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| 1 | Future Physics Programme of BESⅢ显示文摘There has recently been a dramatic renewal of interest in hadron spectroscopy and charm physics. This renaissance has been driven in part by the discovery of a plethora of charmonium-like XYZ states at BESⅢ and B factories, and the observation of an intriguing proton-antiproton threshold enhancement and the possibly related X(1835) meson state at BESⅢ, as well as the threshold measurements of charm mesons and charm baryons. We present a detailed survey of the important topics in tau-charm physics and hadron physics that can be further explored at BESⅢ during the remaining operation period of BEPCⅡ. This survey will help in the optimization of the data-taking plan over the coming years, and provides physics motivation for the possible upgrade of BEPCⅡ to higher luminosity. | M.Ablikim M.N.Achasov P.Adlarson S.Ahmed M.Albrecht M.Alekseev A.Amoroso F.F.An Q.An Y.Bai O.Bakina R.Baldini Ferroli Y.Ban K.Begzsuren J.V.Bennett N.Berger M.Bertani D.Bettoni F.Bianchi J Biernat J.Bloms I.Boyko R.A.Briere L.Calibbi H.Cai X.Cai A.Calcaterra G.F.Cao N.Cao S.A.Cetin J.Chai J.F.Chang W.L.Chang J.Charles G.Chelkov Chen G.Chen H.S.Chen J.C.Chen M.L.Chen S.J.Chen Y.B.Chen H.Y.Cheng W.Cheng G.Cibinetto F.Cossio X.F.Cui H.L.Dai J.P.Dai X.C.Dai A.Dbeyssi D.Dedovich Z.Y.Deng A.Denig Denysenko M.Destefanis S.Descotes-Genon F.De Mori Y.Ding C.Dong J.Dong L.Y.Dong M.Y.Dong Z.L.Dou S.X.Du S.I.Eidelman J.Z.Fan J.Fang S.S.Fang Y.Fang R.Farinelli L.Fava F.Feldbauer G.Felici C.Q.Feng M.Fritsch C.D.Fu Y.Fu Q.Gao X.L.Gao Y.Gao Y.Gao Y.G.Gao Z.Gao B.Garillon I.Garzia E.M.Gersabeck A.Gilman K.Goetzen L.Gong W.X.Gong W.Gradl M.Greco L.M.Gu M.H.Gu Y.T.Gu A.Q.Guo F.K.Guo L.B.Guo R.P.Guo Y.P.Guo A.Guskov S.Han X.Q.Hao F.A.Harris K.L.He F.H.Heinsius T.Held Y.K.Heng Y.R.Hou Z.L.Hou H.M.Hu J.F.Hu T.Hu Y.Hu G.S.Huang J.S.Huang X.T.Huang X.Z.Huang Z.L.Huang N.Huesken T.Hussain W.Ikegami Andersson W.Imoehl M.Irshad Q.Ji Q.P.Ji X.B.Ji X.L.Ji H.L.Jiang X.S.Jiang X.Y.Jiang J.B.Jiao Z.Jiao D.P.Jin S.Jin Y.Jin T.Johansson N.Kalantar-Nayestanaki X.S.Kang R.Kappert M.Kavatsyuk B.C.Ke I.K.Keshk T.Khan A.Khoukaz P.Kiese R.Kiuchi R.Kliemt L.Koch O.B.Kolcu B.Kopf M.Kuemmel M.Kuessner A.Kupsc M.Kurth M.G.Kurth W.Kuhn J.S.Lange P.Larin L.Lavezzi H.Leithoff T.Lenz C.Li Cheng Li D.M.Li F.Li F.Y.Li G.Li H.B.Li H.J.Li J.C.Li J.W.Li Ke Li L.K.Li Lei Li P.L.Li P.R.Li Q.Y.Li W.D.Li W.G.Li X.H.Li X.L.Li X.N.Li X.Q.Li Z.B.Li H.Liang H.Liang Y.F.Liang Y.T.Liang G.R.Liao L.Z.Liao J.Libby C.X.Lin D.X.Lin Y.J.Lin B.Liu B.J.Liu C.X.Liu D.Liu D.Y.Liu F.H.Liu Fang Liu Feng Liu H.B.Liu H.M.Liu Huanhuan Liu Huihui Liu J.B.Liu J.Y.Liu K.Y.Liu Ke Liu Q.Liu S.B.Liu T.Liu X.Liu X.Y.Liu Y.B.Liu Z.A.Liu Zhiqing Liu Y.F.Long X.C.Lou H.J.Lu J.D.Lu J.G.Lu Y.Lu Y.P.Lu C.L.Luo M.X.Luo P.W.Luo T.Luo X.L.Luo S.Lusso X.R.Lyu F.C.Ma H.L.Ma L.L.Ma M.M.Ma Q.M.Ma X.N.Ma X.X.Ma X.Y.Ma Y.M.Ma F.E.Maas M.Maggiora S.Maldaner S.Malde Q.A.Malik A.Mangoni Y.J.Mao Z.P.Mao S.Marcello Z.X.Meng J.G.Messchendorp G.Mezzadri J.Min T.J.Min R.E.Mitchell X.H.Mo Y.J.Mo C.Morales Morales N.Yu.Muchnoi H.Muramatsu A.Mustafa S.Nakhoul Y.Nefedov F.Nerling I.B.Nikolaev Z.Ning S.Nisar S.L.Niu S.L.Olsen Q.Ouyang S.Pacetti Y.Pan M.Papenbrock P.Patteri M.Pelizaeus H.P.Peng K.Peters A.A.Petrov J.Pettersson J.L.Ping R.G.Ping A.Pitka R.Poling V.Prasad M.Qi T.Y.Qi S.Qian C.F.Qiao N.Qin X.P.Qin X.S.Qin Z.H.Qin J.F.Qiu S.Q.Qu K.H.Rashid C.F.Redmer M.Richter M.Ripka A.Rivetti V.Rodin M.Rolo G.Rong J.L.Rosner Ch.Rosner M.Rump A.Sarantsev M.Savrie K.Schoenning W.Shan X.Y.Shan M.Shao C.P.Shen P.X.Shen X.Y.Shen H.Y.Sheng X.Shi X.D Shi J.J.Song Q.Q.Song X.Y.Song S.Sosio C.Sowa S.Spataro F.F.Sui G.X.Sun J.F.Sun L.Sun S.S.Sun X.H.Sun Y.J.Sun Y.K Sun Y.Z.Sun Z.J.Sun Z.T.Sun Y.T Tan C.J.Tang G.Y.Tang X.Tang V.Thoren B.Tsednee I.Uman B.Wang B.L.Wang C.W.Wang D.Y.Wang H.H.Wang K.Wang L.L.Wang L.S.Wang M.Wang M.Z.Wang Wang Meng P.L.Wang R.M.Wang W.P.Wang X.Wang X.F.Wang X.L.Wang Y.Wang Y.F.Wang Z.Wang Z.G.Wang Z.Y.Wang Zongyuan Wang T.Weber D.H.Wei P.Weidenkaff H.W.Wen S.P.Wen U.Wiedner G.Wilkinson M.Wolke L.H.Wu L.J.Wu Z.Wu L.Xia Y.Xia S.Y.Xiao Y.J.Xiao Z.J.Xiao Y.G.Xie Y.H.Xie T.Y.Xing X.A.Xiong Q.L.Xiu G.F.Xu L.Xu Q.J.Xu W.Xu X.P.Xu F.Yan L.Yan W.B.Yan W.C.Yan Y.H.Yan H.J.Yang H.X.Yang L.Yang R.X.Yang S.L.Yang Y.H.Yang Y.X.Yang Yifan Yang Z.Q.Yang M.Ye M.H.Ye J.H.Yin Z.Y.You B.X.Yu C.X.Yu J.S.Yu C.Z.Yuan X.Q.Yuan Y.Yuan A.Yuncu A.A.Zafar Y.Zeng B.X.Zhang B.Y.Zhang C.C.Zhang D.H.Zhang H.H.Zhang H.Y.Zhang J.Zhang J.L.Zhang J.Q.Zhang J.W.Zhang J.Y.Zhang J.Z.Zhang K.Zhang L.Zhang S.F.Zhang T.J.Zhang X.Y.Zhang Y.Zhang Y.H.Zhang Y.T.Zhang Yang Zhang Yao Zhang Yi Zhang Yu Zhang Z.H.Zhang Z.P.Zhang Z.Q.Zhang Z.Y.Zhang G.Zhao J.W.Zhao J.Y.Zhao J.Z.Zhao Lei Zhao Ling Zhao M.G.Zhao Q.Zhao S.J.Zhao T.C.Zhao Y.B.Zhao Z.G.Zhao A.Zhemchugov B.Zheng J.P.Zheng Y.Zheng Y.H.Zheng B.Zhong L.Zhou L.P.Zhou Q.Zhou X.Zhou X.K.Zhou Xingyu Zhou Xiaoyu Zhou Xu Zhou A.N.Zhu J.Zhu J.Zhu K.Zhu K.J.Zhu S.H.Zhu W.J.Zhu X.L.Zhu Y.C.Zhu Y.S.Zhu Z.A.Zhu J.Zhuang B.S.Zou J.H.Zou 无 | 2020 | Chinese Physics C2020，44，4： | 517 |
| 2 | Study of BESIII trigger efficiencies with the 2018 J/ψ data显示文摘Using a dedicated data sample taken in 2018 on the J/ψpeak,we perform a detailed study of the trigger efficiencies of the BESIII detector.The efficiencies are determined from three representative physics processes,namely Bhabha scattering,dimuon production and generic hadronic events with charged particles.The combined efficiency of all active triggers approaches 100%in most cases,with uncertainties small enough not to affect most physics analyses. | M.Ablikim M.N.Achasov P.Adlarson S.Ahmed M.Albrecht R.Aliberti A.Amoroso M.R.An Q.An X.H.Bai Y.Bai O.Bakina R.Baldini Ferroli I.Balossino Y.Ban K.Begzsuren N.Berger M.Bertani D.Bettoni F.Bianchi J.Bloms A.Bortone I.Boyko R.A.Briere H.Cai X.Cai A.Calcaterra G.F.Cao N.Cao S.A.Cetin J.F.Chang W.L.Chang G.Chelkov D.Y.Chen G.Chen H.S.Chen M.L.Chen S.J.Chen X.R.Chen Y.B.Chen Z.J Chen W.S.Cheng G.Cibinetto F.Cossio X.F.Cui H.L.Dai X.C.Dai A.Dbeyssi R.E.de Boer D.Dedovich Z.Y.Deng A.Denig I.Denysenko M.Destefanis F.De Mori Y.Ding C.Dong J.Dong L.Y.Dong M.Y.Dong X.Dong S.X.Du Y.L.Fan J.Fang S.S.Fang Y.Fang R.Farinelli L.Fava F.Feldbauer G.Felici C.Q.Feng J.H.Feng M.Fritsch C.D.Fu Y.Gao Y.Gao Y.Gao Y.G.Gao I.Garzia P.T.Ge C.Geng E.M.Gersabeck A Gilman K.Goetzen L.Gong W.X.Gong W.Gradl M.Greco L.M.Gu M.H.Gu S.Gu Y.T.Gu C.Y Guan A.Q.Guo L.B.Guo R.P.Guo Y.P.Guo A.Guskov T.T.Han W.Y.Han X.Q.Hao F.A.Harris H Hüsken K.L.He F.H.Heinsius C.H.Heinz T.Held Y.K.Heng C.Herold M.Himmelreich T.Holtmann Y.R.Hou Z.L.Hou H.M.Hu J.F.Hu T.Hu Y.Hu G.S.Huang L.Q.Huang X.T.Huang Y.P.Huang Z.Huang T.Hussain W.Ikegami Andersson W.Imoehl M.Irshad S.Jaeger S.Janchiv Q.Ji Q.P.Ji X.B.Ji X.L.Ji H.B.Jiang X.S.Jiang J.B.Jiao Z.Jiao S.Jin Y.Jin T.Johansson N.Kalantar-Nayestanaki X.S.Kang R.Kappert M.Kavatsyuk B.C.Ke I.K.Keshk A.Khoukaz P.Kiese R.Kiuchi R.Kliemt L.Koch O.B.Kolcu B.Kopf M.Kuemmel M.Kuessner A.Kupsc M.G.Kurth W.Kühn J.J.Lane J.S.Lange P.Larin A.Lavania L.Lavezzi Z.H.Lei H.Leithoff M.Lellmann T.Lenz C.Li C.H.Li Cheng Li D.M.Li F.Li G.Li H.Li H.Li H.B.Li H.J.Li J.L.Li J.Q.Li J.S.Li Ke Li L.K.Li Lei Li P.R.Li S.Y.Li W.D.Li W.G.Li X.H.Li X.L.Li Z.Y.Li H.Liang H.Liang H.Liang Y.F.Liang Y.T.Liang L.Z.Liao J.Libby C.X.Lin B.J.Liu C.X.Liu D.Liu F.H.Liu Fang Liu Feng Liu H.B.Liu H.M.Liu Huanhuan Liu Huihui Liu J.B.Liu J.L.Liu J.Y.Liu K.Liu K.Y.Liu Ke Liu L.Liu M.H.Liu P.L.Liu Q.Liu Q.Liu S.B.Liu Shuai Liu T.Liu W.M.Liu X.Liu Y.Liu Y.B.Liu Z.A.Liu Z.Q.Liu X.C.Lou F.X.Lu H.J.Lu J.D.Lu J.G.Lu X.L.Lu Y.Lu Y.P.Lu C.L.Luo M.X.Luo b P.W.Luo T.Luo X.L.Luo S.Lusso X.R.Lyu F.C.Ma H.L.Ma L.L.Ma M.M.Ma Q.M.Ma R.Q.Ma R.T.Ma X.X.Ma X.Y.Ma F.E.Maas M.Maggiora S.Maldaner S.Malde Q.A.Malik A.Mangoni Y.J.Mao Z.P.Mao S.Marcello Z.X.Meng J.G.Messchendorp G.Mezzadri T.J.Min R.E.Mitchell X.H.Mo Y.J.Mo N.Yu.Muchnoi H.Muramatsu S.Nakhoul Y.Nefedov F.Nerling I.B.Nikolaev Z.Ning S.Nisar S.L.Olsen Q.Ouyang S.Pacetti X.Pan Y.Pan A.Pathak P.Patteri M.Pelizaeus H.P.Peng K.Peters J.Pettersson J.L.Ping R.G.Ping R.Poling V.Prasad H.Qi H.R.Qi K.H.Qi M.Qi T.Y.Qi T.Y.Qi S.Qian W.-B.Qian Z.Qian C.F.Qiao L.Q.Qin X.S.Qin Z.H.Qin J.F.Qiu S.Q.Qu K.H.Rashid K.Ravindran C.F.Redmer A.Rivetti V.Rodin M.Rolo G.Rong Ch.Rosner M.Rump H.S.Sang A.Sarantsev Y.Schelhaas C.Schnier K.Schoenning M.Scodeggio D.C.Shan W.Shan X.Y.Shan J.F.Shangguan M.Shao C.P.Shen P.X.Shen X.Y.Shen H.C.Shi R.S.Shi X.Shi X.D Shi W.M.Song Y.X.Song S.Sosio S.Spataro K.X.Su P.P.Su F.F.Sui G.X.Sun H.K.Sun J.F.Sun L.Sun S.S.Sun T.Sun W.Y.Sun X Sun Y.J.Sun Y.K.Sun Y.Z.Sun Z.T.Sun Y.H.Tan Y.X.Tan C.J.Tang G.Y.Tang J.Tang J.X.Teng V.Thoren I.Uman B.Wang C.W.Wang D.Y.Wang H.J.Wang H.P.Wang K.Wang L.L.Wang M.Wang M.Z.Wang Meng Wang W.Wang W.H.Wang W.P.Wang X.Wang X.F.Wang X.L.Wang Y.Wang Y.D.Wang Y.F.Wang Y.Q.Wang Y.Y.Wang Z.Wang Z.Y.Wang Ziyi Wang Zongyuan Wang D.H.Wei P.Weidenkaff F.Weidner S.P.Wen D.J.White U.Wiedner G.Wilkinson M.Wolke L.Wollenberg J.F.Wu L.H.Wu L.J.Wu X.Wu Z.Wu L.Xia H.Xiao S.Y.Xiao Z.J.Xiao X.H.Xie Y.G.Xie Y.H.Xie T.Y.Xing G.F.Xu Q.J.Xu W.Xu X.P.Xu F.Yan L.Yan W.B.Yan W.C.Yan Xu Yan H.J.Yang H.X.Yang L.Yang S.L.Yang Y.X.Yang Yifan Yang Zhi Yang M.Ye M.H.Ye J.H.Yin Z.Y.You B.X.Yu C.X.Yu G.Yu J.S.Yu T.Yu C.Z.Yuan L.Yuan X.Q.Yuan Y.Yuan Z.Y.Yuan C.X.Yue A.Yuncu A.A.Zafar Y.Zeng B.X.Zhang Guangyi Zhang H.Zhang H.H.Zhang H.Y.Zhang J.J.Zhang J.L.Zhang J.Q.Zhang J.W.Zhang J.Y.Zhang J.Z.Zhang Jianyu Zhang Jiawei Zhang L.Q.Zhang Lei Zhang S.Zhang S.F.Zhang Shulei Zhang X.D.Zhang X.Y.Zhang Y.Zhang Y.H.Zhang Y.T.Zhang Yan Zhang Yao Zhang Yi Zhang Z.H.Zhang Z.Y.Zhang G.Zhao J.Zhao J.Y.Zhao J.Z.Zhao Lei Zhao Ling Zhao M.G.Zhao Q.Zhao S.J.Zhao Y.B.Zhao Y.X.Zhao Z.G.Zhao A.Zhemchugov B.Zheng J.P.Zheng Y.Zheng Y.H.Zheng B.Zhong C.Zhong L.P.Zhou Q.Zhou X.Zhou X.K.Zhou X.R.Zhou A.N.Zhu J.Zhu K.Zhu K.J.Zhu S.H.Zhu T.J.Zhu W.J.Zhu W.J.Zhu Y.C.Zhu Z.A.Zhu B.S.Zou J.H.Zou | 2021 | Chinese Physics C2021，45，2： | 33 |
| 3 | Constructing two-scale network microstructure with nano-Ti5Si3 for superhigh creep resistance显示文摘The improvement of mechanical properties must be achieved by designing and constructing more suitable microstructure,such as hierarchical microstructure.In order to significantly enhance the creep resistance of titanium matrix composites(TMCs),two-scale network microstructure was constructed including the first-scale network(<150μm)with micro-TiB whisker(TiBw)reinforcement and the second-scale network(<30μm)with nano-Ti5Si3 reinforcement by powder metallurgy and in-situ synthesis.The results showed that the creep rate of the composite was remarkably reduced by an order of magnitude compared with the Ti6Al4V alloy at 550℃,600℃,650℃ under the stresses between 100 MPa and 350 MPa.Moreover,the rupture time of the composite was increased by 20 times,compared with that of the Ti6Al4 Valloy at 550℃/300 MPa.The superior creep resistance could be attributed to the hierarchical microstructure.The micro-TiBw reinforcement in the first-scale network boundary contributed to creep resistance primarily by blocking grain boundary sliding,while the nano-Ti5Si3 particle in the second-scale network boundary mainly by hindering phase boundary sliding.In addition,the nano-Ti5Si3 particle was dissolved,and precipitated with smaller size than the primary Ti5Si3.This phenomenon was attributed to Si element diffusion under high temperature and external stress,which could further continuously enhance the creep resistance.Finally,the creep rate during steady-state stage was significantly decreased,which manifested superior creep resistance of the composite. | Y.Jiao L.J.Huang S.L.Wei H.X.Peng Q.An S.Jiang L.Geng | 2019 | Journal of Materials Science & Technology2019，35，8： | 14 |
| 4 | Observation of the Crab Nebula with LHAASO-KM2A−a performance study显示文摘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 TeV.Even though the detector construction is still underway,half of the KM2A array has been operating stably since the end of 2019.In this paper,we present the KM2A data analysis pipeline and the first observation of the Crab Nebula,a standard candle in very high energy γ-ray astronomy.We 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 2020.With the observations,we test the detector performance,including angular resolution,pointing accuracy and cosmic-ray background rejection power.The energy spectrum of the Crab Nebula in the energy range 10-250 TeV fits well with a single power-law function dN/dE=(1.13±0.05stat±0.08sys)×10^(-14).(E/20 TeV)-309±0.06stat±0.02syscm^(-2) s^(-1) TeV^(-1).It is consistent with previous measurements by other experiments.This 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. | 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 | 2021 | Chinese Physics C2021，45，2： | 2 |
| 5 | Highly Virulent Porcine Reproductive and Respiratory Syndrome Virus Emerged in China显示文摘 | Y.‐J.Zhou X.‐F.Hao Z.‐J.Tian G.‐Z.Tong D.Yoo T.‐Q.An T.Zhou G.‐X.Li H.‐J.Qiu T.‐C.Wei X.‐F.Yuan | 2008 | Transboundary and Emerging Diseases (鈥?)2008，，3： | 1 |
| 6 | Electrophoretic deposition of carbon nanotubes onto carbon-fiber fabric for production of carbon/epoxy composites with improved mechanical properties显示文摘 | Q.An A.N.Rider E.T.Thostenson | | 0，，11： | 1 |
| 7 | Geometrical reconstruction of fluorescence events observed by the LHAASO experiment显示文摘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 telescopes.To 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 fundamental.This 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)detectors.Two approaches,which take full advantage ofthe WFCTA detectors.are investigated.One 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 SiPMs.The 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. | 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.Zhou R.Zhou X.X.Zhou C.G.Zhu F.R.Zhu H.Zhu K.J.Zhu X.Zuo 无 | 2021 | Chinese Physics C2021，45，4： | 1 |
| 8 | Measurements of the center-of-mass energies of e^(+)e^(-)collisions at BESIII显示文摘During the 2016-17 and 2018-19 running periods,the BESIII experiment collected 7.5 fb of e^(+)e^(-)collision data at center-of-mass energies ranging from 4.13 to 4.44 GeV.These data samples are primarily used for the study of excited charmonium and charmoniumlike states.By analyzing the di-muon process e^(+)e^(-)→(γISR=FSR)μ^(+)μ^(-),we measure the center-of-mass energies of the data samples with a precision of 0.6 MeV.Through a run-by-run study,we find that the center-of-mass energies were stable throughout most of the data-collection period. | M.Ablikim M.N.Achasov P.Adlarson S.Ahmed M.Albrecht R.Aliberti A.Amoroso M.R.An Q.An X.H.Bai Y.Bai O.Bakina R.Baldini Ferroli I.Balossino Y.Ban K.Begzsuren N.Berger M.Bertani D.Bettoni F.Bianchi J.Bloms A.Bortone I.Boyko R.A.Briere H.Cai X.Cai A.Calcaterra G.F.Cao N.Cao S.A.Cetin J.F.Chang W.L.Chang G.Chelkov D.Y.Chen G.Chen H.S.Chen M.L.Chen S.J.Chen X.R.Chen Y.B.Chen Z.J.Chen W.S.Cheng G.Cibinetto F.Cossio X.F.Cui H.L.Dai X.C.Dai A.Dbeyssi R.E.de Boer D.Dedovich Z.Y.Deng A.Denig I.Denysenko M.Destefanis F.De Mori Y.Ding C.Dong J.Dong L.Y.Dong M.Y.Dong X.Dong S.X.Du Y.L.Fan J.Fang S.S.Fang Y.Fang R.Farinelli L.Fava F.Feldbauer G.Felici C.Q.Feng J.H.Feng M.Fritsch C.D.Fu Y.Gao Y.Gao Y.Gao Y.G.Gao I.Garzia P.T.Ge C.Geng E.M.Gersabeck A Gilman K.Goetzen L.Gong W.X.Gong W.Gradl M.Greco L.M.Gu M.H.Gu Y.T.Gu C.Y Guan A.Q.Guo L.B.Guo R.P.Guo Y.P.Guo A.Guskov T.T.Han W.Y.Han X.Q.Hao F.A.Harris K.L.He F.H.Heinsius C.H.Heinz T.Held Y.K.Heng C.Herold M.Himmelreich T.Holtmann G.Y.Hou Y.R.Hou Z.L.Hou H.M.Hu J.F.Hu T.Hu Y.Hu G.S.Huang L.Q.Huang X.T.Huang Y.P.Huang Z.Huang T.Hussain N Husken W.Ikegami Andersson W.Imoehl M.Irshad S.Jaeger S.Janchiv Q.Ji Q.P.Ji X.B.Ji X.L.Ji Y.Y.Ji H.B.Jiang X.S.Jiang J.B.Jiao Z.Jiao S.Jin Y.Jin M.Q.Jing T.Johansson N.Kalantar-Nayestanaki X.S.Kang R.Kappert M.Kavatsyuk B.C.Ke I.K.Keshk A.Khoukaz P.Kiese R.Kiuchi R.Kliemt L.Koch O.B.Kolcu B.Kopf M.Kuemmel M.Kuessner A.Kupsc M.G.Kurth W.Kuhn J.J.Lane J.S.Lange P.Larin A.Lavania L.Lavezzi Z.H.Lei H.Leithoff M.Lellmann T.Lenz C.Li C.H.Li Cheng Li D.M.Li F.Li G.Li H.Li H.Li H.B.Li H.J.Li J.L.Li J.Q.Li J.S.Li Ke Li L.K.Li Lei Li P.R.Li S.Y.Li W.D.Li W.G.Li X.H.Li X.L.Li Xiaoyu Li Z.Y.Li H.Liang H.Liang H.Liang Y.F.Liang Y.T.Liang G.R.Liao 廖龙洲 J.Libby C.X.Lin B.J.Liu C.X.Liu D.Liu F.H.Liu Fang Liu Feng Liu H.B.Liu H.M.Liu Huanhuan Liu Huihui Liu J.B.Liu J.L.Liu J.Y.Liu K.Liu K.Y.Liu L.Liu M.H.Liu P.L.Liu Q.Liu Q.Liu S.B.Liu Shuai Liu T.Liu W.M.Liu X.Liu Y.Liu Y.B.Liu Z.A.Liu Z.Q.Liu X.C.Lou F.X.Lu H.J.Lu J.D.Lu J.G.Lu X.L.Lu Y.Lu Y.P.Lu C.L.Luo M.X.Luo P.W.Luo T.Luo X.L.Luo X.R.Lyu F.C.Ma H.L.Ma L.L.Ma M.M.Ma Q.M.Ma R.Q.Ma R.T.Ma X.X.Ma X.Y.Ma F.E.Maas M.Maggiora S.Maldaner S.Malde Q.A.Malik A.Mangoni Y.J.Mao Z.P.Mao S.Marcello Z.X.Meng J.G.Messchendorp G.Mezzadri T.J.Min R.E.Mitchell X.H.Mo N.Yu.Muchnoi H.Muramatsu S.Nakhoul Y.Nefedov F.Nerling I.B.Nikolaev Z.Ning S.Nisar S.L.Olsen Q.Ouyang S.Pacetti X.Pan Y.Pan A.Pathak A.Pathak P.Patteri M.Pelizaeus H.P.Peng K.Peters J.Pettersson J.L.Ping R.G.Ping S.Pogodin R.Poling V.Prasad H.Qi H.R.Qi K.H.Qi M.Qi T.Y.Qi S.Qian W.B.Qian Z.Qian C.F.Qiao L.Q.Qin X.P.Qin X.S.Qin Z.H.Qin J.F.Qiu S.Q.Qu K.H.Rashid K.Ravindran C.F.Redmer A.Rivetti V.Rodin M.Rolo G.Rong Ch.Rosner M.Rump H.S.Sang A.Sarantsev Y.Schelhaas C.Schnier K.Schoenning M.Scodeggio D.C.Shan W.Shan X.Y.Shan J.F.Shangguan M.Shao C.P.Shen H.F.Shen P.X.Shen X.Y.Shen H.C.Shi R.S.Shi X.Shi X.D Shi J.J.Song W.M.Song Y.X.Song S.Sosio S.Spataro K.X.Su P.P.Su F.F.Sui G.X.Sun H.K.Sun J.F.Sun L.Sun S.S.Sun T.Sun W.Y.Sun W.Y.Sun X Sun Y.J.Sun Y.K.Sun Y.Z.Sun Z.T.Sun Y.H.Tan Y.X.Tan C.J.Tang G.Y.Tang J.Tang J.X.Teng V.Thoren W.H.Tian Y.T.Tian I.Uman B.Wang C.W.Wang D.Y.Wang H.J.Wang H.P.Wang K.Wang L.L.Wang M.Wang M.Z.Wang Meng Wang W.Wang W.H.Wang W.P.Wang X.Wang X.F.Wang X.L.Wang Y.Wang Y.Wang Y.D.Wang Y.F.Wang Y.Q.Wang Y.Y.Wang Z.Wang Z.Y.Wang Ziyi Wang Zongyuan Wang D.H.Wei F.Weidner S.P.Wen D.J.White U.Wiedner G.Wilkinson M.Wolke L.Wollenberg J.F.Wu L.H.Wu L.J.Wu X.Wu Z.Wu L.Xia H.Xiao S.Y.Xiao Z.J.Xiao X.H.Xie Y.G.Xie Y.H.Xie T.Y.Xing G.F.Xu Q.J.Xu W.Xu X.P.Xu Y.C.Xu F.Yan L.Yan W.B.Yan W.C.Yan Xu Yan H.J.Yang H.X.Yang L.Yang S.L.Yang Y.X.Yang Yifan Yang Zhi Yang M.Ye M.H.Ye J.H.Yin Z.Y.You B.X.Yu C.X.Yu G.Yu J.S.Yu T.Yu 苑长征 L.Yuan X.Q.Yuan Y.Yuan Z.Y.Yuan C.X.Yue A.A.Zafar X.Zeng Zeng Y.Zeng A.Q.Zhang B.X.Zhang Guangyi Zhang H.Zhang H.H.Zhang H.H.Zhang H.Y.Zhang J.J.Zhang J.L.Zhang J.Q.Zhang J.W.Zhang J.Y.Zhang J.Z.Zhang Jianyu Zhang Jiawei Zhang L.M.Zhang L.Q.Zhang Lei Zhang S.Zhang S.F.Zhang Shulei Zhang X.D.Zhang X.Y.Zhang Y.Zhang Y.T.Zhang Y.H.Zhang Yan Zhang Yao Zhang Z.Y.Zhang G.Zhao J.Zhao J.Y.Zhao J.Z.Zhao Lei Zhao Ling Zhao M.G.Zhao Q.Zhao S.J.Zhao Y.B.Zhao Y.X.Zhao Z.G.Zhao A.Zhemchugov B.Zheng J.P.Zheng Y.H.Zheng B.Zhong C.Zhong L.P.Zhou Q.Zhou X.Zhou X.K.Zhou X.R.Zhou X.Y.Zhou A.N.Zhu J.Zhu K.Zhu K.J.Zhu S.H.Zhu T.J.Zhu W.J.Zhu W.J.Zhu Y.C.Zhu Z.A.Zhu B.S.Zou J.H.Zou | 2021 | Chinese Physics C2021，45，10： | 0 |
| 9 | STCF conceptual design report (Volume 1): Physics & detector显示文摘The superτ-charm facility(STCF)is an electron–positron collider proposed by the Chinese particle physics community.It is designed to operate in a center-of-mass energy range from 2 to 7 GeV with a peak luminosity of 0.5×1035 cm–2·s–1 or higher.The 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 Model.The STCF project in China is under development with an extensive R&D program.This 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. | 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 M.Saur W.Shan X.Y.Shan L.L.Shang M.Shao L.Shekhtman C.P.Shen J.M.Shen Z.T.Shen H.C.Shi X.D.Shi B.Shwartz A.Sokolov J.J.Song W.M.Song Y.Song Y.X.Song A.Sukharev J.F.Sun L.Sun X.M.Sun Y.J.Sun Z.P.Sun J.Tang S.S.Tang Z.B.Tang C.H.Tian J.S.Tian Y.Tian Y.Tikhonov K.Todyshev T.Uglov V.Vorobyev B.D.Wan B.L.Wang B.Wang D.Y.Wang G.Y.Wang G.L.Wang H.L.Wang J.Wang J.H.Wang J.C.Wang M.L.Wang R.Wang R.Wang S.B.Wang W.Wang W.P.Wang X.C.Wang X.D.Wang X.L.Wang X.L.Wang X.P.Wang X.F.Wang Y.D.Wang Y.P.Wang Y.Q.Wang Y.L.Wang Y.G.Wang Z.Y.Wang Z.Y.Wang Z.L.Wang Z.G.Wang D.H.Wei X.L.Wei X.M.Wei Q.G.Wen X.J.Wen G.Wilkinson B.Wu J.J.Wu L.Wu P.Wu T.W.Wu Y.S.Wu L.Xia T.Xiang C.W.Xiao D.Xiao M.Xiao K.P.Xie Y.H.Xie Y.Xing Z.Z.Xing X.N.Xiong F.R.Xu J.Xu L.L.Xu Q.N.Xu X.C.Xu X.P.Xu Y.C.Xu Y.P.Xu Y.Xu Z.Z.Xu D.W.Xuan F.F.Xue L.Yan M.J.Yan W.B.Yan W.C.Yan X.S.Yan B.F.Yang C.Yang H.J.Yang H.R.Yang H.T.Yang J.F.Yang S.L.Yang Y.D.Yang Y.H.Yang Y.S.Yang Y.L.Yang Z.W.Yang Z.Y.Yang D.L.Yao H.Yin X.H.Yin N.Yokozaki S.Y.You Z.Y.You C.X.Yu F.S.Yu G.L.Yu H.L.Yu J.S.Yu J.Q.Yu L.Yuan X.B.Yuan Z.Y.Yuan Y.F.Yue M.Zeng S.Zeng A.L.Zhang B.W.Zhang G.Y.Zhang G.Q.Zhang H.J.Zhang H.B.Zhang J.Y.Zhang J.L.Zhang J.Zhang L.Zhang L.M.Zhang Q.A.Zhang R.Zhang S.L.Zhang T.Zhang X.Zhang Y.Zhang Y.J.Zhang Y.X.Zhang Y.T.Zhang Y.F.Zhang Y.C.Zhang Y.Zhang Y.Zhang Y.M.Zhang Y.L.Zhang Z.H.Zhang Z.Y.Zhang Z.Y.Zhang H.Y.Zhao J.Zhao L.Zhao M.G.Zhao Q.Zhao R.G.Zhao R.P.Zhao Y.X.Zhao Z.G.Zhao Z.X.Zhao A.Zhemchugov B.Zheng L.Zheng Q.B.Zheng R.Zheng Y.H.Zheng X.H.Zhong H.J.Zhou H.Q.Zhou H.Zhou S.H.Zhou X.Zhou X.K.Zhou X.P.Zhou X.R.Zhou Y.L.Zhou Y.Zhou Y.X.Zhou Z.Y.Zhou J.Y.Zhu K.Zhu R.D.Zhu R.L.Zhu S.H.Zhu Y.C.Zhu Z.A.Zhu V.Zhukova V.Zhulanov B.S.Zou Y.B.Zuo | 2024 | Frontiers of physics2024，19，1： | 0 |
| 10 | Performance of LHAASO-WCDA and observation of the Crab Nebula as a standard candle显示文摘The first Water Cherenkov detector of the LHAASO experiment(WCDA-1)has been operating since April 2019.The data for the first year have been analyzed to test its performance by observing the Crab Nebula as a standard candle.The WCDA-1 achieves a sensitivity of 65 mCU per year,with a statistical threshold of 5 cr.To 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-induced showers.The 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 design specifications.The energy resolution is found to be 33%for gamma rays around 6 TeV.The spectral energy distribution 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. | F.Aharonian Q.An 阿西克古 白立新 白云翔 包逸炜 D.Bastieri 毕效军 毕玉江 蔡浩 蔡金庭 曹臻 曹喆 常进 常劲帆 常潇川 陈宝民 陈建 陈良 陈亮 陈龙 陈明君 陈玛丽 陈起辉 陈素弘 陈松战 陈天禄 陈秀林 陈阳 程宁 程辉东 崔树旺 崔晓红 崔昱东 戴本忠 代洪亮 戴子高 单增罗布 D.della Volpe B.D'Ettorre Piazzoli 董湘军 樊军辉 范一中 范志香 方军 方堃 冯存峰 封莉 冯少辉 冯有亮 高博 高川东 高启 高卫 葛茂茂 耿利斯 龚光华 苟全补 顾旻皓 郭俊广 郭晓磊 郭义庆 郭莹莹 韩毅昂 何会海 贺昊宁 何坚承 何思乐 何新波 何钰 M.Heller 贺远强 侯超 侯贤 胡红波 胡森 胡世聪 呼晓军 黄代绘 黄秋兰 黄文昊 黄性涛 黄志成 纪方 季筱璐 贾焕玉 江琨 姜泽军 靳超 D.Kuleshov K.Levochkin 李兵兵 李骢 李澄 李飞 李海波 李会财 李华阳 李捷 李凯 李文龙 李昕 李新 李秀荣 李尧 李一卓 李哲 徐卓 梁恩维 梁云峰 林苏杰 刘冰 刘成 刘栋 刘虎 刘海东 刘佳 刘江来 刘佳松 刘金艳 刘茂元 柳若愚 刘四明 刘伟 刘以农 刘彰兴 龙文杰 鲁睿 吕洪魁 马伯强 马玲玲 马欣华 毛基荣 A.Masood W.Mitthumsiri T.Montamli 南云程 庞彬宇 P.Pattarakijwanich 裴致远 齐孟尧 B.Q.Qiao D.Ruffolo V.Rulev A.Saiz 邵琅 O.Shchegolev 盛祥东 石京燕 宋慧超 Yu.V.Stenkin V.Stepanov 孙秦宁 孙晓娜 孙志斌 谭柏轩 唐泽波 田文武 王博东 王超 王辉 王洪光 王建成 王界双 王利苹 王玲玉 王润娜 王为 王伟 王祥高 王晓洁 王祥玉 王玉东 王岩谨 王亚平 王铮 王振 王忠海 王仲翔 韦大明 魏俊杰 魏永健 文韬 吴超勇 吴含荣 武莎 吴文雄 吴雪峰 席邵强 夏捷 夏君集 项光漫 肖刚 肖胡兵 辛广广 辛玉良 邢祎 徐东莲 徐仁新 薛良 闫大海 杨朝文 杨冯帆 杨佳盈 杨莉莉 杨明洁 杨睿智 杨深邦 姚玉华 姚志国 叶一锰 尹丽巧 尹娜 游晓浩 游智勇 于艳红 袁强 曾厚敦 曾婷轩 曾玮 曾宗康 查敏 翟徐徐 张彬彬 张海明 张恒英 张建立 张进文 张力 张路 张丽霞 张鹏飞 张佩佩 张瑞 张少如 张寿山 张潇 张笑鹏 张毅 张盈 张云峰 张月雷 赵兵 赵静 赵雷 赵立志 赵世平 郑福 郑应 周斌 周浩 周佳能 周平 周荣 周勋秀 祝成光 祝凤荣 朱辉 朱科军 左雄 | 2021 | Chinese Physics C2021，45，8： | 0 |
| 11 | Reconstruction of Cherenkov image bymultiple telescopes of LHAASO-WFCTA显示文摘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’region.The 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 goal.Multiple telescopes are put together and point to connected directions for a larger FoV.Method Telescopes are deployed spatially as close as possible,but due to their own size,the distance between two adjacent telescopes is about 10 m.Therefore,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 telescopes.An event building method for Cherenkov images measured by multiple telescopes of WFCTA is developed.The performance of the shower measurements using the combined images is evaluated by comparing with showers that are fully contained by a virtual telescope in simulation.Results 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. | 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.S.Zhang X.Zhang X.P.Zhang Y.F.Zhang Y.L.Zhang Yi Zhang Yong 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 | 2022 | Radiation Detection Technology and Methods2022，6，4： | 0 |
| 12 | A dynamic range extension system for LHAASOWCDA-1显示文摘Purpose The main scientific goal of LHAASO-WCDA is to survey gamma-ray sources with energy from 100 GeV to 30 TeV.To observe high-energy shower events,especially to measure the energy spectrum of cosmic rays from 100 TeV to 10 PeV,a dynamic range extension system(WCDA++)is designed to use a 1.5-inch PMT with a dynamic range of four orders of magnitude for each cell in WCDA-1.Method The dynamic range is extended by using these PMTs to measure the effective charge density in the core region of air shower events,which is an important parameter for identifying the composition of primary particles.Result and Conclusion The system has been running for more than one year.In this paper,the details of the design and performance of WCDA++are presented. | F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi H.Cai J.T.Cai Z.Cao Z.Cao J.Chang J.F.Chang X.C.Chang B.M.Chen J.Chen L.Chen L.Chen L.Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen X.L.Chen Y.Chen N.Cheng Y.D.Cheng S.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu D.della Volpe B.D’Ettorre Piazzoli X.J.Dong J.H.Fan Y.Z.Fan Z.X.Fan J.Fang K.Fang C.F.Feng L.Feng S.H.Feng Y.L.Feng B.Gao C.D.Gao Q.Gao W.Gao M.M.Ge L.S.Geng G.H.Gong Q.B.Gou M.H.Gu J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He S.L.He X.B.He Y.He M.Heller Y.K.Hor C.Hou X.Hou H.B.Hu S.Hu S.C.Hu X.J.Hu D.H.Huang Q.L.Huang W.H.Huang X.T.Huang 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 P.Zhou R.Zhou X.X.Zhou C.G.Zhu F.R.Zhu H.Zhu K.J.Zhu X.Zuo | 2021 | Radiation Detection Technology and Methods2021，5，4： | 0 |
| 13 | Line-of-shower trigger method to lower energy threshold for GRB detection using LHAASO-WCDA显示文摘Purpose Observation of high energy and very high emission from Gamma Ray Bursts(GRBs)is crucial to study the gigantic explosion and the underline processes.With a large field-of-view and almost full duty cycle,the Water Cherenkov Detector Array(WCDA),a sub-array of the Large High Altitude Air Shower Observatory(LHAASO),is appropriate to monitor the very high energy emission from unpredictable transients such as GRBs.Method Nevertheless,the main issue for an extensive air shower array is the high energy threshold which limits the horizon of the detector.To address this issue a new trigger method is developed in this article to lower the energy threshold of WCDA for GRB observation.Result The proposed method significantly improves the detection efficiency of WCDA for gamma-rays around the GRB direction at 10-300 GeV.The sensitivity of the WCDA for GRB detection with the new trigger method is estimated.The achieved sensitivity of the quarter WCDA array above 10 GeV is comparable with that of Fermi-LAT.The data analysis process and corresponding fluence upper limit for GRB 190719C is presented as an example. | 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.Chan 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.Chen Y.D.Chen S.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu D.della Volpe B.D’Ettorre Piazzoli X.J.Don J.H.Fan Y.Z.Fan Z.X.Fan J.Fang K.Fan C.F.Feng L.Feng S.H.Fen Y.L.Feng B.Gao C.D.Gao Q.Gao W.Gao M.M.Ge L.S.Gen 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.Huan W.H.Huang X.T.Huang Z.C.Huang F.Ji X.L.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.Levochkin B.B.Li C.Li C.Li F.Li H.B.Li H.C.Li H.Y.Li J.Li K.Li W.L.Li X.Li X.Li X.R.Li Y.Li Y.Z.Li Z.Li Z.Li E.W.Liang Y.F.Liang S.J.Lin B.Liu C.Liu D.Liu H.Liu H.D.Liu J.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.N.Liu Z.X.Liu W.J.Long R.Lu H.K.Lv B.Q.Ma L.L.Ma X.H.Ma J.R.Mao A.Masood W.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Sáiz L.Shao O.Shchegolev X.D.Shen 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.Wan C.Wang H.Wang H.G.Wang J.C.Wang J.S.Wang L.P.Wang L.Y.Wan R.N.Wang W.Wang W.Wang X.G.Wang X.J.Wan X.Y.Wang Y.D.Wan Y.J.Wan 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.Yan 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.Zhan X.Zhang X.P.Zhan Y.Zhan Y.Zhang Y.F.Zhang Y.L.Zhan 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 The LHAASO Collaboration | 2021 | Radiation Detection Technology and Methods2021，5，4： | 0 |
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