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STCF conceptual design report (Volume 1): physics & detector

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Frontiers of physics 2024年第1期19卷 1-154页

作者： m.Achasov x.C.Ai l.p.An R.Aliberti Q.An x.Z.Bai y.Bai O.Bakina A.Barnyakov V.Blinov V.Bobrovnikov D.Bodrov A.Bogomyagkov A.Bondar I.Boyko Z.H.Bu F.m.Cai H.Cai j.j.cao Q.H.cao x.cao Z.cao Q.Chang K.T.Chao D.y.Chen H.Chen H.x.Chen j.F.Chen K.Chen l.l.Chen p.Chen S.l.Chen S.m.Chen S.Chen S.p.Chen W.Chen x.Chen x.F.Chen x.R.Chen y.Chen y.Q.Chen H.y.Cheng j.Cheng S.Cheng T.G.Cheng j.p.Dai l.y.Dai x.C.Dai D.Dedovich A.Denig I.Denisenko j.m.Dias D.Z.Ding l.y.dong W.H.dong V.Druzhinin D.S.Du y.j.Du Z.G.Du l.m.Duan D.Epifanov y.l.Fan S.S.Fang Z.j.Fang G.Fedotovich C.Q.Feng x.Feng y.T.Feng j.l.Fu j.Gao y.n.Gao p.S.Ge C.Q.Geng l.S.Geng A.Gilman l.Gong T.Gong B.Gou W.Gradl j.l.gu A.guevara l.C.gui A.Q.guo F.K.guo j.C.guo j.guo y.p.guo Z.H.guo A.guskov K.l.Han l.Han m.Han x.Q.Hao j.B.He S.Q.He x.G.He y.l.He Z.B.He Z.x.Heng B.l.Hou T.j.Hou y.R.Hou C.y.Hu H.m.Hu K.Hu R.j.Hu W.H.Hu x.H.Hu y.C.Hu j.Hua G.S.Huang j.S.Huang m.Huang Q.y.Huang W.Q.Huang x.T.Huang x.j.Huang y.B.Huang y.S.Huang n.Hüsken V.Ivanov Q.p.ji j.j.jia S.jia Z.K.jia H.B.jiang j.jiang S.Z.jiang j.B.jiao Z.jiao H.j.jing x.l.Kang x.S.Kang B.C.Ke m.Kenzie A.Khoukaz I.Koop E.Kravchenko A.Kuzmin y.lei E.levichev C.H.li C.li D.y.li F.li G.li G.li H.B.li H.li H.n.li H.j.li H.l.li j.m.li j.li l.li l.li l.y.li n.li p.R.li R.H.li S.li T.li W.j.li x.li x.H.li x.Q.li x.H.li y.li y.y.li Z.j.li H.liang j.H.liang y.T.liang G.R.liao l.Z.liao y.liao C.x.lin D.x.lin x.S.lin B.j.liu C.W.liu D.liu F.liu G.m.liu H.B.liu j.liu j.j.liu j.B.liu K.liu K.y.liu K.liu l.liu Q.liu S.B.liu T.liu x.liu y.W.liu y.liu y.l.liu Z.Q.liu Z.y.liu Z.W.liu I.logashenko y.long C.G.lu j.x.lu n.lu Q.F.lü y.lu y.lu Z.lu p.lukin F.j.luo T.luo x.F.luo y.H.luo H.j.lyu x.R.lyu j.p.ma p.ma y.ma y.m.ma F.maas S.malde D.matvienko Z.x.meng R.mitchell A.nefediev y.nefedov S.l.Olsen Q.Ouyang p.pakhlov G.pakhlova x.pan y.pan E.passemar y.p.pei H.p.peng l.peng x.y.peng x.j.peng K.peters S.pivovarov E.pyata B.B.Qi y.Q.Qi W.B.Qian y.Qian C.F.Qiao j.j.Qin j.j.Qin l.Q.Qin x.S.Qin T.l.Qiu j.Rademacker C.F.Redmer H.y.Sang Anhui University Hefei 230039China Beihang University Beijing 100191China Budker Institute of nuclear physics Novosibirsk 630090Russia CAS Key laboratory of Theoretical physics Institute of Theoretical PhysicsChinese Academy of SciencesBeijing 100190China Cavendish laboratory University of CambridgeJJ Thomson AveCambridge CB30HEUnited Kingdom Central China normal University Wuhan 430079China Central South University Changsha 410083China China University of Geosciences Wuhan 430074China China University of mining and Technology Xuzhou 221116China École polytechnique Fédérale de lausanne(EpFl) LausanneSwitzerland Fudan University Shanghai 200433China Goethe University Frankfurt D-60325 Frankfurt am MainGermany guangxi normal University Guilin 541004China guangxi Uninversity Nanning 530004China Hangzhou Institute for Advanced Study UCASHangzhou 310024China Hebei normal University Shijiazhuang 050024China Hebei University Baoding 071002China Hefei University of Technology Hefei 230601China Helmholtz Institute mainz Staudinger Weg 18D-55099 MainzGermany Henan normal University Xinxiang 453007China Henan University Kaifeng 475004China High Energy physics Center Chung-Ang UniversitySeoul 06974Korea Higher School of Economy 11 pokrovsky Bulvar Moscow 109028Russia Huangshan University Huangshan 245000China Hubei University of Automotive Technology Shiyan 442002China Hunan normal University Changsha 410081China Hunan University of Science and Technology Xiangtan 411201China Hunan University Changsha 410082China Indiana University BloomingtonIndiana 47405USA Inner mongolia University Hohhot 010021China Institute of Advanced Science Facilities Shenzhen 518107China Institute of High Energy physics Chinese Academy of SciencesBeijing 100049China Institute of modern physics Chinese Academy of SciencesLanzhou 730000China Institute of physics Academia SinicaTaipeiTaiwan 11529China Institute of Theoretical physics Chinese Academy of SciencesBeijing 100190China jilin University Changch

The superτ-charm facility(STCF)is an electron–positron collider proposed by the Chinese particle physics *** is designed to operate in a center-of-mass energy range from 2 to 7 GeV with a peak luminosity of 0.5×10^(35) cm^(–2)·s^(–1) or *** STCF will produce a data sample about a factor of 100 larger than that of the presentτ-charm factory—the BEpCII,providing a unique platform for exploring the asymmetry of matter-antimatter(charge-parity violation),in-depth studies of the internal structure of hadrons and the nature of non-perturbative strong interactions,as well as searching for exotic hadrons and physics beyond the Standard *** STCF project in China is under development with an extensive R&D *** document presents the physics opportunities at the STCF,describes conceptual designs of the STCF detector system,and discusses future plans for detector R&D and physics case studies.

关键词： electron–positron collider tau-charm region high luminosity STCF detector conceptual design

Amplitude analysis of the decays D^(0)→π^(+)π^(−)π^(+)π^(−)and D^(0)→π^(+)π^(−)π^(0)π^(0)

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Chinese physics C 2024年第8期48卷 6-33页

作者： m.Ablikim m.n.Achasov p.Adlarson O.Afedulidis x.C.Ai R.Aliberti A.Amoroso Q.An y.Bai O.Bakina I.Balossino y.Ban H.-R.Bao V.Batozskaya K.Begzsuren n.Berger m.Berlowski m.Bertani D.Bettoni F.Bianchi E.Bianco A.Bortone I.Boyko R.A.Briere A.Brueggemann H.Cai x.Cai A.Calcaterra G.F.cao n.cao S.A.Cetin j.F.Chang W.l.Chang G.R.Che G.Chelkov C.Chen C.H.Chen Chao Chen G.Chen H.S.Chen m.l.Chen S.j.Chen S.l.Chen S.m.Chen T.Chen x.R.Chen x.T.Chen y.B.Chen y.Q.Chen Z.j.Chen Z.y.Chen S.K.Choi x.Chu G.Cibinetto F.Cossio j.j.Cui H.l.Dai j.p.Dai A.Dbeyssi R.E.de Boer D.Dedovich C.Q.Deng Z.y.Deng A.Denig I.Denysenko m.Destefanis F.De mori B.Fang S.S.Fang W.x.Fang y.Fang y.Q.Fang R.Farinelli l.Fava F.Feldbauer G.Felici C.Q.Feng j.H.Feng y.T.Feng K.Fischer m.Fritsch C.D.Fu j.l.Fu y.W.Fu H.Gao y.n.Gao yang Gao S.Garbolino I.Garzia p.T.Ge Z.W.Ge C.Geng E.m.Gersabeck B.Ding x.x.Ding y.Ding y.Ding j.dong l.y.dong m.y.dong x.dong m.C.Du S.x.Du Z.H.Duan p.Egorov y.H.Fan j.Fang jA.Gilman K.Goetzen l.Gong W.x.Gong W.Gradl S.Gramigna m.Greco m.H.gu y.T.gu C.y.guan Z.l.guan A.Q.guo l.B.guo m.j.guo R.p.guo y.p.guo A.guskov j.gutierrez K.l.Han T.T.Han x.Q.Hao F.A.Harris K.K.He K.l.He F.H.Heinsius C.H.Heinz y.K.Heng C.Herold T.Holtmann p.C.Hong G.y.Hou x.T.Hou y.R.Hou Z.l.Hou B.y.Hu H.m.Hu j.F.Hu T.Hu y.Hu G.S.Huang K.x.Huang l.Q.Huang x.T.Huang y.p.Huang T.Hussain F.H\"olzken n.H\"usken n.in der Wiesche m.Irshad j.jackson S.janchiv j.H.jeong Q.ji Q.p.ji W.ji x.B.ji x.l.ji y.y.ji x.Q.jia Z.K.jia D.jiang H.B.jiang p.C.jiang S.S.jiang T.j.jiang x.S.jiang y.jiang j.B.jiao j.K.jiao Z.jiao S.jin y.jin m.Q.jing x.m.jing T.johansson S.Kabana n.Kalantar-nayestanaki x.l.Kang x.S.Kang m.Kavatsyuk B.C.Ke V.Khachatryan A.Khoukaz R.Kiuchi O.B.Kolcu B.Kopf m.Kuessner x.Kui A.Kupsc W.K\"uhn j.j.lane p.larin l.lavezzi T.T.lei Z.H.lei H.leithoff m.lellmann T.lenz C.li C.li C.H.li Cheng li D.m.li F.li G.li H.li H.B.li H.j.li H.n.li Hui li j.R.li j.S.li K.li l.j.li l.K.li lei li m.H.li p.R.li Q.m.li Q.x.li R.li S.x.li T.li W.D.li W.G.li x.li x.H.li x.l.li x.y.li y Institute of High Energy physics Chinese Academy of SciencesBeijing 100049China Beihang University Beijing 100191China Bochum Ruhr-University D-44780 BochumGermany Budker Institute of nuclear physics SB RAS(BInp) Novosibirsk 630090Russia Carnegie mellon University PittsburghPennsylvania 15213USA Central China normal University Wuhan 430079China Central South University Changsha 410083China China Center of Advanced Science and Technology Beijing 100190China China University of Geosciences Wuhan 430074China Chung-Ang University Seoul06974Republic of Korea COmSATS University Islamabad Lahore CampusDefence RoadOff Raiwind Road54000 LahorePakistan Fudan University Shanghai 200433China GSI Helmholtzcentre for Heavy Ion Research GmbH D-64291 DarmstadtGermany guangxi normal University Guilin 541004China guangxi University Nanning 530004China Hangzhou normal University Hangzhou 310036China Hebei University Baoding 071002China Helmholtz Institute mainz Staudinger Weg 18D-55099 MainzGermany Henan normal University Xinxiang 453007China Henan University Kaifeng 475004China Henan University of Science and Technology Luoyang 471003China Henan University of Technology Zhengzhou 450001China Huangshan College Huangshan 245000China Hunan normal University Changsha 410081China Hunan University Changsha 410082China Indian Institute of Technology madras Chennai 600036India Indiana University BloomingtonIndiana 47405USA InFn laboratori nazionali di Frascati INFN Laboratori Nazionali di FrascatiI-00044FrascatiItaly InFn laboratori nazionali di Frascati INFN Sezione di PerugiaI-06100PerugiaItaly InFn laboratori nazionali di Frascati University of PerugiaI-06100PerugiaItaly InFn Sezione di Ferrara INFN Sezione di FerraraI-44122FerraraItaly InFn Sezione di Ferrara University of FerraraI-44122FerraraItaly Inner mongolia University Hohhot 010021China Institute of modern physics Lanzhou 730000China Institute of physics and Technology Peace Avenue 54BUlaanbaatar 13330Mongolia Instituto de A

Using e^(+)e^(−)annihilation data corresponding to an integrated luminosity of 2.93 fb^(−1)taken at the center-of-mass energy√s=3.773 GeV with the BESIII detector,a joint amplitude analysis is performed on the decays D^(0)→π^(+)π^(−)π^(+)π^(−)and D^(0)→π^(+)π^(−)π^(0)π^(0)(non-η).The fit fractions of individual components are obtained,and large interferences among the dominant components of the decays D^(0)→a_(1)(1260)π,D^(0)→π(1300)π,D^(0)→ρ(770)ρ(770),and D^(0)→2(ππ)_(S)are observed in both *** the obtained amplitude model,the Cp-even fractions of D^(0)→π^(+)π^(−)π^(+)π^(−)and D^(0)→π^(+)π^(−)π^(0)π^(0)(non-η)are determined to be(75.2±1.1_(stat).±1.5_(syst.))%and(68.9±1.5_(stat).±2.4_(syst.))%,*** branching fractions of D^(0)→π^(+)π^(−)π^(+)π^(−)and D^(0)→π^(+)π^(−)π^(0)π^(0)(non-η)are measured to be(0.688±0.010_(stat.)±0.010_(syst.))%and(0.951±0.025_(stat.)±0.021_(syst.))%,*** amplitude analysis provides an important model for the binning strategy in measuring the strong phase parameters of D^(0)→4πwhen used to determine the CKm angleγ(ϕ_(3))via the B^(−)→DK^(−)decay.

关键词： BESIII D^(0)meson decays amplitude analysis Cp-even fraction

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 Chuandong Gao Cong li Ruo-yu liu Ruizhi yang 不详 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 ChengduChina Institute of Frontier and Interdisciplinary 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 detection of aγ-ray bubble spanning at least 100deg2 in ultra-high energy(UHE)up to a few peV in the direction 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 indexΓ(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 clouds,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 reproduced by the assumption of a particle accelerator in the core,continuously injecting protons into the ambient medium.

关键词： Cosmic rays γ-rays Interstellar medium Star cluster

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

large-scale interplant exchange of macromolecules between soybean and dodder under nutrient stresses

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plant Diversity 2024年第1期46卷 116-125页

作者： jingxiong zhang Shalan li Wenxing li Zerui Feng Shuhan zhang xijie Zheng yuxing xu guojing Shen man Zhao guoyan cao xuna Wu jianqiang Wu Department of Economic plants and Biotechnology Yunnan Key Laboratory for Wild Plant ResourcesKunming Institute of BotanyChinese Academy of SciencesKunming 650201China CAS Center for Excellence in Biotic Interactions University of Chinese Academy of SciencesBeijing 100049China State Key laboratory of Conservation and Utilization of Bio-Resources in yunnan and Center for life Science School of Life SciencesYunnan UniversityKunming 650500China

parasitic plants and their hosts communicate through haustorial *** deficiency is a common stress for plants,yet little is known about whether and how host plants and parasites communicate during adaptation to such nutrient *** this study,we used transcriptomics and proteomics to analyze how soybean(Glycine max)and its parasitizing dodder(Cuscuta australis)respond to nitrate and phosphate deficiency(-n and-p).After-n and-p treatment,the soybean and dodder plants exhibited substantial changes of transcriptome and proteome,although soybean plants showed very few transcriptional responses to-p and dodder did not show any transcriptional changes to either-n ***,large-scale interplant transport of mRnAs and proteins was *** the mobile mRnAs only comprised at most 0.2%of the transcriptomes,the foreign mobile proteins could reach 6.8%of the total proteins,suggesting that proteins may be the major forms of interplant ***,the interplant mobility of macromolecules was specifically affected by the nutrient regimes and the transport of these macromolecules was very likely independently *** study provides new insight into the communication between host plants and parasites under stress conditions.

关键词： Cuscuta mobile molecules nutrient deficiency Host plant-parasitic plant interaction Interplant transport Systemic signaling

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

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

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 2019 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

Observation of the y(4230)and a new structure in e^(+)e^(-)→K^(+)K^(-)j/Ψ

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Chinese physics C 2022年第11期46卷 7-21页

作者：麦迪娜 m.n.Achasov p.Adlarson m.Albrecht R.Aliberti A.Amoroso 安美儒安琪白旭红白羽 O.Bakina R.Baldini Ferroli I.Balossino 班勇 V.Batozskaya D.Becker K.Begzsuren n.Berger m.Bertani D.Bettoni F.Bianchi j.Bloms A.Bortone I.Boyko R.A.Briere A.Brueggemann 蔡浩蔡啸 A.Calcaterra 曹国富曹宁 S.A.Cetin 常劲帆常万玲 G.Chelkov 陈琛陈刚陈和生陈玛丽陈申见 T.Chen 陈旭荣 x.T.Chen 陈元柏陈卓俊成伟帅初晓 G.Cibinetto F.Cossio 崔佳佳代洪亮代建平 A.Dbeyssi R.Ede Boer D.Dedovich 邓子艳 A.Denig I.Denysenko m.Destefanis F.De mori 丁勇董静董燎原董明义董翔杜书先 p.Egorov 范玉兰方建房双世方文兴方易 R.Farinelli l.Fava F.Feldbauer G.Felici 封常青冯俊华 K.Fischer m.Fritsch C.Fritzsch 傅成栋高涵高原宁高扬 S.Garbolino I.Garzia 葛潘婷耿聪 E.m.Gersabeck A Gilman K.Goetzen 龚丽龚文煊 W.Gradl m.Greco 顾旻皓关春懿郭爱强郭立波郭如盼郭玉萍 A.guskov 韩婷婷韩文颖郝喜庆 F.A.Harris 何凯凯何康林 F.H.Heinsius C.H.Heinz 衡月昆 C.Herold m.Himmelreich T.Holtmann 侯国一侯颖锐侯治龙胡海明 j.F.Hu 胡涛胡誉黄光顺黄凯旋黄麟钦黄麟钦黄性涛黄燕萍 Z.Huang T.Hussain n Hüsken W.Imoehl m.Irshad j.jackson S.jaeger S.janchiv Q.ji 姬清平季晓斌季筱璐吉钰瑶贾泽坤姜侯兵姜赛赛江晓山 y.jiang 焦健斌焦铮金山金毅荆茂强 T.johansson n.Kalantar-nayestanaki 康晓珅 R.Kappert m.Kavatsyuk 柯百谦 I.K.Keshk A.Khoukaz p.Kiese R.Kiuchi R.Kliemt l.Koch O.B.Kolcu B.Kopf m.Kuemmel m.Kuessner A.Kupsc W.Kühn j.j.lane j.S.lange p.larin A.lavania l.lavezzi 雷祚弘 H.leithoff m.lellmann T.lenz 李聪李翠李春花李澄李德民李飞李刚李贺 H.li 李海波李惠静 H.n.li j.Q.li 李静舒李井文李科 l.j li 李龙科李蕾李明浩李培荣李素娴栗帅迎李腾李卫东李卫国李旭红李晓玲李晓宇李紫源梁浩梁昊梁浩梁勇飞梁羽铁廖广睿廖龙洲 j.libby A.limphirat C.x.lin 林德旭 T.lin 刘北江刘春秀 D.liu 刘福虎刘芳刘峰 G.m.liu H.liu 刘怀民刘欢欢刘汇慧刘建北刘佳俊刘晶译刘凯刘魁勇刘珂刘亮刘美宏刘佩莲刘倩刘树彬刘桐刘维克刘卫民刘翔刘英刘玉斌刘振安刘智青娄辛丑卢飞翔吕海江吕军光陆小玲卢宇卢云鹏卢泽辉罗成林罗民兴罗涛罗小兰吕晓睿吕翌丰马凤才马海龙马连良马明明马秋梅马润秋马瑞廷马骁妍马尧 FEmaas m.maggiora S.maldaner S.malde Q.A.malik A.mangoni 冒亚军毛泽普 S.marcello 孟召霞 j.G.messchendorp G.mezzadri H.miao 闵天觉 R.E.mitchell 莫晓虎 n.yu.muchnoi H.muramatsu y.nefedov F.nerling I.B.nikolaev 宁哲 S.nisar 牛艳 S.l.Olsen 欧阳群 S.pacetti 潘祥 y.pan A.pathak A.pathak m.pelizaeus 彭海平 K.peters j.pettersson 平加伦平荣刚 S.plura S.pogodin R.poling V.prasad 齐法制齐航漆红荣祈鸣齐天钰钱森钱文斌钱圳乔从丰秦佳佳秦丽清覃潇平秦小帅秦中华邱进发屈三强 S.Q.Qu Institute of High Energy physics Beijing 100049China Beihang University Beijing 100191China Beijing Institute of petrochemical Technology Beijing 102617China Bochum Ruhr-University D-44780 BochumGermany Carnegie mellon University PittsburghPennsylvania 15213USA Central China normal University Wuhan 430079China China Center of Advanced Science and Technology Beijing 100190China COmSATS University Islamabad Lahore CampusDefence RoadOff Raiwind Road54000 LahorePakistan Fudan University Shanghai 200433China G.I.Budker Institute of nuclear physics SB RAS(BInp) Novosibirsk 630090Russia GSI Helmholtzcentre for Heavy Ion Research GmbH D-64291 DarmstadtGermany guangxi normal University Guilin 541004China Hangzhou normal University Hangzhou 310036China Helmholtz Institute mainz Staudinger Weg 18D-55099 MainzGermany Henan normal University Xinxiang 453007China Henan University of Science and Technology Luoyang 471003China Henan University of Technology Zhengzhou 450001China Huangshan College Huangshan 245000China Hunan normal University Changsha 410081China Hunan University Changsha 410082China Indian Institute of Technology madras Chennai 600036India Indiana University BloomingtonIndiana 47405USA InFn laboratori nazionali di Frascati INFN Laboratori Nazionali di FrascatiI-00044FrascatiItaly InFn laboratori nazionali di Frascati INFN Sezione di PerugiaI-06100PerugiaItaly InFn laboratori nazionali di Frascati University of PerugiaI-06100PerugiaItaly InFn Sezione di Ferrara INFN Sezione di FerraraI-44122FerraraItaly InFn Sezione di Ferrara University of FerraraI-44122FerraraItaly Institute of modern physics Lanzhou 730000China Institute of physics and Technology Peace Ave.54BUlaanbaatar 13330Mongolia jilin University Changchun 130012China johannes gutenberg University of mainz Johann-Joachim-Becher-Weg 45D-55099 MainzGermany joint Institute for nuclear Research 141980 DubnaMoscow regionRussia justus-liebig-Universitaet Giessen II.Physikalisches InstitutHeinrich-Buff-Ring 16

The cross sections of e^(+)e^(-)→K^(+)K^(-)j/Ψat center-of-mass energies from 4.127 to 4.600 GeV are measured based on 15.6 fb-1data collected with the BESⅢ detector operating at the BEpCⅡ storage *** resonant structures are observed in the line shape of the cross *** mass and width of the first structure are measured to be(4225.3±2.3±21.5)meV and(72.9±6.1±30.8)meV,*** are consistent with those of the established y(4230).The second structure is observed for the first time with a statistical significance greater than 8σ,denoted as y(4500).Its mass and width are determined to be(4484.7±13.3±24.1)meV and(111.1±30.1±15.2)meV,*** first presented uncertainties are statistical and the second ones are *** product of the electronic partial width with the decay branching fractionΓ(y(4230)→e^(+)e^(−))B(y(4230)→K^(+)K^(−)j/Ψ)is reported.

关键词： y states charmonium-like states BESⅢ