reveals the mechanism of the emerging magnetoelastic energy with the space variation and visualizes the reversal pathway of the *** deterministic electric-field control of the single magnetic vortex textures demonstrates a new approach to integrate the low-dimensional spin texture into the magnetoelectric thin film devices with low energy consumption.

关键词： Deterministic reversal Electric-field control Space-varying strain Single magnetic vortex Multiferroic heterostructures

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Optimization of performance of the KM2A full array using the Crab Nebula

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Chinese physics C 2024年第6期48卷 169-178页

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 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 Chengdu 610000China Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institut for Nuclear physics P.O.Box 10398069029 HeidelbergGermany State Key Laboratory of Particle Detection and Electronics China university of Science and Technology of china Hefei 230026China School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China center for astrophysics Guangzhou UniversityGuangzhou 510006China Hebei Normal university Shijiazhuang 050024China Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China 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 UniversityZhuhai 519000&Guangzhou 510275China School of physics and Astronomy Yunnan UniversityKunming 650091China Département de Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève24 Quai Ernest Ansermet1211 GenevaSwitzerland Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China APC Universit'e Paris Cit'eCNRS/IN2P3CEA/IRFUObservat

The full array of the Large High Altitude Air Shower Observatory(LHAASO)has been in operation since July *** its kilometer-square array(KM2A),we optimized the selection criteria for very high and ultrahigh energyγ-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 *** the implementation of these new selection criteria,the angular resolution was also significantly improved by approximately 10%at tens of *** aspects of the full KM2A array performance,such as the pointing error,were also calibrated using the Crab *** resulting energy spectrum of the Crab Nebula in the energy range of 10-1000 TeV are well fitted by a log-parabola model,which is consistent with the previous results from LHAASO and other experiments.

关键词： γ-ray Crab Nebula significance

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Overview to the Hard X-ray Modulation Telescope (Insight-HXMT) Satellite

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Science china(physics,Mechanics & Astronomy) 2020年第4期63卷 2-19页

作者： Shuang-nan Zhang TiPei Li FangJun Lu LiMing Song YuPeng X u CongZhan Liu Yong Chen XueLei Cao QingCui Bu Zhi Chang Gang Chen Li Chen TianXiang Chen YiBao Chen YuPeng Chen Wei Cui WeiWei Cui JingKang Deng YongWei Dong Yuan Yuan Du MinXue Fu GuanHua Gao He Gao Min Gao MingYu Ge YuDong Gu Ju Guan Can Gungor ChengCheng Guo DaWei Han Wei Hu Yue Huang Jia Huo ShuMei Jia LuHua Jiang WeiChun Jiang Jing Jin YongJie Jin Bing Li ChengKui Li Gang Li MaoShun Li Wei Li Xian Li XiaoBo Li XuFang Li YanGuo Li ZiJian Li ZhengWei Li XiaoHua liang JinYuan Liao GuoQing Liu HongWei Liu ShaoZhen Liu XiaoJing Liu Yuan Liu YiNong Liu Bo Lu XueFeng Lu Tao Luo Xiang Ma Bin Meng Yi nang JianYin Nie Ge Ou JinLu Qu Na Sai RenCheng Shang GuoHong Shen liang Sun Ying Tan Lian Tao YouLi Tuo Chen wang ChunQin wang GuoFeng wang HuanYu wang Juan wang WenShuai wang YuSa wang XiangYang Wen BaiYang Wu BoBing Wu Mei Wu GuangCheng Xiao ShaoLin Xiong LinLi Yan JiaWei Yang Sheng Yang YanJi Yang QiBin Yi Bin Yuan AiMei Zhang ChunLei Zhang ChengMo Zhang Fan Zhang HongMei Zhang Juan Zhang Qiang Zhang ShenYi Zhangs Shu Zhang Tong Zhang WanChang Zhang Wei Zhang WenZhao Zhang Yi Zhang YiFei Zhang YongJie Zhang Yue Zhang Zhao Zhang Zhi Zhang Ziliang Zhang HaiSheng Zhao XiaoFan Zhao ShiJie Zheng JianFeng Zhou YuXuan Zhu Yue Zhu RenLin Zhuang Key Laboratory of Particle astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China university of Chinese Academy of Sciences Beijing 100049China department of Astronomy Tsinghua UniversityBeijing 100084China department of physics Tsinghua UniversityBeijing 100084China department of Astronomy Beijing Normal UniversityBeijing 100088China department of Engineering physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science center Chinese Academy of SciencesBeijing 100190China

As china’s first X-ray astronomical satellite, the Hard X-ray Modulation Telescope (HXMT), which was dubbed as Insight-HXMT after the launch on June 15, 2.17, is a wide-band(1-250 ke V) slat-collimator-based X-ray astronomy satellite with the capability of all-sky monitoring in 0.2-3 Me V. It was designed to perform pointing, scanning and gamma-ray burst(GRB)observations and, based on the Direct Demodulation Method (DDM), the image of the scanned sky region can be *** we give an overview of the mission and its progresses, including payload, core sciences, ground calibration/facility, ground segment, data archive, software, in-orbit performance, calibration, background model, observations and some preliminary results.

关键词： X-and γ-ray telescopes and instrumentation neutron stars black holes X-ray binaries γ-ray bursts

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盘点气候风险机遇,展望健康繁荣未来

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科学通报 2024年第27期69卷 4005-4011页

作者：张诗卉张弛蔡闻佳白玉琪 Max Callaghan 常楠陈彬陈慧琪程亮亮戴瀚程代鑫范维澄房小怡高仝耿阳关大博胡艺馨华峻翊黄存瑞黄弘黄建斌黄小猛纪思翰蒋俏蕾姜晓朋 Gregor Kiesewetter 李湉湉梁璐林波荣林华亮刘欢刘起勇刘小波刘钊刘竹刘昱甫陆波鲁晨曦罗震宇马伟米志付任超 Marina Romanello 沈鉴翔苏婧孙语泽孙昕璐汤绪 Maria Walawender 王灿王情汪蕊 Laura Warnecke 魏汪宇文三妹谢杨熊辉徐冰颜钰杨秀姚芳虹俞乐袁嘉灿曾仪娉张镜张璐张锐张尚辰张少辉赵梦真郑大山周浩周景博周子乔罗勇宫鹏清华大学地球系统科学系北京100084 北京理工大学管理学院北京100081 Mercator Research Institute on Global Commons and Climate Change Mercator Research Institute on Global Commons and Climate ChangeBerlin 10829Germany 南京医科大学公共卫生学院南京211166 北京师范大学环境学院北京100875 中山大学公共卫生学院广州510080 北京大学环境科学与工程学院北京100871 清华大学公共安全研究所北京100084 清华大学工程物理系北京100084 中国气象科学研究院气象影响与风险研究中心北京100086 山东师范大学商学院济南250013 清华大学建筑学院北京100084 南方科技大学统计与数据科学系深圳518055 中国海洋大学国际事务与公共管理学院青岛266003 清华大学万科公共卫生学院北京100084 清华大学新闻与传播学院北京100084 世界卫生组织驻华代表处北京100600 Pollution Management Research Group EnergyClimateand Environment ProgramInternational Institute for Applied Systems Analysis(IIASA)Laxenburg 1-A-2361Austria 中国疾病预防控制中心环境与健康相关产品安全所环境健康风险评估室北京102206 department of Landscape Architecture&Environmental Planning University of CaliforniaBerkeley CA 94607USA 清华大学环境学院北京100084 中国疾病预防控制中心传染病预防控制所传染病预防控制国家重点实验室北京102206 北京经济管理职业学院临空经济管理学院北京100102 中国气象局国家气候中心北京100081 Geography College of Life and Environmental SciencesUniversity of ExeterExeter EX12LUUK 山东大学齐鲁医学院公共卫生学院流行病学系济南250002 The Bartlett School of Sustainable Construction University College LondonLondon WC1H 0ALUK 香港大学建筑学院中国香港999077 Institute for Global Health University College LondonLondon WC1H 0ALUK 清华大学人文学院北京100084 复旦大学大气与海洋系/大气科学研究院上海200438 复旦大学极端天气/气候事件与人体健康风险互联和治理国际卓越中心上海200438 北京航空航天大学经济与管理学院北京100083 香港科技大学计算机科学与工程系广州511453 清华大学气候变化与可持续发展研究院北京100084 北京大学体育教研部北京100871 清华大学苏世民学院北京100084 清华大学城市治理与可持续发展研究院北京100084 百度研究院北京100091 香港大学地球科学系和地理系中国香港999077

气候变化带来的健康风险与日俱增,煤炭消费及相关碳排放量的反弹,再度敲响了中国气候变化警钟.2022年,中国面临了严峻的气候挑战.极端天气事件发生的频率和强度不断上升,许多地区气温纪录屡创新高,全国平均气温攀升至历史第二高位,同时... 详细信息

气候变化带来的健康风险与日俱增,煤炭消费及相关碳排放量的反弹,再度敲响了中国气候变化警钟.2022年,中国面临了严峻的气候挑战.极端天气事件发生的频率和强度不断上升,许多地区气温纪录屡创新高,全国平均气温攀升至历史第二高位,同时降水量自2.12年以来创新低,南方地区遭遇夏秋连旱,而湖南和东北地区则出现了极端降雨和洪涝灾害.采取及时、充分的措施不仅能减轻气候变化对健康的影响,还将保护基础设施不被极端天气破坏.

关键词：煤炭消费极端天气事件基础设施气候变化极端降雨碳排放量气候风险盘点

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Timing analysis of the black hole candidate EXO 1846–031 with Insight-HXMT monitoring

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Research in Astronomy and astrophysics 2021年第3期21卷 193-204页

作者： He-Xin Liu Yue Huang Guang-Cheng Xiao Qing-Cui Bu Jin-Lu Qu Shu Zhang Shuang-nan Zhang Shu-Mei Jia Fang-Jun Lu Xiang Ma Lian Tao Wei Zhang Li Chen Li-Ming Song Ti-Pei Li Yu-Peng Xu Xue-Lei Cao Yong Chen Cong-Zhan Liu Ce Cai Zhi Chang Gang Chen Tian-Xiang Chen Yi-Bao Chen Yu-Peng Chen Wei Cui Wei-Wei Cui Jing-Kang Deng Yong-Wei Dong Yuan-Yuan Du Min-Xue Fu Guan-Hua Gao He Gao Min Gao Ming-Yu Ge Yu-Dong Gu Ju Guan Cheng-Cheng Guo Da-Wei Han Jia Huo Lu-Hua Jiang Wei-Chun Jiang Jing Jin Yong-Jie Jin Ling-Da Kong Bing Li Cheng-Kui Li Gang Li Mao-Shun Li Wei Li Xian Li Xiao-Bo Li Xu-Fang Li Yang-Guo Li Zheng-Wei Li Xiao-Hua liang Jing-Yuan Liao Bai-Sheng Liu Guo-Qing Liu Hong-Wei Liu Xiao-Jing Liu Yi-Nong Liu Bo Lu Xue-Feng Lu Qi Luo Tao Luo Bin Meng Yi nang Jian-Yin Nie Ge Ou Na Sai Ren-Cheng Shang Xin-Ying Song liang Sun Ying Tan You-Li Tuo Chen wang Guo-Feng wang Juan wang Ling-Jun wang Weng-Shuai wang Yu-Sa wang Xiang-Yang Wen Bai-Yang Wu Bo-Bing Wu Mei Wu Shuo Xiao Shao-Lin Xiong He Xu Jia-Wei Yang Sheng Yang Yan-Ji Yang Yi-Jung Yang Qi-Bin Yi Qian-Qing Yin Yuan You Ai-Mei Zhang Cheng-Mo Zhang Fan Zhang Hong-Mei Zhang Juan Zhang Tong Zhang Wan-Chang Zhang Wen-Zhao Zhang Yi Zhang Yi-Fei Zhang Yong-Jie Zhang Yuan-Hang Zhang Yue Zhang Zhao Zhang Zhi Zhang Zi-liang Zhang Hai-Sheng Zhao Xiao-Fan Zhao Shi-Jie Zheng Yao-Guang Zheng Deng-Ke Zhou Jian-Feng Zhou Yu-Xuan Zhu Ren-Lin Zhuang Yue Zhu Key Laboratory of Particle astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China university of Chinese Academy of Sciences Chinese Academy of SciencesBeijing 100049China Institut fur Astronomie und Astrophysik Kepler Center for Astro and Particle PhysicsEberhard Karls Universität72076 TubingenGermany department of Astronomy Beijing Normal UniversityBeijing 100088China department of Astronomy Tsinghua UniversityBeijing 100084China department of physics Tsinghua UniversityBeijing 100084China department of Engineering physics Tsinghua UniversityBeijing 100084China Key Laboratory of Space Astronomy and Technology National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China College of physics Sciences&Technology Hebei UniversityBaoding 071002Hebei ProvinceChina

We present the observational results from a detailed timing analysis of the black hole candidate EXO 1846-031 during its outburst in 2.19 with the observations of Insight-HXMT,NICER and *** outburst can be classified roughly into four different ***-C quasi-periodic oscillations(QPOs)observed by NICER(about 0.1-6 Hz)and Insight-HXMT(about 0.7-8 Hz)are also reported in this ***,we study various physical quantities related to QPO *** QPO rms-frequency relationship in the energy band 1-10 keV indicates that there is a turning pointing in frequency around2 Hz,which is similar to that of GRS 1915+105.A possible hypothesis for the relationship above may be related to the inclination of the source,which may require a high inclination to explain *** relationships between QPO frequency and QPO rms,hardness,total fractional rms and count rate have also been found in other transient sources,which can indicate that the origin of type-C QPOs is non-thermal.

关键词： X-ray binaries black hole candidate QPO EXO 1846–031

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硫酸盐非均相机制对颗粒物污染的影响:上海典型污染事件的WRF-Chem模拟

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环境科学 2022年第5期43卷 2294-2303页

作者：张茹涵张皓然冯伟航汤克勤马亚平王红丽黄成胡建林张宏亮李楠南京信息工程大学环境科学与工程学院江苏省大气环境监测与污染控制高技术研究重点实验室江苏省大气环境与装备技术协同创新中心南京210044 复旦大学环境科学与工程系上海200438 赫尔辛基大学理学院芬兰00014 北京大学物理学院大气与海洋科学系北京100871 上海市环境科学研究院国家环境保护城市大气复合污染成因与防治重点实验室上海200233

硫酸盐气溶胶是大气中细颗粒物(PM_(2.5))的重要组成部分,对霾的形成起着重要作用.传统的模式中硫酸盐生成机制主要包括SO_(2)与·OH的气相反应和SO_(2)·H_(2)O水合物产生的亚硫酸与O_(3)/H_(2)O_(2)的液相反应.SO_(2)非均相生成硫酸... 详细信息

硫酸盐气溶胶是大气中细颗粒物(PM_(2.5))的重要组成部分,对霾的形成起着重要作用.传统的模式中硫酸盐生成机制主要包括SO_(2)与·OH的气相反应和SO_(2)·H_(2)O水合物产生的亚硫酸与O_(3)/H_(2)O_(2)的液相反应.SO_(2)非均相生成硫酸盐的机制(在高NH_(3)情景下,以NO_(2)为氧化剂,非均相摄取SO_(2))非常重要,尤其成为重污染期间颗粒物浓度暴发性增长的原因之一.将硫酸盐非均相机制的参数化方案纳入WRF-Chem模式,模拟了2.17年1月的长三角区域污染物浓度,评估了硫酸盐非均相反应对颗粒物浓度模拟的提高及其对长三角重污染的贡献.结果表明,传统WRF-Chem模式模拟的上海地区硫酸盐月均浓度为6.5μg·m^(-3),较观测值低估33%;尤其是在重颗粒物污染期间,低估高达127%.加入硫酸盐非均相机制后,WRF-Chem对硫酸盐的模拟效果得到显著提升,月均硫酸盐模拟浓度较传统模式提高2.1μg·m^(-3),更好地与地面观测站点的观测值匹配(标准化平均偏差由-48%~-34%降低到-29%~-13%);尤其是在颗粒物污染时段,硫酸盐浓度的提升高达28.2~37.2μg·m^(-3)(104%~167%).研究提高了对长三角地区冬季大气污染的模拟能力,为制定科学地管控策略提供了支持.

关键词：硫酸盐非均相反应天气研究与预报耦合大气化学模型(WRF-Chem) PM_(2.5) 长三角

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Feasibility and physics potential of detecting ^(8)B solar neutrinos at JUNO

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Chinese physics C 2021年第2期45卷 93-110页

作者： Angel Abusleme Thomas Adam Shakeel Ahmad Sebastiano Aiello Muhammad Akram Nawab Ali Fengpeng An Guangpeng An Qi An Giuseppe Andronico Nikolay Anfimov Vito Antonelli Tatiana Antoshkina Burin Asavapibhop João Pedro Athayde Marcondes de André Didier Auguste Andrej Babic Wander Baldini Andrea Barresi Eric Baussan Marco Bellato Antonio Bergnoli Enrico Bernieri David Biare Thilo Birkenfeld Sylvie Blin David Blum Simon Blyth Anastasia Bolshakova Mathieu Bongrand Clément Bordereau Dominique Breton Augusto Brigatti Riccardo Brugnera Riccardo Bruno Antonio Budano Max Buesken Mario Buscemi Jose Busto Ilya Butorov Anatael Cabrera Hao Cai Xiao Cai Yanke Cai Zhiyan Cai Antonio Cammi Agustin Campeny Chuanya Cao Guofu Cao Jun Cao Rossella Caruso Cédric Cerna Jinfan Chang Yun Chang Pingping Chen Po-An Chen Shaomin Chen Shenjian Chen Xurong Chen Yi-Wen Chen Yixue Chen Yu Chen Zhang Chen Jie Cheng Yaping Cheng Alexander Chepurnov Davide Chiesa Pietro Chimenti Artem Chukanov Anna Chuvashova Gérard Claverie Catia Clementi Barbara Clerbaux Selma Conforti Di Lorenzo Daniele Corti Salvatore Costa Flavio Dal Corso Christophe De La Taille Jiawei Deng Zhi Deng Ziyan Deng Wilfried Depnering Marco Diaz Xuefeng Ding Yayun Ding Bayu Dirgantara Sergey Dmitrievsky Tadeas Dohnal Georgy Donchenko Jianmeng Dong Damien Dornic Evgeny Doroshkevich Marcos Dracos Frédéric Druillole Shuxian Du Stefano Dusini Martin Dvorak Timo Enqvist Heike Enzmann Andrea Fabbri Lukas Fajt Donghua Fan Lei Fan Can Fang Jian Fang Marco Fargetta Anna Fatkina Dmitry Fedoseev Vladko Fekete Li-Cheng Feng Qichun Feng Richard Ford Andrey Formozov Amélie Fournier Haonan Gan Feng Gao Alberto Garfagnini Alexandre Göttel Christoph Genster Marco Giammarchi Agnese Giaz Nunzio Giudice Franco Giuliani Maxim Gonchar Guanghua Gong Hui Gong Oleg Gorchakov Yuri Gornushkin Marco Grassi Christian Grewing Maxim Gromov Vasily Gromov Minghao Gu Xiaofei Gu Yu Gu Mengyun Guan Nunzio Guardone Maria Gul Cong Guo Jingyuan Guo Wanlei Guo Xinheng Guo Yuhang Guo Paul Hackspacher Caren Hagner Ran Han Yan Yerevan physics Institute YerevanArmenia UniversitéLibre de Bruxelles BrusselsBelgium Universidade Estadual de Londrina LondrinaBrazil Pontificia Universidade Catolica do Rio de Janeiro RioBrazil Pontificia Universidad Católica de Chile SantiagoChile Universidad Tecnica Federico Santa Maria ValparaisoChile beijing Institute of Spacecraft Environment Engineering BeijingChina beijing Normal university BeijingChina china Institute of Atomic Energy BeijingChina Institute of High Energy physics BeijingChina North china Electric Power university BeijingChina School of physics Peking UniversityBeijingChina tsinghua university BeijingChina university of Chinese Academy of Sciences BeijingChina Jilin university ChangchunChina College of Electronic Science and Engineering National University of Defense TechnologyChangshaChina Chongqing university ChongqingChina Dongguan university of Technology DongguanChina Jinan university GuangzhouChina Sun Yat-Sen university GuangzhouChina Harbin Institute of Technology HarbinChina university of Science and Technology of china HefeiChina The Radiochemistry and Nuclear Chemistry Group in university of South china HengyangChina Wuyi university JiangmenChina Shandong university JinanChina Institute of Modern physics Chinese Academy of SciencesLanzhouChina nanjing university NanjingChina Guangxi university NanningChina East china university of Science and Technology ShanghaiChina School of physics and Astronomy Shanghai Jiao Tong UniversityShanghaiChina Tsung-Dao Lee Institute Shanghai Jiao Tong UniversityShanghaiChina Institute of Hydrogeology and Environmental Geology Chinese Academy of Geological SciencesShijiazhuangChina nankai university TianjinChina Wuhan university WuhanChina Xi’an Jiaotong university Xi’anChina Xiamen university XiamenChina School of physics and Microelectronics Zhengzhou UniversityZhengzhouChina Institute of physics National Chiao-Tung university Hsinchu National United university Miao-Li department of physics National T

The Jiangmen Underground Neutrino Observatory(JUNO)features a 20 kt multi-purpose underground liquid scintillator sphere as its main *** of JUNO's features make it an excellent location for^8B solar neutrino measurements,such as its low-energy threshold,high energy resolution compared with water Cherenkov detectors,and much larger target mass compared with previous liquid scintillator *** this paper,we present a comprehensive assessment of JUNO's potential for detecting^8B solar neutrinos via the neutrino-electron elastic scattering process.A reduced 2 MeV threshold for the recoil electron energy is found to be achievable,assuming that the intrinsic radioactive background^(238)U and^(232)Th in the liquid scintillator can be controlled to 10^(-17)g/*** ten years of data acquisition,approximately 60,000 signal and 30,000 background events are *** large sample will enable an examination of the distortion of the recoil electron spectrum that is dominated by the neutrino flavor transformation in the dense solar matter,which will shed new light on the inconsistency between the measured electron spectra and the predictions of the standard three-flavor neutrino oscillation *** m^(2)_(21)=4.8times10^(-5);(7.5times10^(-5))eV^(2),JUNO can provide evidence of neutrino oscillation in the Earth at approximately the 3sigma(2sigma)level by measuring the non-zero signal rate variation with respect to the solar zenith ***,JUNO can simultaneously measureDelta m^2_(21)using^8B solar neutrinos to a precision of 20% or better,depending on the central value,and to sub-percent precision using reactor antineutrinos.A comparison of these two measurements from the same detector will help understand the current mild inconsistency between the value of Delta m^2_(21)reported by solar neutrino experiments and the KamLAND experiment.

关键词： neutrino oscillation solar neutrino JUNO

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Geometrical reconstruction of fluorescence events observed by the LHAASO experiment

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Chinese physics C 2021年第4期45卷 416-425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.DEtorre Piazzoli X.J.Dong J.H.Fan Y.Z.Fan Z.X.Fan J.Fang J.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.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.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.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.F.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 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 Paricle Detection and Electronics China university of Science and Technology of china HefeiAnhui 230026China department 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 UniversityGuangzhouGuangdong 510006China School of physics and Astronomy&School of physics(Guangzhou) Sun Yat-sen UniversityZhuhaiGuangdong 519000China School of Physical Science and Technology Guangxi UniversityNanningGuangxi 530004China Hebei Normal university ShijiazhuangHebei 050024China School of physics and Microelectronics Zhengzhou UniversityZhengzhouHenan 450001China School of Astronomy and Space Science Nanjing UniversityNanjingJiangsu 210023China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjingJiangsu 210023China Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdaoShandong 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 Southwest Jiaotong UniversityChengduSichuan 610031China College of physics Sichuan UniversityChengduSichuan 610065China Key Laboratory of Cosmic Rays(Tibet university) Ministry of EducationLhasaTibet 850000China School of physics and technology Wuhan UniversityWuhanHubei 430072Ch

The LHAASO-WFCTA experiment,which aims to observe cosmic rays in the sub-EeV range using the fluorescence technique,uses a new generation of high-performance *** ensure that the experiment has ex-cellent detection capability associated with the measurement of the energy spectrum,the primary composition of cosmic rays,and so on,an accurate geometrical reconstruction of air-shower events is *** paper de-scribes the development and testing of geometrical reconstruction for stereo viewed events using the WFCTA(Wide Field of view Cherenkov/Fluorescence Telescope Array)*** approaches,which take full advantage ofthe WFCTA *** *** is the stereo-angular method,which uses the pointing of triggered SiPMs in the shower trajectory,and the other is the stereo-timing method,which uses the triggering time of the fired *** results show that both methods have good geometrical resolution:the resolution of the stereo-timing method is slightly better than the stereo-angular method because the resolution of the latter is slightly limited by the shower track length.

关键词： cosmic ray fluorescence telescope stereo observation geometrical reconstruction

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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.wang 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.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.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 Dipartimento di Fisica dell’Universitàdi Napoli“Federico II” Complesso Universitario di Monte Sant’Angelovia Cinthia80126 NapoliItaly School of physics and Astronomy Yunnan UniversityKunming 650091YunnanChina Département de Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève

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’*** 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 point to connected directions for a larger *** Telescopes are deployed 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 shower measurements using the combined images is evaluated by comparing with showers 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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Observation of the Crab Nebula with LHAASO-KM2A−a performance study

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Chinese physics C 2021年第2期45卷 518-530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 J.Chang J.F.Chang X.C.Chang B.M.Chen J.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 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 F.Li H.B.Li H.C.Li H.Y.Li J.Li K.Li W.L.Li X.Li X.R.Li Y.Li Y.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 X.G.wang X.J.wang X.Y.wang Y.D.wang Y.J.wang Y.P.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.X.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhang X.Zhang X.P.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 Key Laboratory of Particle Astrophyics&Experimental physics Division&Computing center Institute of High Energy PhysicsChinese Academy of Sciences100049 BeijingChina university of Chinese Academy of Sciences 100049 BeijingChina TIANFU Cosmic Ray Research center ChengduSichuanChina State Key Laboratory of Particle Detection and Electronics China university of Science and Technology of china 230026 HefeiAnhuiChina department of Engineering physics Tsinghua University100084 BeijingChina National Astronomical Observatories Chinese Academy of Sciences100101 BeijingChina National Space Science center Chinese Academy of Sciences100190 BeijingChina School of physics Peking University100871 BeijingChina center for astrophysics Guangzhou University510006 GuangzhouGuangdongChina School of physics and Astronomy&School of physics(Guangzhou) Sun Yat-sen University519000 ZhuhaiGuangdongChina School of Physical Science and Technology Guangxi University530004 NanningGuangxiChina Hebei Normal university 050024 ShijiazhuangHebeiChina School of physics and Microelectronics Zhengzhou University450001 ZhengzhouHenanChina School of Astronomy and Space Science Nanjing University210023 NanjingJiangsuChina Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of Sciences210023 NanjingJiangsuChina Institute of Frontier and Interdisciplinary Science Shandong University266237 QingdaoShandongChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of Sciences200030 ShanghaiChina Tsung-Dao Lee Institute&School of physics and Astronomy Shanghai Jiao Tong University200240 ShanghaiChina School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong University610031 ChengduSichuanChina College of physics Sichuan University610065 ChengduSichuanChina Key Laboratory of Cosmic Rays(Tibet university) Ministry of Education850000 LhasaTibetChina School of physics and Tec

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 γ-ray sources at energies above 10 *** though the detector construction is still underway,half of the KM2A array has been operating stably since the end of *** this paper,we present the KM2A data analysis pipeline and the first observation of the Crab Nebula,a standard candle in very high energy γ-ray *** detect γ-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 2.19 and May *** the observations,we test the detector performance,including angular resolution,pointing accuracy and cosmic-ray background rejection *** 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)-309±0.06stat±0.02syscm^(-2) s^(-1) TeV^(-1).It is consistent with previous measurements by other *** opens a new window of γ-ray astronomy above 0.1 PeV through which new ultrahigh-energy γ-ray phenomena,such as cosmic PeVatrons,might be discovered.

关键词： γ-ray Crab Nebula extensive air showers cosmic rays

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