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Evid.nce for particle acceleration approaching PeV energies in the W51 complex

Science Bulletin 2024年第18期69卷 2833-2841页

作者： Cao, Zhen Aharonian, F. Axikegu Bai, Y.X. Bao, Y.W. Bastieri, d. Bi, X.J. Bi, Y.J. Bian, W. Bukevich, A.V. Cao, Q. Cao, W.Y. Cao, Zhe Chang, J. Chang, J.F. Chen, A.M. Chen, E.S. Chen, H.X. Chen, Liang Chen, Lin Chen, Long Chen, M.J. Chen, M.L. Chen, Q.H. Chen, S. Chen, S.H. Chen, S.Z. Chen, T.L. Chen, Y. Cheng, N. Cheng, Y.d. Cui, M.Y. Cui, S.W. Cui, X.H. Cui, Y.d. d.i, B.Z. d.i, H.L. d.i, Z.G. d.nzengluobu d.ng, X.Q. d.an, K.K. Fan, J.H. Fan, Y.Z. Fang, J. Fang, J.H. Fang, K. Feng, C.F. Feng, H. Feng, L. Feng, S.H. Feng, X.T. Feng, Y. Feng, Y.L. Gabici, S. Gao, B. Gao, C.d. Gao, Q. Gao, W. Gao, W.K. Ge, M.M. Geng, L.S. Giacinti, G. Gong, G.H. Gou, Q.B. Gu, M.H. Guo, F.L. Guo, X.L. Guo, Y.Q. Guo, Y.Y. Han, Y.A. Hasan, M. He, H.H. He, H.N. He, J.Y. He, Y. Hor, Y.K. Hou, B.W. Hou, C. Hou, X. Hu, H.B. Hu, Q. Hu, S.C. Huang, d.H. Huang, T.Q. Huang, W.J. Huang, X.T. Huang, X.Y. Huang, Y. Ji, X.L. Jia, H.Y. Jia, K. Jiang, K. Jiang, X.W. Jiang, Z.J. Jin, M. Kang, M.M. Karpikov, I. kuleshov. d. Kurinov, K. Li, B.B. Li, C.M. Li, Cheng Li, Cong Li, d. Li, F. Li, H.B. Li, H.C. Li, Jian Li, Jie Li, K. Li, S.d. Li, W.L. Li, X.R. Li, Xin Li, Y.Z. Li, Zhe Li, Zhuo Liang, E.W. Liang, Y.F. Lin, S.J. Liu, B. Liu, C. Liu, d. Liu, d.B. Liu, H. Liu, H.d. Liu, J. Liu, J.L. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, Y. Liu, Y.N. Luo, Q. Luo, Y. Lv, H.K. Ma, B.Q. Ma, L.L. Ma, X.H. Mao, J.R. Min, Z. Mitthumsiri, W. Mu, H.J. Nan, Y.C. Neronov, A. Ou, L.J. Pattarakijwanich, P. Pei, Z.Y. Qi, J.C. Qi, M.Y. Qiao, B.Q. Qin, J.J. Raza, A. Ruffolo, d. Sáiz, A. Saeed. M. Semikoz, d. Shao, L. Shchegolev, O. Sheng, X.d. Shu, F.W. Song, H.C. Stenkin, Yu.V. Stepanov, V. Su, Y. Sun, d.X. Sun, Q.N. Sun, X.N. Sun, Z.B. Takata, J. Tam, P.H.T. Key Laboratory of Particle Astrophysics & Experimental Physics d.vision & Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing 100049 China University of Chinese Acad.my of Sciences Beijing 100049 China TIANFU Cosmic Ray Research Center Chengdu China d.blin Institute for Ad.anced.Stud.es 31 Fitzwilliam Place 2 Dublin Ireland Max-Planck-Institut for Nuclear Physics P.O. Box 103980 Heidelberg 69029 Germany School of Physical Science and.Technology & School of Information Science and.Technology Southwest Jiaotong University Chengdu 610031 China School of Astronomy and.Space Science Nanjing University Nanjing 210023 China Center for Astrophysics Guangzhou University Guangzhou 510006 China Tsung-d.o Lee Institute & School of Physics and.Astronomy Shanghai Jiao Tong University Shanghai 200240 China Institute for Nuclear Research of Russian Acad.my of Sciences Moscow 117312 Russia Hebei Normal University Shijiazhuang 050024 China University of Science and.Technology of China Hefei 230026 China State Key Laboratory of Particle d.tection and.Electronics China Key Laboratory of d.rk Matter and.Space Astronomy & Key Laboratory of Rad.o Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing 210023 China Research Center for Astronomical Computing Zhejiang Laboratory Hangzhou 311121 China Key Laboratory for Research in Galaxies and.Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai 200030 China School of Physics and.Astronomy Yunnan University Kunming 650091 China Key Laboratory of Cosmic Rays (Tibet University) Ministry of Education Lhasa 850000 China National Astronomical Observatories Chinese Academy of Sciences Beijing 100101 China School of Physics and.Astronomy (Zhuhai) & School of Physics (Guangzhou) & Sino-French Institute of Nuclear Engineering and.Technology (Zhuhai) Sun Yat-sen University Zhuhai 519000 & Guangzhou 510275 Guangdong China Institute of Frontier and.

The γ-ray emission from the W51 complex is wid.ly acknowled.ed.to be attributed.to the interaction between the cosmic rays (CRs) accelerated.by the shock of supernova remnant (SNR) W51C and.the d.nse molecular cloud. in the ad.acent star-forming region, W51B. However, the maximum acceleration capability of W51C for CRs remains elusive. Based.on observations cond.cted.with the Large High Altitud. Air Shower Observatory (LHAASO), we report a significant d.tection of γ rays emanating from the W51 complex, with energies from 2 to 200 TeV. The LHAASO measurements, for the first time, extend.the γ-ray emission from the W51 complex beyond.100 TeV and.reveal a significant spectrum bend.ng at tens of TeV. By combining the "π0-d.cay bump" featured.d.ta from Fermi-LAT, the broad.and.γ-ray spectrum of the W51 region can be well-characterized.by a simple pp-collision mod.l. The observed.spectral bend.ng feature suggests an exponential cutoff at ∼400 TeV or a power-law break at ∼200 TeV in the CR proton spectrum, most likely provid.ng the first evid.nce of SNRs serving as CR accelerators approaching the PeV regime. Ad.itionally, two young star clusters within W51B could.also be theoretically viable to prod.ce the most energetic γ rays observed.by LHAASO. Our find.ngs strongly support the presence of extreme CR accelerators within the W51 complex and.provid. new insights into the origin of Galactic CRs. © 2024 Science China Press

关键词： Cosmic rays

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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.d.lla 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 d.vision&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Acad.my of Sciences Beijing 100049China Tianfu Cosmic Ray Research Center Chengdu 610000China d.blin Institute for Ad.anced.Stud.es 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 10398069029 HeidelbergGermany State Key Laboratory of Particle d.tection 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 d.rk Matter and.Space Astronomy&Key Laboratory of Rad.o Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Tsung-d.o 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 d.partement d. Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève24 Quai Ernest Ansermet1211 GenevaSwitzerland Institute of Frontier and.Interd.sciplinary Science Shandong UniversityQingdao 266237China APC Universit'e Paris Cit'eCNRS/IN2P3CEA/IRFUObservat

The full array of the Large High Altitud. 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 d.ta collected.from August 2021 to August 2022,resulting in an improvement in significance of the d.tection 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 mod.l,which is consistent with the previous results from LHAASO and.other experiments.

关键词： γ-ray Crab Nebula significance

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机械手连杆的挠曲变形对抓手位置和形态的影响

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机器人 2000年第2期22卷 122-127页

作者：焦国太阿.德.依科拉夫瓦.谢.库利绍夫华北工学院8系莫斯科工业大学机器人教研室

以机械手运动学及连杆坐标变换为基础 ,在已知各连杆由于挠曲变形所产生的相对微小位移的条件下 ,提出了计算机器人抓手的位置和形态误差的方法 .并以斯坦福机械手为例进行了实例计算。

关键词：机械手连杆挠曲变形机器人抓手位置

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Performance and.calibration of quark/gluon-jet taggers using 140 fb^(-1) of pp collisions at √s=13 TeV with the ATLAS d.tector

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Chinese Physics C 2024年第2期48卷 1-25页

作者： G. Aad.B. Abbott K. Abeling N.J. Abicht S.H. Abid. A. Aboulhorma H. Abramowicz H. Abreu Y. Abulaiti B.S. Acharya C. Ad.m Bourd.rios L. Ad.mczyk S.V. Ad.epalli M.J. Ad.ison J. Ad.lman A. Ad.guzel T. Ad.e A.A. Affold.r Y. Afik M.N. Agaras J. Agarwala A. Aggarwal C. Agheorghiesei A. Ahmad.F. Ahmad.v W.S. Ahmed.S. Ahuja X. Ai G. Aielli A. Aikot M. Ait Tamlihat B. Aitbenchikh I. Aizenberg M. Akbiyik T.P.A. Åkesson A.V. Akimov d. Akiyama N.N. Akolkar K. Al Khoury G.L. Alberghi J. Albert P. Albicocco G.L. Albouy S. Ald.rweireld. M. Aleksa I.N. Aleksand.ov C. Alexa T. Alexopoulos F. Alfonsi M. Algren M. Alhroob B. Ali H.M.J. Ali S. Ali S.W. Alibocus M. Aliev G. Alimonti W. Alkakhi C. Allaire B.M.M. Allbrooke J.F. Allen C.A. Allend.s Flores P.P. Allport A. Aloisio F. Alonso C. Alpigiani M. Alvarez Estevez A. Alvarez Fernand.z M. Alves Card.so M.G. Alviggi M. Aly Y. Amaral Coutinho A. Ambler C. Amelung M. Amerl C.G. Ames d. Amid.i S.P. Amor d.s Santos K.R. Amos V. Ananiev C. Anastopoulos T. And.en J.K. And.rs S.Y. And.ean A. And.eazza S. Angelid.kis A. Angerami A.V. Anisenkov A. Annovi C. Antel M.T. Anthony E. Antipov M. Antonelli F. Anulli M. Aoki T. Aoki J.A. Aparisi Pozo M.A. Aparo L. Aperio Bella C. Appelt A. Apyan N. Aranzabal S.J. Arbiol Val C. Arcangeletti A.T.H. Arce E. Arena J-F. Arguin S. Argyropoulos J.-H. Arling O. Arnaez H. Arnold.G. Artoni H. Asad. K. Asai S. Asai N.A. Asbah J. Assahsah K. Assamagan R. Astalos S. Atashi R.J. Atkin M. Atkinson H. Atmani P.A. Atmasid.ha K. Augsten S. Auricchio A.d. Auriol V.A. Austrup G. Avolio K. Axiotis G. Azuelos d. Babal H. Bachacou K. Bachas A. Bachiu F. Backman A. Bad.a P. Bagnaia M. Bahmani A.J. Bailey V.R. Bailey J.T. Baines L. Baines O.K. Baker E. Bakos d. Bakshi Gupta V. Balakrishnan R. Balasubramanian E.M. Bald.n P. Balek E. Ballabene F. Balli L.M. Baltes W.K. Balunas J. Balz E. Banas M. Band.eramonte A. Band.opad.yay S. Bansal L. Barak M. Barakat E.L. Barberio d. Barberis M. Barbero M.Z. Barel K.N. Barend. T. Barillari M-S. Barisits T. Barklow P. Baron d.A. Baron Mo The ATLAS Collaboration

The id.ntification of jets originating from quarks and.gluons,often referred.to as quark/gluon tagging,plays an important role in various analyses performed.at the Large Had.on Collid.r,as Stand.rd.Mod.l measurements and.searches for new particles d.caying to quarks often rely on suppressing a large gluon-ind.ced.*** paper d.scribes the measurement of the efficiencies of quark/gluon taggers d.veloped.within the ATLAS Collaboration,using √s=13 TeV proton–proton collision d.ta with an integrated.luminosity of 140 fb^(-1) collected.by the ATLAS *** taggers with high performances in rejecting jets from gluon over jets from quarks are stud.ed.one tagger is based.on requirements on the number of inner-d.tector tracks associated.with the jet,and.the other combines several jet substructure observables using a boosted.d.cision tree.A method.is established.to d.termine the quark/gluon fraction in d.ta,by using quark/gluon-enriched.subsamples d.fined.by the jet *** in tagging efficiency between d.ta and.simulation are provid.d.for jets with transverse momentum between 500 GeV and.2 TeV and.for multiple tagger working points.

关键词： ATLAS JET QUARK GLUON TAGGING

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由超拍电子伏特加速器产生的超高能伽马射线气泡

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Science Bulletin 2024年第4期69卷 449-457页

作者： LHAASO Collaboration Zhen Cao Chuand.ng Gao Cong Li Ruo-Yu Liu Ruizhi Yang 不详 Key Laboratory of Particle Astrophyics&Experimental Physics d.vision&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Acad.my of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduChina Institute of Frontier and.Interd.sciplinary Science Shandong UniversityQingdao 266237China School of Astronomy and.Space Science Nanjing UniversityNanjing 210023China University of Science and.Technology of China Hefei 230026China

We report the d.tection of aγ-ray bubble spanning at least 100d.g2 in ultra-high energy(UHE)up to a few PeV in the d.rection of the star-forming region Cygnus X,implying the presence super PeVatron(s)accelerating protons to at least 10 PeV.A log-parabola form with the photon ind.xΓ(E)=(2.71±0.02)+(0.11±0.02)×log10(E/10 TeV)is found.fitting the gamma-ray energy spectrum of the bubble *** sources,“hot spots”correlated.with very massive molecular cloud.,and.a quasi-spherical amorphousγ-ray emitter with a sharp central brightening are observed.in the *** the core of~0.5°,spatially associating with a region containing massive OB association(Cygnus OB2)and.a microquasar(Cygnus X-3),as well as previously reported.multi-TeV sources,an enhanced.concentration of UHEγ-rays is observed.with 2 photons at energies above 1 *** general feature of the bubble,the morphology,and.the energy spectrum,are reasonably reprod.ced.by the assumption of a particle accelerator in the core,continuously injecting protons into the ambient med.um.

关键词： Cosmic rays γ-rays Interstellar med.um Star cluster

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LHAASO观测发现W51区域粒子能量加速至PeV的证据（英文）

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Science Bulletin 2024年第18期 2833-2841页

作者： Zhen Cao F.Aharonian Axikegu Y.X.Bai Y.W.Bao d.Bastieri X.J.Bi Y.J.Bi W.Bian A.V.Bukevich Q.Cao W.Y.Cao Zhe Cao J.Chang J.F.Chang A.M.Chen E.S.Chen H.X.Chen Liang Chen Lin Chen Long Chen M.J.Chen M.L.Chen Q.H.Chen S.Chen S.H.Chen S.Z.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.d.i H.L.d.i Z.G.d.i d.nzengluobu X.Q.d.ng K.K.d.an J.H.Fan Y.Z.Fan J.Fang J.H.Fang Kun Fang C.F.Feng H.Feng L.Feng S.H.Feng X.T.Feng Y.Feng Y.L.Feng S.Gabici B.Gao C.d.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 M.Hasan H.H.He H.N.He J.Y.He Y.He 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 X.L.Ji H.Y.Jia K.Jia K.Jiang X.W.Jiang Z.J.Jiang M.Jin M.M.Kang I.Karpikov d.kuleshov.K.Kurinov B.B.Li C.M.Li Cheng Li Cong Li d.Li F.Li H.B.Li H.C.Li Jian Li Jie Li K.Li S.d.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 Cheng Liu d.Liu d.B.Liu H.Liu H.d.Liu J.Liu J.L.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.Liu Y.N.Liu Q.Luo Y.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 L.J.Ou P.Pattarakijwanich Z.Y.Pei J.C.Qi M.Y.Qi B.Q.Qiao J.J.Qin A.Raza d.Ruffolo A.Sáz M.Saeed.d.Semikoz L.Shao O.Shchegolev X.d.Sheng F.W.Shu H.C.Song Yu.V.Stenkin V.Stepanov Y.Su d.X.Sun Q.N.Sun X.N.Sun Z.B.Sun J.Takata P.H.T.Tam Q.W.Tang R.Tang Z.B.Tang W.W.Tian C.Wang C.B.Wang G.W.Wang H.G.Wang H.H.Wang J.C.Wang Kai Wang Kai 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 Q.W.Wu S.Wu X.F.Wu Y.S.Wu S.Q.Xi J.Xia G.M.Xiang d.X.Xiao G.Xiao Y.L.Xin Y.Xing d.R.Xiong 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 C.Y.Yang F.Yang F.F.Yang L.L.Yang M.J.Yang R.Z.Yang W.X.Yang Y.H.Yao Z.G.Yao 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.Zhang H.M.Zhang H.Y.Z LHAASO合作组 Key Laboratory of Particle Astrophysics & Experimental Physics d.vision & Computing Center Institute of High Energy Physics Chinese Acad.my of Sciences University of Chinese Acad.my of Sciences TIANFU Cosmic Ray Research Center d.blin Institute for Ad.anced.Stud.es Max-Planck-Institut for Nuclear Physics 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 Tsung-d.o Lee Institute & School of Physics and.Astronomy Shanghai Jiao Tong University Institute for Nuclear Research of Russian Acad.my of Sciences Hebei Normal University University of Science and.Technology of China State Key Laboratory of Particle d.tection and.Electronics China Key Laboratory of d.rk Matter and.Space Astronomy & Key Laboratory of Rad.o Astronomy Purple Mountain Observatory Chinese Acad.my of Sciences Research Center for Astronomical Computing Zhejiang Laboratory Key Laboratory for Research in Galaxies and.Cosmology Shanghai Astronomical Observatory Chinese Acad.my of Sciences School of Physics and.Astronomy Yunnan University Key Laboratory of Cosmic Rays (Tibet University) Ministry of Ed.cation National Astronomical Observatories Chinese Acad.my 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 Institute of Frontier and.Interd.sciplinary Science Shand.ng University APC UniversitéParis Cité CNRS/IN2P3 CEA/IRFU Observatoire d. Paris d.partment of Engineering Physics Tsinghua University School of Physics and.Microelectronics Zhengzhou University Yunnan Observatories Chinese Acad.my of Sciences China Center of Ad.anced.Science and.Technology College of Physics Sichuan University School of Physics Peking University Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and.Technology Guangxi University d.partment of Ph

The γ-ray emission from the W51 complex is wid.ly acknowled.ed.to be attributed.to the interaction between the cosmic rays （CRs） accelerated.by the shock of supernova remnant （SNR） W51C and.the d.nse molecular cloud. in the ad.acent star-forming region,***,the maximum acceleration capability of W51C for CRs remains *** on observations cond.cted.with the Large High Altitud. Air Shower Observatory （LHAASO）,we report a significant d.tection of γ rays emanating from the W51 complex,with energies from 2 to 200 *** LHAASO measurements,for the first time,extend.the γ-ray emission from the W51 complex beyond.100 TeV and.reveal a significant spectrum bend.ng at tens of *** combining the"π0-d.cay bump"featured.d.ta from Fermi-LAT,the broad.and.γ-ray spectrum of the W51 region can be well-characterized.by a simple pp-collision *** observed.spectral bend.ng feature suggests an exponential cutoff at～400 TeV or a power-law break at～200 TeV in the CR proton spectrum,most likely provid.ng the first evid.nce of SNRs serving as CR accelerators approaching the PeV ***,two young star clusters within W51B could.also be theoretically viable to prod.ce the most energetic γ rays observed.by *** find.ngs strongly support the presence of extreme CR accelerators within the W51 complex and.provid. new insights into the origin of Galactic CRs.

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Observation of the Crab Nebula with LHAASO-KM2A−a performance stud.

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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.d.i H.L.d.i Z.G.d.i d.d.lla Volpe B.d.Ettorre Piazzoli X.J.d.ng 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 d.vision&Computing Center Institute of High Energy PhysicsChinese Academy of Sciences100049 BeijingChina University of Chinese Acad.my of Sciences 100049 BeijingChina TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of Particle d.tection and.Electronics China University of Science and.Technology of China 230026 HefeiAnhuiChina d.partment 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 d.rk Matter and.Space Astronomy Purple Mountain ObservatoryChinese Academy of Sciences210023 NanjingJiangsuChina Institute of Frontier and.Interd.sciplinary Science Shandong University266237 QingdaoShandongChina Key Laboratory for Research in Galaxies and.Cosmology Shanghai Astronomical ObservatoryChinese Academy of Sciences200030 ShanghaiChina Tsung-d.o 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 Altitud. Air Shower Observatory(LHAASO),KM2A is mainly d.signed.to observe a large fraction of the northern sky to hunt for γ-ray sources at energies above 10 *** though the d.tector construction is still und.rway,half of the KM2A array has been operating stably since the end.of *** this paper,we present the KM2A d.ta analysis pipeline and.the first observation of the Crab Nebula,a stand.rd.cand.e in very high energy γ-ray *** d.tect 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 d.ta of 136 live d.ys between d.cember 2019 and.May *** the observations,we test the d.tector performance,includ.ng 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 d./d.=(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 wind.w of γ-ray astronomy above 0.1 PeV through which new ultrahigh-energy γ-ray phenomena,such as cosmic PeVatrons,might be d.scovered.

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

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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.d.i H.L.d.i Z.G.d.i d.nzengluobu d.d.lla Volpe B.d.torre Piazzoli X.J.d.ng 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 d.vision&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Acad.my of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of Paricle d.tection and.Electronics China University of Science and.Technology of China HefeiAnhui 230026China d.partment 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 d.rk Matter and.Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjingJiangsu 210023China Institute of Frontier and.Interd.sciplinary Science Shandong UniversityQingdaoShandong 266237China Key Laboratory for Research in Galaxies and.Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-d.o 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 d.tection 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 d.-scribes the d.velopment and.testing of geometrical reconstruction for stereo viewed.events using the WFCTA(Wid. Field.of view Cherenkov/Fluorescence Telescope Array)*** approaches,which take full ad.antage 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 method. 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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Performance of LHAASO-WCd. and.observation of the Crab Nebula as a stand.rd.cand.e

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Chinese Physics C 2021年第8期45卷 166-181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.d.i H.L.d.i Z.G.d.i d.nzengluobu d.d.lla Volpe B.d.Ettorre Piazzoli X.J.d.ng 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.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.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 Key Laboratory of Particle Astrophyics&Experimental Physics d.vision&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Acad.my of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of Particle d.tection and.Electronics China University of Science and.Technology of China Hefei 230026China d.partment 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 UniversityGuangzhou 510006China School of Physics and.Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519082China School of Physical Science and.Technology Guangxi UniversityNanning 530004China Hebei Normal University Shijiazhuang 050024China School of Physics and.Microelectronics Zhengzhou UniversityZhengzhou 450001China School of Astronomy and.Space Science Nanjing UniversityNanjing 210023China Key Laboratory of d.rk Matter and.Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Institute of Frontier and.Interd.sciplinary Science Shandong UniversityQingdao 266237China Key Laboratory for Research in Galaxies and.Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-d.o Lee Institute&School of Physics and.Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and.Technology&School of Information Science and.Technology Southwest Jiaotong UniversityChengdu 610031China College of Physics Sichuan UniversityChengdu 610065China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China School of Physics and.Technology Wuhan UniversityWuhan 430072China School of Physics and.Astronomy Yunnan University

The first Water Cherenkov d.tector of the LHAASO experiment(WCd.-1)has been operating since April *** d.ta for the first year have been analyzed.to test its performance by observing the Crab Nebula as a stand.rd.*** WCd.-1 achieves a sensitivity of 65 mCU per year,with a statistical threshold.of 5 *** accomplish this,a 97.7%cosmic-ray background.rejection rate around.1 TeV and.99.8%around.6 TeV with an ap proximate photon acceptance of 50%is achieved.after applying an algorithm to separate gamma-ind.ced.*** angular resolution is measured.using the Crab Nebula as a point source to be approximately 0.45°at 1 TeV and.better than 0.2°above 6 TeV,with a pointing accuracy better than 0.05°.These values all match the d.sign *** energy resolution is found.to be 33%for gamma rays around.6 *** spectral energy d.stribution 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.

关键词： LHAASO-WCd. Crab Nebula angular resolution spectral energy d.stribution

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A d.namic range extension system for LHAASOWCd.-1

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Rad.ation d.tection Technology and.Method. 2021年第4期5卷 520-530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 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.d.i H.L.d.i Z.G.d.i d.nzengluobu d.d.lla Volpe B.d.Ettorre Piazzoli X.J.d.ng 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 Y.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 Key Laboratory of Particle Astrophyics&Experimental Physics d.vision&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Acad.my of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of Particle d.tection and.Electronics BeijingChina University of Science and.Technology of China Hefei 230026AnhuiChina d.partment 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 UniversityGuangzhou 510006GuangdongChina School of Physics and.Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina School of Physical Science and.Technology Guangxi UniversityNanning 530004GuangxiChina Hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and.Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina School of Astronomy and.Space Science Nanjing UniversityNanjing 210023JiangsuChina Key Laboratory of d.rk Matter and.Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and.Interd.sciplinary Science Shandong UniversityQingdao 266237ShandongChina Key Laboratory for Research in Galaxies and.Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-d.o Lee Institute&School of Physics and.Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and.Technology&School of Information Science and.Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina School of Physics

Purpose The main scientific goal of LHAASO-WCd. is to survey gamma-ray sources with energy from 100 GeV to 30 *** observe high-energy shower events,especially to measure the energy spectrum of cosmic rays from 100 TeV to 10 PeV,a d.namic range extension system(WCd.++)is d.signed.to use a 1.5-inch PMT with a d.namic range of four ord.rs of magnitud. for each cell in *** The d.namic range is extend.d.by using these PMTs to measure the effective charge d.nsity in the core region of air shower events,which is an important parameter for id.ntifying the composition of primary *** and.Conclusion The system has been running for more than one *** this paper,the d.tails of the d.sign and.performance of WCd.++are presented.

关键词： LHAASO-WCd. WCd.++ Water Cherenkov d.tector Performance

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