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Reconstruction of.Cherenkov image bymultiple telescopes of.lHAASO-Wf.TA

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 z.e Cao z.en 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 Piaz.oli B.z.Dai H.l.Dai z.G.Dai Danz.ngluobu Ddella Volpe K.K.Duan j.H.f.n Y.z.f.n z.X.f.n j.f.ng K.f.ng C.f.f.ng l.f.ng S.H.f.ng X.T.f.ng Y.l.f.ng 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.j. H.Y.j.a K.j.a K.j.ang z.j.j.ang M.j.n 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 j.an li j.e li K.li Wlli XRli Xin li Xin li Yz.i z.e li z.uo 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.l.o 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.Pattarakij.anich z.Y.Pei M.Y.q. Y.q.q. B.q.q.ao j.j.q.n D.Ruf.olo 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 z.en wang z.eng 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.z.ng T.X.z.ng W.z.ng z.K.z.ng M.z.a X.X.z.ai B.B.z.ang f.z.ang H.M.z.ang H.Y.z.ang j.l.z.ang l.X.z.ang li z.ang lu z.ang P.f.z.ang P.P.z.ang R.z.ang S.B.z.ang S.R.z.ang 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 TIANf. Cosmic Ray Research Center ChengduSichuanChina Dublin Institute f.r Advanced Studies 31 Fitzwilliam Place2DublinIreland Max-Planck-Institut f.r 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.Inf.rmation Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of.Physics Sichuan UniversityChengdu 610065SichuanChina School of.Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Center f.r 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 f.r 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(z.uhai)&Sino-f.ench Institute of.Nuclear Engineering and Technology(z.uhai) Sun Yat-sen UniversityZhuhai 519000China School of.Physics(Guangz.ou) Sun Yat-sen UniversityGuangzhou 510275GuangdongChina Dipartimento di f.sica dell’Universitàdi Napoli“f.derico II” Complesso Universitario di Monte Sant’Angelovia Cinthia80126 NapoliItaly School of.Physics and Astronomy Yunnan UniversityKunming 650091YunnanChina Département de Physiq.e 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.dif.erent cosmic ray compositions around the‘knee’*** Wide f.eld-of.View(f.V)Cherenkov Telescope Array(Wf.TA),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 f.r a larger *** Telescopes are deployed spatially as close as possible,but due to their own siz.,the distance between two adj.cent telescopes is about 10 ***,the Cherenkov lateral distribution and the parallax between the two telescopes should be considered in the event building process f.r images crossing over the boundaries of.f.Vs of.the *** event building method f.r Cherenkov images measured by multiple telescopes of.Wf.TA is *** perf.rmance of.the shower measurements using the combined images is evaluated by comparing with showers that are f.lly contained by a virtual telescope in *** and conclusion It is proved that the developed event building process can help to increase the f.V of.Wf.TA by 30%while maintaining the same reconstruction q.ality,compared to the separate telescope reconstruction method.

关键词： method directions conclusion

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lHAASO-KM2A detector simulation using Geant4

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Radiation Detection Technology and Methods 2024年第3期8卷 1437-1447页

作者： z.en Cao f.Aharonian q.An Axikegu Y.X.Bai Y.W.Bao D.Bastieri X.j.Bi Y.j.Bi j.T.Cai q.Cao W.Y.Cao z.e Cao j.Chang j.f.Chang A.M.Chen E.S.Chen liang Chen lin Chen long Chen M.j.Chen M.l.Chen q.H.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.Dai H.l.Dai z.G.Dai Danz.ngluobu X.q.Dong K.K.Duan j.H.f.n Y.z.f.n j.f.ng K.f.ng C.f.f.ng l.f.ng S.H.f.ng X.T.f.ng Y.l.f.ng S.Gabici B.Gao C.D.Gao l.q.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 H.H.He H.N.He j.Y.He X.B.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 z.C.huang X.l.j. H.Y.j.a K.j.a K.j.ang X.W.j.ang z.j.j.ang M.j.n M.M.Kang T.Ke D.Kuleshov K.Kurinov B.B.li Cheng li Cong li D.li f.li H.B.li H.C.li H.Y.li j.li j.an li j.e li K.li W.l.li W.l.li X.R.li Xin li Y.z.li z.e li z.uo 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.Y.liu M.Y.liu R.Y.liu S.M.liu W.liu Y.liu Y.N.liu R.lu q.l.o 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 z.W.Ou B.Y.Pang P.Pattarakij.anich z.Y.Pei M.Y.q. Y.q.q. B.q.q.ao j.j.q.n D.Ruf.olo A.Sáiz.D.Semikoz.C.Y.Shao l.Shao O.Shchegolev X.D.Sheng f.W.Shu H.C.Song Yu.V.Stenkin V.Stepanov Y.Su q.N.Sun X.N.Sun z.B.Sun P.H.T.Tam q.W.Tang z.B.Tang W.W.Tian C.wang C.B.wang G.W.wang H.G.wang H.H.wang j.C.wang K.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 z.en wang z.eng 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.f.Xu R.X.Xu W.l.Xu l.Xue D.H.Yan j.z.Yan T.Yan C.W.Yang f.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.z.ng T.X.z.ng W.z.ng M.z.a B.B.z.ang f.z.ang H.M.z.ang H.Y.z.ang j.l.z.ang l.X.z.ang li z.ang P.f.z.ang P.P.z.ang R.z.ang S.B.z. Key laboratory of.Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing100049China University of.Chinese Academy of.Sciences Beijing100049China TIANf. Cosmic Ray Research Center ChengduSichuanChina Dublin Institute f.r Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institute f.r Nuclear Physics 69029Heidelberg103980Germany State Key laboratory of.Particle Detection and Electronics BeijingChina University of.Science and Technology of.China Hefei230026AnhuiChina School of.Physical Science and Technology&School of.Inf.rmation Science and Technology Southwest Jiaotong UniversityChengdu610031SichuanChina School of.Astronomy and Space Science Nanjing UniversityNanjing210023JiangsuChina Center f.r Astrophysics Guangzhou UniversityGuangzhou510006GuangdongChina Hebei Normal University Shijiazhuang050024HebeiChina Key laboratory of.Dark Matter and Space Astronomy&Key laboratory of.Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Tsung-Dao lee Institute&School of.Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Key laboratory f.r 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(z.uhai)&School of.Physics(Guangz.ou)&Sino-f.ench Institute of.Nuclear Engineering and Technology(z.uhai) Sun Yat-sen UniversityGuangzhouZhuhai 510275519000GuangdongChina School of.Physics and Astronomy Yunnan UniversityKunming 650091YunnanChina Institute of.f.ontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina APC UniversitéParis CitéCNRS/IN2P3CEA/IRFUObservatoire de ParisParis 11975205France Department of.Engineering Phys

KM2A is one of.the main sub-arrays of.lHAASO,working on gamma ray astronomy and cosmic ray physics at energies above 10 *** simulation is the important f.undation f.r estimating detector perf.rmance and data *** is a big challenge to simulate the KM2A detector in the f.amework of.Geant4 due to the need to track numerous photons f.om a large number of.detector units(>6000)with large altitude dif.erence(30)and huge coverage(1.3).In this paper,the design of.the KM2A simulation code G4KM2A based on Geant4 is *** process of.G4KM2A is optimiz.d mainly in memory consumption to avoid memory *** simplif.cations are used to signif.cantly speed up the execution of.*** running time is reduced by at least 30 times compared to f.ll detector *** particle distributions and the core/angle resolution comparison between simulation and experimental data of.the f.ll KM2A array are also presented,which show good agreement.

关键词： lHAASO KM2A Simulation GEANT4

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A dynamic range extension system f.r lHAASOWCDA-1

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Radiation Detection Technology and Methods 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.Dai H.l.Dai z.G.Dai Danz.ngluobu D.della Volpe B.D’Ettorre Piaz.oli X.j.Dong j.H.f.n Y.z.f.n z.X.f.n j.f.ng K.f.ng C.f.f.ng l.f.ng S.H.f.ng Y.l.f.ng 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.j. X.l.j. H.Y.j.a K.j.ang z.j.j.ang C.j.n 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.Pattarakij.anich z.Y.Pei M.Y.q. D.Ruf.olo 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.z.ng T.X.z.ng W.z.ng z.K.z.ng M.z.a X.X.z.ai B.B.z.ang H.M.z.ang H.Y.z.ang j.l.z.ang j.W.z.ang l.z.ang l.z.ang l.X.z.ang P.f.z.ang P.P.z.ang R.z.ang S.R.z.ang S.S.z.ang X.z.ang X.P.z.ang Y.z.ang Y.z.ang Y.f.z.ang Y.l.z.ang B.z.ao j.z.ao l.z.ao l.z.z.ao S.P.z.ao f.z.eng Y.z.eng B.z.ou H.z.ou j.N.z.ou 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 TIANf. Cosmic Ray Research Center ChengduSichuanChina State Key laboratory of.Particle Detection and Electronics BeijingChina University of.Science and Technology of.China Hefei 230026AnhuiChina 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 f.r Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of.Physics and Astronomy&School of.Physics(Guangz.ou) 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.Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of.f.ontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina Key laboratory f.r 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&School of.Inf.rmation 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 scientif.c goal of.lHAASO-WCDA is to survey gamma-ray sources with energy f.om 100 GeV to 30 *** observe high-energy shower events,especially to measure the energy spectrum of.cosmic rays f.om 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.f.ur orders of.magnitude f.r each cell in *** The dynamic range is extended by using these PMTs to measure the ef.ective charge density in the core region of.air shower events,which is an important parameter f.r identif.ing the composition of.primary *** and Conclusion The system has been running f.r more than one *** this paper,the details of.the design and perf.rmance of.WCDA++are presented.

关键词： lHAASO-WCDA WCDA++ Water Cherenkov detector Perf.rmance

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Perf.rmance of.lHAASO-WCDA and observation of.the Crab Nebula as a standard candle

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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.Dai H.l.Dai z.G.Dai Danz.ngluobu D.della Volpe B.D'Ettorre Piaz.oli X.j.Dong j.H.f.n Y.z.f.n z.X.f.n j.f.ng K.f.ng C.f.f.ng l.f.ng S.H.f.ng Y.l.f.ng 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.j. X.l.j. H.Y.j.a K.j.ang z.j.j.ang C.j.n 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.Pattarakij.anich z.Y.Pei M.Y.q. B.q.q.ao D.Ruf.olo 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.z.ng T.X.z.ng W.z.ng z.K.z.ng M.z.a X.X.z.ai B.B.z.ang H.M.z.ang H.Y.z.ang j.l.z.ang j.W.z.ang l.z.ang l.z.ang l.X.z.ang P.f.z.ang P.P.z.ang R.z.ang S.R.z.ang S.S.z.ang X.z.ang X.P.z.ang Y.z.ang Y.z.ang Y.f.z.ang Y.l.z.ang B.z.ao j.z.ao l.z.ao l.z.z.ao S.P.z.ao f.z.eng Y.z.eng B.z.ou H.z.ou j.N.z.ou 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 TIANf. Cosmic Ray Research Center ChengduSichuanChina State Key laboratory of.Particle Detection and Electronics China University of.Science and Technology of.China Hefei 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 f.r Astrophysics Guangzhou UniversityGuangzhou 510006China School of.Physics and Astronomy&School of.Physics(Guangz.ou) 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.Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Institute of.f.ontier and Interdisciplinary Science Shandong UniversityQingdao 266237China Key laboratory f.r 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&School of.Inf.rmation 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 f.rst Water Cherenkov detector of.the lHAASO experiment(WCDA-1)has been operating since April *** data f.r the f.rst year have been analyz.d to test its perf.rmance by observing the Crab Nebula as a standard *** WCDA-1 achieves a sensitivity of.65 mCU per year,with a statistical threshold of.5 *** accomplish this,a 97.7%cosmic-ray background rej.ction rate around 1 TeV and 99.8%around 6 TeV with an ap proximate photon acceptance of.50%is achieved af.er applying an algorithm to separate gamma-induced *** 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 *** energy resolution is f.und to be 33%f.r gamma rays around 6 *** spectral energy distribution of.the Crab Nebula in the range f.om 500 GeV to 15.8 TeV is measured and f.und to be in agreement with the results f.om other TeV gamma ray observatories.

关键词： lHAASO-WCDA Crab Nebula angular resolution spectral energy distribution

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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.Af.dulidis X.C.Ai R.Aliberti A.Amoroso q.An Y.Bai O.Bakina I.Balossino Y.Ban H.-R.Bao V.Batoz.kaya K.Begz.uren 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.Destef.nis f.De Mori B.f.ng S.S.f.ng W.X.f.ng Y.f.ng Y.q.f.ng R.f.rinelli l.f.va f.f.ldbauer G.f.lici C.q.f.ng j.H.f.ng Y.T.f.ng K.f.scher M.f.itsch C.D.f. j.l.f. Y.W.f. H.Gao Y.N.Gao Yang Gao S.Garbolino I.Garz.a 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.f.n j.f.ng j..Gilman K.Goetz.n 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\"olz.en N.H\"usken N.in der Wiesche M.Irshad j.j.ckson S.j.nchiv j.H.j.ong q.j. q.P.j. W.j. X.B.j. X.l.j. Y.Y.j. X.q.j.a z.K.j.a D.j.ang H.B.j.ang P.C.j.ang S.S.j.ang T.j.j.ang X.S.j.ang Y.j.ang j.B.j.ao j.K.j.ao z.j.ao S.j.n Y.j.n M.q.j.ng X.M.j.ng T.j.hansson 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.lavez.i T.T.lei z.H.lei H.leithof. 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 f.dan University Shanghai 200433China GSI Helmholtz.entre f.r Heavy Ion Research GmbH D-64291 DarmstadtGermany Guangxi Normal University Guilin 541004China Guangxi University Nanning 530004China Hangz.ou 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 INf. laboratori Naz.onali di f.ascati INFN Laboratori Nazionali di FrascatiI-00044FrascatiItaly INf. laboratori Naz.onali di f.ascati INFN Sezione di PerugiaI-06100PerugiaItaly INf. laboratori Naz.onali di f.ascati University of PerugiaI-06100PerugiaItaly INf. Sez.one di f.rrara INFN Sezione di FerraraI-44122FerraraItaly INf. Sez.one di f.rrara 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 f.^(−1)taken at the center-of.mass energy√s=3.773 GeV with the BESIII detector,a j.int amplitude analysis is perf.rmed on the decays D^(0)→π^(+)π^(−)π^(+)π^(−)and D^(0)→π^(+)π^(−)π^(0)π^(0)(non-η).The f.t f.actions of.individual components are obtained,and large interf.rences 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 f.actions 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 f.actions 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 f.r 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 f.action

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line-of.shower trigger method to lower energy threshold f.r GRB detection using lHAASO-WCDA

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Radiation Detection Technology and Methods 2021年第4期5卷 531-541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.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 Danz.ngluobu D.della Volpe B.D’Ettorre Piaz.oli X.j.Don j.H.f.n Y.z.f.n z.X.f.n j.f.ng K.f.n C.f.f.ng l.f.ng S.H.f.n Y.l.f.ng 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.j. X.l.j. H.Y.j.a K.j.ang z.j.j.ang C.j.n 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.Pattarakij.anich z.Y.Pei M.Y.q. D.Ruf.olo 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.z.ng T.X.z.ng W.z.ng z.K.z.ng M.z.a X.X.z.ai B.B.z.ang H.M.z.ang H.Y.z.ang j.l.z.ang j.W.z.ang l.z.ang l.z.ang l.X.z.ang P.f.z.ang P.P.z.ang R.z.ang S.R.z.ang S.S.z.an X.z.ang X.P.z.an Y.z.an Y.z.ang Y.f.z.ang Y.l.z.an B.z.ao j.z.ao l.z.ao l.z.z.ao S.P.z.ao f.z.eng Y.z.eng B.z.ou H.z.ou j.N.z.ou P.z.ou R.z.ou X.X.z.ou C.G. Key laboratory of.Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of.Chinese Academy of.Sciences Beijing 100049China TIANf. Cosmic Ray Research Center ChengduSichuanChina State Key laboratory of.Particle Detection and Electronics BeijingChina University of.Science and Technology of.China Hefei 230026AnhuiChina 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 f.r Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of.Physics and Astronomy&School of.Physics(Guangz.ou) 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.Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of.f.ontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina Key laboratory f.r 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&School of.Inf.rmation 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.Physic

Purpose Observation of.high energy and very high emission f.om Gamma Ray Bursts(GRBs)is crucial to study the gigantic explosion and the underline *** a large f.eld-of.view and almost f.ll 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 f.om unpredictable transients such as *** Nevertheless,the main issue f.r an extensive air shower array is the high energy threshold which limits the horiz.n of.the *** address this issue a new trigger method is developed in this article to lower the energy threshold of.WCDA f.r GRB *** The proposed method signif.cantly improves the detection ef.iciency of.WCDA f.r gamma-rays around the GRB direction at 10-300 *** sensitivity of.the WCDA f.r GRB detection with the new trigger method is *** achieved sensitivity of.the q.arter WCDA array above 10 GeV is comparable with that of.*** data analysis process and corresponding f.uence upper limit f.r GRB 190719C is presented as an example.

关键词： lHAASO WCDA GRB

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Evidence f.r the decays of.∧_c^+→∑^+η and ∑^+η’

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Chinese Physics C 2019年第8期43卷 15-23页

作者： M.Ablikim f.f.An q.An Y.Bai Y.Ban H.Cai X.Cai G.f.Cao j.f.Chang G.Chen H.S.Chen j.C.Chen M.l.Chen P.l.Chen S.j.Chen Y.B.Chen W.Cheng H.lDai j.P.Dai z.Y.deng Y.Ding C.Dong j.Dong l.Y.Dong M.Y.Dong z.l.Dou S.X.Du P.f.Duan j.z.f.n j.f.ng S.S.f.ng Y.f.ng C.q.f.ng C.D.f. Y.f. q.Gao X.l.Gao Y.Gao Y.G.Gao z.Gao l.Gong W.X.Gong l.M.Gu M.H.Gu Y.T.Gu A.q.Guo l.B.Guo R.P.Guo Y.P.Guo S.Han X.q.Hao K.l.He Y.K.Heng 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 q.j. q.P.j. X.B.j. X.l.j. X.S.j.ang X.Y.j.ang j.B.j.ao z.j.ao D.P.j.n S.j.n Y.j.n X.S.Kang B.C.Ke 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 lei li P.l.li P.R.li q.Y.li T.li W.D.li W.G.li X.l.li X.N. li X.q.l. z.B.li H.liang Y.f.liang Y.T.liang G.R.liao l.z.liao C.X.lin D.X.lin B.liu B.j.liu C.X.liu D.liu D.Y.liu f.H.liu f.ng liu f.ng liu H.B.liu H.l.liu H.M.liu huanhuan liu huihui liu j.B.liu j.Y.liu K.liu K.Y.liu Ke liu q.l.u S.B.liu X.liu Y.B.liu z.A.liu z.iq.ng 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 T.luo X.l.luo 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 Y.j.Mao z.P.Mao z.X.Meng j.Min T.j.Min X.H.Mo Y.j.Mo z.Ning S.l.Niu S.l.Olsen q.Ouyang Y.Pan H.P.Peng j.l.Ping R.G.Ping H.R.q. M.q. T.Y.q. S.q.an C.f.q.ao N.q.n z.H.q.n j.f.q.u S.q.q. G.Rong W.Shan X.Y.Shan M.Shao C.P. Shen P.X.Shen X.Y.Shen H.Y.Sheng X.Shi j.j.Song X.Y.Song 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 B.wang B.l.wang C.W.wang D.Y.wang Dan wang K.wang l.l.wang l.S.wang M.wang Meng wang P.wang P.l.wang W.P.wang X.f.wang Y.wang Y.f.wang z.wang z.G.wang z.Y.wang z.ngyuan wang D.H.Wei S.P.Wen l.H.Wu l.j.Wu z.Wu l.Xia Y.Xia D.Xiao Y.j.Xiao z.j.Xiao Y.G.Xie Y.H.Xie X.A.Xiong q.l.Xiu G.f.Xu j.j.Xu l.Xu q.j.Xu q.N.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 S.l.Yang Y.H.Yang Y.X.Yang Yif.n 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 Y.Yuan Y.z.ng B.X.z.ang B.Y.z.ang Institute of.High Energy Physics G.I.Budker Institute of.Nuclear Physics SB RAS(BINP) the Novosibirsk State University Helmholtz.Institute Mainz Bochum Ruhr-University University of.Turin INf. State Key laboratory of.Particle Detection and Electronics University of.Science and Technology of.China Southeast University j.int Institute f.r Nuclear Research INf. laboratori Naz.onali di f.ascati Peking University Institute of.Physics and Technology Indiana University Bloomington Carnegie Mellon University j.hannes Gutenberg University of.Mainz INf. Sez.one di f.rrara Wuhan University Ankara University University of.Chinese Academy of.Sciences Istanbul Bilgi University the Moscow Institute of.Physics and Technology the f.nctional Electronics laboratory Tomsk State University University of.South China Nanj.ng University Shanghai j.ao Tong University Key laboratory f.r Particle Physics Astrophysics and CosmologyMinistry of EducationShanghai Key Laboratory for Particle Physics and CosmologyInstitute of Nuclear and Particle Physics liaoning University Nankai University z.engz.ou University Tsinghua University University of.f.rrara University of.Eastern Piedmont Central China Normal University University of.Minnesota Minneapolis GSI Helmholtz.entre f.r Heavy Ion Research GmbH Guangxi University Nanj.ng Normal University KVI-CART University of Groningen Henan Normal University University of.Hawaii Honolulu Shandong University University of.the Punj.b University of.Muenster Uppsala University huangshan College University of.j.nan j.stus-liebig-Universitaet Giessen II.Physikalisches Institut Istanbul Arel University Soochow University Beij.ng Institute of.Petrochemical Technology China Center of.Advanced Science and Technology Sun Yat-Sen University Sichuan University Guangxi Normal University Indian Institute of.Technology Madras Shanxi University Henan University of.Science and Technology lanz.ou University z.ej.ang University f.dan University Key laboratory of.Nuclear Physics and Ion-beam Application(MOE)and Institute of

We study the hadronic decays of.∧c+ to the f.nal states ∑+η and ∑+η’,using an e+e-annihilation data sample of.567 pb-1 taken at a center-of.mass energy of.4.6 GeV with the BESIII detector at the BEPCⅡ *** f.nd evidence f.r the decays ∧c+→∑+η and ∑+η’ with statistical signif.cance of.2.5σ and 3.2σ,*** to the ref.rence decays ∧c+→∑+π0 and ∑+ω,we obtain the ratios of.the branching f.actions■and ■to be 0.35±0.16±0.02 and 0.86±0.34±0.04,*** upper limits at the 90% conf.dence level are set to be■and■.Using BESIII measurements of.the branching f.actions of.the ref.rence decays,we determine B（∧c+→∑+η）=（0.41±0.19±0.05）%（f.rst uncertainties are statistical and the second *** obtained branching f.action of.∧c+→∑+η is consistent with the previous measurement,and the branching f.action of.∧c+→∑+η’ is measured f.r the f.rst time.

关键词： charmed baryon ∧c^+ decays branching f.actions

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Prospects f.r a multi-TeV gamma-ray sky survey with the lHAASO water Cherenkov detector array

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Chinese Physics C 2020年第6期44卷 123-132页

作者： f.Aharonian V.Alekseenko q.An Axikegu l.X.Bai Y.W.Bao D.Bastieri9 X.j.Bi H.Cai z.e Cao z.en Cao j.Chang j.f.Chang X.C.Chang S.P.Chao B.M.Chen j.Chen l.Chen l.Chen M.l.Chen M.j.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 Danz.ngluobu B.D'Ettorre Piaz.oli j.f.ng j.H.f.n Y.z.f.n C.f.f.ng l.f.ng S.H.f.ng Y.l.f.ng B.Gao q.Gao W.Gao M.M.Ge l.S.Geng G.H.Gong q.B.Gou M.H.Gu Y.q.Guo Y.Y.Guo Y.A.Han H.H.He j.C.He M.Heller S.l.He Y.He C.Hou D.H.huang q.l.huang W.H.huang X.T.huang H.B.hu S.hu H.Y.j.a K.j.ang f.j. C.j.n X.l.j. K.levochkin E.W.liang Y.f.liang Cheng li Cong li f.li H.li H.B.li H.C.li H.M.li j.li K.li W.l.li X.li X.R.li Y.li z.li z.li B.liu C.liu D.liu H.D.liu H.liu j.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 j.R.Mao A.Masood X.H.Ma W.Mitthumsiri T.Montaruli Y.C.Nan P.Pattarakij.anich z.Y.Pei B.q.q.ao M.Y.q. D.Ruf.olo V.Rulev A.Sáiz.l.Shao O.Shchegolev X.D.Sheng j.R.Shi Y.Stenkin V.Stepanov z.B.Sun P.H.T.Tam z.B.Tang W.W.Tian D.D.Volpe C.wang H.wang H.G.wang j.C.wang l.Y.wang W.wang W.wang X.G.wang X.Y.wang X.j.wang Y.D.wang Y.j.wang Y.N.wang Y.P.wang z.wang z.H.wang z.X.wang D.M.Wei j.j.Wei T.Wen C.Y.Wu H.R.Wu S.Wu W.X.Wu X.f.Wu G.M.Xiang G.Xiao G.G.Xin Y.Xing R.X.Xu l.Xue D.H.Yan C.W.Yang f.f.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 q.Yuan Y.H.Yu z.j.j.ang H.D.z.ng T.X.z.ng W.z.ng z.K.z.ng M.z.a B.B.z.ang H.M.z.ang H.Y.z.ang j.l.z.ang j.W.z.ang l.z.ang P.f.z.ang P.P.z.ang S.R.z.ang S.S.z.ang X.z.ang X.P.z.ang Yi z.ang Yong z.ang Y.f.g z.ang B.z.ao j.z.ao l.z.ao l.z.z.ao f.z.eng Y.z.eng j.N.z.ou P.z.ou R.z.ou X.X.z.ou C.G.z.u f.R.z.u H.z.u K.j.z.u X.z.o Institute of.High Energy Physics Chinese Academy of SciencesBeijing 100049China University of.Chinese Academy of.Sciences Beijing 100049China TIANf. Cosmic Ray Research Center ChengduShichuanChina University of.Science and Technology of.China 230026 HefeiAnhuiChina Tsinghua University 100084 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 f.r Astrophysics Guangzhou University510006 GuangzhouGuangdongChina Sun Yat-sen University 519000 ZhuhaiGuangdongChina Shool of.Physics and Technology Guangxi University530004 NanningGuangxiChina Hebei Normal University 050024 ShijiazhuangHebeiChina School of.Physics and Engineering Zhengzhou University450001 ZhengzhouHenanChina Nanj.ng University 210023 NanjingJiangsuChina Key laboratory of.Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of Sciences210034 NanjingJiangsuChina Institute of.f.ontier and Interdisciplinary Science Shandong University266237 QingdaoShandongChina Shanghai Astronomical Observatory Chinese Academy of Sciences200030 ShanghaiChina School of.Physical Science and Technology Southwest Jiaotong University610031 ChengduSichuanChina Sichuan University 610065 ChengduSichuanChina Key laboratory of.Cosmic Rays(Tibet University) Ministry of Education850000 LhasaTibetChina School of.physics and technology Wuhan university430072 WuhanChina Yunnan University 650091 KunmingYunnanChina Yunnan Astronomical Observatories Chinese Academy of Sciences650216 KunmingYunnanChina Institute f.r Nuclear Research Russian Academy of SciencesMoscowRussia Département de Physiq.e Nucléaire et Corpusculaire Facultéde SciencesUniversitéde GenéveGenevaSwitzerland Department of.Physics Faculty of ScienceMahidol UniversityBangkokThailand Dublin Institute f.r Advanced Studies 31 Fitzwilliam PlaceDublin 2Ireland Max-Planc

The Water Cherenkov Detector Array(WCDA) is a maj.r component of.the large High Altitude Air Shower Array Observatory(lHAASO), a new generation cosmic-ray experiment with unprecedented sensitivity, currently under construction. WCDA is aimed at the study of.TeV γ-rays. In order to evaluate the prospects of.searching f.r TeV γ-ray sources with WCDA, we present a proj.ction of.the one-year sensitivity of.WCDA to TeV γ-ray sources f.om TeVCat using an all-sky approach. Out of.128 TeVCat sources observable by WCDA up to a z.nith angle of.45°, we estimate that 42 would be detectable in one year of.observations at a median energy of.1 TeV. Most of.them are Galactic sources, and the extragalactic sources are Active Galactic Nuclei(AGN).

关键词： TeVγ-ray astronomy observational prospect lHAASO-WCDA

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Existing of.SARS-CoV like viruses in domestic civets in China

Existing of SARS-CoV like viruses in domestic civets in Chin...

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2004年中国科学院新生病毒性疾病控制学术讨论会

作者： H.z.wang f.deng H.Song B.K.Bai H.l.wang G.W.z.ang z.l.Shi l.j.Tang Y.W.z.ou X.f.An W.q.hu z.Chen S.Y.z.ang S.j.Chen G.P.z.ao z.Chen z.hu Wuhan Institute of.Virology CAS Ruij.n Hospital Af.iliated to Shanghai Second Medical University hubei CDC Tongj. Medical College Institute of.z.ology CAS Chinese National human Genome Center at Shanghai Wuhan Institute of.Virology CAS

he SARS coronavirus (SARS-CoV) has been identif.ed to be the cause of.SARS, yet it remains unclear where the SARS coronavirus evolved f.om. Evidence suggests the SARS-CoV emerged f.om animal sources and it has been reported that SARS-CoV like virus were f.und f.om Himalayan palm civets in a lived animal market in Guangdong China (Guan et al., 2003). In this work, we studied the existing of.SARS-CoV like virus in domestic civets in China. Three civet f.rms, named CS, ES, Wf. in hubei and hunan Provinces of.China were investigated. Oral swabs, f.cal swabs, and serum samples were taken f.om about 10 civets in each f.rm. The oral swabs were tested with RT-PCR f.r viral nucleic acid and with ElISA f.r viral antigen. Serum samples were tested with ElISA f.r SARS-CoV specif.c antibodies. Some of.the RT-PCR products were cloned and seq.enced. Tissue samples f.om certain civets were also collected and observed under electron microscope. In situ hybridiz.tion using SARS-CoV specif.c probes were also perf.rmed. Combing the primary results of.all the tests, it suggests that SARS-CoV like viruses exist in domestic civets and can cause chronic inf.ction in those animals.

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Antineutrino energy spectrum unf.lding based on the Daya Bay measurement and its applications

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Chinese Physics C 2021年第7期45卷 1-19页

作者： f.P.An A.B.Balantekin M.Bishai S.Blyth G.f.Cao j.Cao j.f.Chang Y.Chang H.S.Chen S.M.Chen Y.Chen Y.X.Chen j.Cheng z.K.Cheng j.j.Cherwinka M.C.Chu j.P.Cummings O.Dalager f.S.deng Y.Y.Ding M.V.Diwan T.Dohnal D.Dolz.ikov j.Dove M.Dvorak D.A.Dwyer j.P.Gallo M.Gonchar G.H.Gong H.Gong M.Grassi W.q.Gu j.Y.Guo l.Guo X.H.Guo Y.H.Guo z.Guo R.W.Hackenburg S.Hans a M.He K.M.Heeger Y.K.Heng Y.K.Hor Y.B.Hsiung B.z.hu j.R.hu T.hu z.j.hu H.X.huang j.H.huang X.T.huang Y.B.huang P.huber D.E.j.f.e K.l.j.n X.l.j. X.P.j. R.A.j.hnson D.j.nes l.Kang S.H.Kettel S.Kohn M.Kramer T.j.langf.rd j.lee j.H.C.lee R.T.lei R.leitner j.K.C.leung f.li H.l.li j.j.li q.j.li R.H.li S.li S.C.li W.D.li X.N.li X.q.l. Y.f.li z.B.li H.liang C.j.lin G.l.lin S.lin j.j.ling j.M.link26 l.littenberg B.R.littlej.hn j.C.liu j.l.liu j.X.liu C.lu H.q.l. K.B.luk B.z.Ma X.B.Ma X.Y.Ma Y.q.Ma R.C.Manduj.no C.Marshall K.T.McDonald R.D.McKeown Y.Meng j.Napolitano D.Naumov E.Naumova T.M.T.Nguyen j.P.Ochoa-Ricoux A.Olshevskiy H.-R.Pan j.Park S.Patton j.C.Peng C.S.j.Pun f.z.q. M.q. X.q.an N.Raper j.Ren C.Morales Reveco R.Rosero B.Roskovec X.C.Ruan H.Steiner j.l.Sun T.Tmej. K.Treskov W.-H.Tse C.E.Tull B.Viren V.Vorobel C.H.wang j.wang M.wang N.Y.wang R.G.wang W.wang W.wang X.wang Y.wang Y.f.wang z.wang z.wang z.M.wang H.Y.Wei l.H.Wei l.j.Wen K.Whisnant C.G.White H.l.H.Wong E.Worcester D.R.Wu f.l.Wu q.Wu W.j.Wu D.M.Xia z.q.Xie z.z.Xing H.K.Xu j.l.Xu T.Xu T.Xue C.G.Yang l.Yang Y.z.Yang H.f.yao M.Ye M.Yeh B.l.Young H.z.Yu z.Y.Yu B.B.Yue V.z.vadskyi S.z.ng Y.z.ng l.z.an C.z.ang f.Y.z.ang H.H.z.ang j.W.z.ang q.M.z.ang S.q.z.ang X.T.z.ang Y.M.z.ang Y.X.z.ang Y.Y.z.ang z.j.z.ang z.P.z.ang z.Y.z.ang j.z.ao R.z.z.ao l.z.ou H.l.z.uang j.H.z.u Institute of.Modern Physics East China University of Science and TechnologyShanghai 200337 University of.Wisconsin MadisonWisconsin 53706 Brookhaven National laboratory UptonNew York 11973 Department of.Physics Nnational Taiwan UniversityTaipei Institute of.High Energy Physics Beijing 100049 National United University Miao-Li Department of.Engineering Physics Tsinghua UniversityBeijing 100048 Shenz.en University Shenzhen 518061 Sun Yat-Sen(z.ongshan)University Guangzhou 510275 North China Electric Power University Beijing 102206 Chinese University of.Hong Kong Hongkong 999077 Siena College LoudonvilleNew York 12211 Department of.Physics and Astronomy University of CaliforniaIrvineCalifornia 92697 University of.Science and Technology of.China Hefei 230022 Charles University Faculty of Mathematics and PhysicsPrague j.int Institute f.r Nuclear Research DubnaMoscow Region Department of.Physics University of Illinois at Urbana-ChampaignUrbanaIllinois 61801 lawrence Berkeley National laboratory BerkeleyCalifornia 94720 Department of.Physics Illinois Institute of TechnologyChicagoIllinois 60616 Beij.ng Normal University Beijing 100875 Department of.Nuclear Science and Technology School of Energy and Power EngineeringXi'an Jiaotong UniversityXi'an 710049 Wright laboratory and Department of.Physics Yale UniversityNew HavenConnecticut 06520 China Institute of.Atomic Energy Beijing 102413 Shandong University Jinan 250002 Guangxi University No.100 Daxue East RoadNanning 530004 Center f.r Neutrino Physics Virginia TechBlacksburgVirginia 24061 Institute of.Physics NCTUHsinchu Department of.Physics University of CincinnatiCincinnatiOhio 45221 Department of.Physics College of Science and TechnologyTemple UniversityPhiladelphiaPennsylvania 19122 Dongguan University of.Technology Dongguan 523808 Department of.Physics University of CaliforniaBerkeleyCalifornia 94720 Department of.Physics The University of Hong KongPokfulamHongkong 999077 School of.Physics Nankai UniversityTianjin 300071 Department o

The prediction of.reactor antineutrino spectra will play a crucial role as reactor experiments enter the precision *** positron energy spectrum of.3.5 million antineutrino inverse beta decay reactions observed by the Daya Bay experiment,in combination with the f.ssion rates of.f.ssile isotopes in the reactor,is used to extract the positron energy spectra resulting f.om the f.ssion of.specif.c *** inf.rmation can be used to produce a precise,data-based prediction of.the antineutrino energy spectrum in other reactor antineutrino experiments with dif.erent f.ssion f.actions than Daya *** positron energy spectra are unf.lded to obtain the antineutrino energy spectra by removing the contribution f.om detector response with the Wiener-SVD unf.lding *** results are obtained with other unf.lding methods.A techniq.e to construct a data-based prediction of.the reactor antineutrino energy spectrum is proposed and *** the reactor f.ssion f.actions,the techniq.e can predict the energy spectrum to a 2%*** addition,we illustrate how to perf.rm a rigorous comparison between the unf.lded antineutrino spectrum and a theoretical model prediction that avoids the input model bias of.the unf.lding method.

关键词： reactor antineutrino energy spectrum Daya Bay application

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