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Geometrical reconstruction of fluorescence events observed by the LHAASO experiment

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chinese Physics c 2021年第4期45卷 416-425页

作者： F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.W.Bao D.Bastieri X.j.Bi Y.j.Bi H.cai j.T.cai Z.cao Z.cao j.chang j.F.chang X.c.chang B.M.chen j.chen L.chen L.chen L.chen M.j.chen M.L.chen Q.H.chen S.H.chen S.Z.chen T.L.chen X.L.chen Y.chen N.cheng Y.D.cheng S.W.cui X.H.cui Y.D.cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu D.della Volpe B.DEtorre Piazzoli X.j.Dong j.H.Fan Y.Z.Fan Z.X.Fan j.Fang j.Fang c.F.Feng L.Feng S.H.Feng Y.L.Feng B.Gao c.D.Gao Q.Gao W.Gao M.M.Ge L.S.Geng G.H.Gong Q.B.Gou M.H.Gu j.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.he H.N.he j.c.he S.L.he X.B.he Y.he M.heller Y.K.Hor c.Hou X.Hou H.B.Hu S.Hu S.c.Hu X.j.Hu D.H.Huang Q.L.Huang W.H.Huang X.T.Huang Z.c.Huang F.ji X.L.ji H.Y.jia K.jiang Z.j.jiang c.jin D.Kuleshov K.Levochkin B.B.Li c.Li c.Li F.Li H.B.Li H.c.Li H.Y.Li j.Li K.Li W.L.Li X.Li X.Li X.R.Li Y.Li Y.Z.Li Z.Li Z.Li E.W.Liang Y.F.Liang S.j.Lin B.Liu c.Liu D.Liu H.Liu H.D.Liu j.Liu j.L.Liu j.L.Liu j.S.Liu j.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.N.Liu Z.X.Liu W.j.Long R.Lu H.K.Lv B.Q.Ma L.L.Ma X.H.Ma j.R.Mao A.Masood W.Mitthumsiri T.Montaruli Y.c.Nan B.Y..Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Saiz L.Shao O.Shchegolev X.D.Sheng j.R.Shi H.c.Song Yu.V.Stenkin V.Stepanov Q.N.Sun X.N.Sun Z.B.Sun P.H.T.Tam Z.B.Tang W.W.Tian B.D.Wang c.Wang H.Wang H.G.Wang j.c.Wang j.S.Wang L.P.Wang L.Y.Wang R.N.Wang W.Wang W.Wang X.G.Wang X.j.Wang X.Y.Wang Y.D.Wang Y.j.Wang Y.P.Wang Z.Wang Z.Wang Z.H.Wang Z.X.Wang D.M.Wei j.j.Wei Y.j.Wei T.Wen c.Y.Wu H.R.Wu S.Wu W.X.Wu X.F.Wu S.Q.Xi j.Xia j.j.Xia G.M.Xiang G.Xiao H.B.Xiao G.G.Xin Y.L.Xin Y.Xing D.L.Xu R.X.Xu L.Xue D.H.Yan c.W.Yang F.F.Yang j.Y.Yang L.L.Yang M.j.Yang R.Z.Yang S.B.Yang Y.H.Yao Z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.D.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha X.X.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang j.L.Zhang j.W.Zhang L.Zhang L.Zhang L.X.Zhang P.F.Zhang P.F.Zhang R.Zhang S.R.Zhang S.S.Zhang X.Zhang X.P.Zhang Y.Zhang Y.Zhang Y.F.Zhang Y.L.Zhang B.Zhao j.Zhao L.Zhao L.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou j.N.Zhou P Key Laboratory of Particle Astrophyics&Experimental Physics Division&computing center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of chinese Academy of Sciences Beijing 100049China TIANFU cosmic Ray Research center ChengduSichuanChina State Key Laboratory of Paricle Detection and Electronics China University of Science and Technology of china HefeiAnhui 230026China Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China center for Astrophysics Guangzhou UniversityGuangzhouGuangdong 510006China School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhaiGuangdong 519000China School of Physical Science and Technology Guangxi UniversityNanningGuangxi 530004China hebei Normal University ShijiazhuangHebei 050024China School of Physics and Microelectronics Zhengzhou UniversityZhengzhouHenan 450001China School of Astronomy and Space Science Nanjing UniversityNanjingJiangsu 210023China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjingJiangsu 210023China Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdaoShandong 266237China Key Laboratory for Research in Galaxies and cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology Southwest Jiaotong UniversityChengduSichuan 610031China college of Physics Sichuan UniversityChengduSichuan 610065China Key Laboratory of cosmic Rays(Tibet University) Ministry of EducationLhasaTibet 850000China School of physics and technology Wuhan UniversityWuhanHubei 430072Ch

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

关键词： cosmic ray fluorescence telescope stereo observation geometrical reconstruction

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

Line-of-shower trigger method to lower energy threshold for 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 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. 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 TIANFU 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 for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina School of Physical Science and Technology Guangxi UniversityNanning 530004GuangxiChina hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina 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&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina college of Physics Sichuan UniversityChengdu 610065SichuanChina Key Laboratory of cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina School of Physic

Purpose Observation of high energy and very high emission from Gamma Ray Bursts(GRBs)is crucial to study the gigantic explosion and the underline *** 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 *** Nevertheless,the main issue for an extensive air shower array is the high energy threshold which limits the horizon of the *** address this issue a new trigger method is developed in this article to lower the energy threshold of WcDA for GRB *** The proposed method significantly improves the detection efficiency of WcDA for gamma-rays around the GRB direction at 10-300 *** sensitivity of the WcDA for GRB detection with the new trigger method is *** achieved sensitivity of the quarter WcDA array above 10 GeV is comparable with that of *** data analysis process and corresponding fluence upper limit for GRB 190719c is presented as an example.

关键词： LHAASO WcDA GRB

A dynamic range extension system for 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 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 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 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 for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina School of Physical Science and Technology Guangxi UniversityNanning 530004GuangxiChina hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina 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&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina college of Physics Sichuan UniversityChengdu 610065SichuanChina Key Laboratory of cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina School of Physics

Purpose The main scientific goal of LHAASO-WcDA is to survey gamma-ray sources with energy from 100 GeV to 30 *** observe high-energy shower events,especially to measure the energy spectrum of cosmic rays from 100 TeV to 10 PeV,a 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 *** 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 *** and conclusion The system has been running for more than one *** this paper,the details of the design and performance of WcDA++are presented.

关键词： LHAASO-WcDA WcDA++ Water cherenkov detector Performance

Performance 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 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 Z.c.Huang F.ji X.L.ji H.Y.jia K.jiang Z.j.jiang c.jin D.Kuleshov K.Levochkin B.B.Li c.Li c.Li F.Li H.B.Li H.c.Li H.Y.Li j.Li K.Li W.L.Li X.Li X.Li X.R.Li Y.Li Y.Z.Li Z.Li Z.Li E.W.Liang Y.F.Liang S.j.Lin B.Liu c.Liu D.Liu H.Liu H.D.Liu j.Liu j.L.Liu j.S.Liu j.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.N.Liu Z.X.Liu W.j.Long R.Lu H.K.Lv B.Q.Ma L.L.Ma X.H.Ma j.R.Mao A.Masood W.Mitthumsiri T.Montaruli Y.c.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi B.Q.Qiao D.Ruffolo V.Rulev A.Saiz L.Shao O.Shchegolev X.D.Sheng j.R.Shi H.c.Song Yu.V.Stenkin V.Stepanov Q.N.Sun X.N.Sun Z.B.Sun P.H.T.Tam Z.B.Tang W.W.Tian B.D.Wang c.Wang H.Wang H.G.Wang j.c.Wang j.S.Wang L.P.Wang L.Y.Wang R.N.Wang W.Wang W.Wang X.G.Wang X.j.Wang X.Y.Wang Y.D.Wang Y.j.Wang Y.P.Wang Z.Wang Z.Wang Z.H.Wang Z.X.Wang D.M.Wei j.j.Wei Y.j.Wei T.Wen c.Y.Wu H.R.Wu S.Wu W.X.Wu X.F.Wu S.Q.Xi j.Xia j.j.Xia G.M.Xiang G.Xiao H.B.Xiao G.G.Xin Y.L.Xin Y.Xing D.L.Xu R.X.Xu L.Xue D.H.Yan c.W.Yang F.F.Yang j.Y.Yang L.L.Yang M.j.Yang R.Z.Yang S.B.Yang Y.H.Yao Z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.D.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha X.X.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang j.L.Zhang j.W.Zhang L.Zhang L.Zhang L.X.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhang X.Zhang X.P.Zhang Y.Zhang Y.Zhang Y.F.Zhang Y.L.Zhang B.Zhao j.Zhao L.Zhao L.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou j.N.Zhou Key Laboratory of Particle Astrophyics&Experimental Physics 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 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 for Astrophysics Guangzhou UniversityGuangzhou 510006China School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519082China School of Physical Science and Technology Guangxi UniversityNanning 530004China hebei Normal University Shijiazhuang 050024China School of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 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&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China college of Physics Sichuan UniversityChengdu 610065China Key Laboratory of cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China School of Physics and Technology Wuhan UniversityWuhan 430072China School of Physics and Astronomy Yunnan University

The first Water cherenkov detector of the LHAASO experiment(WcDA-1)has been operating since April *** data for the first year have been analyzed to test its performance 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 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 *** 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 found to be 33%for gamma rays around 6 *** 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.

关键词： LHAASO-WcDA crab Nebula angular resolution spectral energy distribution

Prospects for 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 Zhe cao Zhen 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 Danzengluobu B.D'Ettorre Piazzoli j.Fang j.H.Fan Y.Z.Fan c.F Feng L.Feng S.H.Feng Y.L.Feng 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.jia K.jiang F.ji c.jin X.L.ji 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.Pattarakijwanich Z.Y.Pei B.Q.Qiao M.Y.Qi D.Ruffolo 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.jiang H.D.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha B.B.Zhang H.M.Zhang H.Y.Zhang j.L.Zhang j.W.Zhang L.Zhang P.F.Zhang P.P.Zhang S.R.Zhang S.S.Zhang X.Zhang X.P.Zhang Yi Zhang Yong Zhang Y.F.g Zhang B.Zhao j.Zhao L.Zhao L.Z.Zhao F.Zheng Y.Zheng j.N.Zhou P.Zhou R.Zhou X.X.Zhou c.G.Zhu F.R.Zhu H.Zhu K.j.Zhu X.Zuo Institute of High Energy Physics Chinese Academy of SciencesBeijing 100049China University of chinese Academy of Sciences Beijing 100049China TIANFU 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 for 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 Nanjing University 210023 NanjingJiangsuChina Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of Sciences210034 NanjingJiangsuChina Institute of Frontier 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 for Nuclear Research Russian Academy of SciencesMoscowRussia Département de Physique Nucléaire et corpusculaire Facultéde SciencesUniversitéde GenéveGenevaSwitzerland Department of Physics Faculty of ScienceMahidol UniversityBangkokThailand Dublin Institute for Advanced Studies 31 Fitzwilliam PlaceDublin 2Ireland Max-Planc

The Water cherenkov Detector Array(WcDA) is a major 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 for TeV γ-ray sources with WcDA, we present a projection of the one-year sensitivity of WcDA to TeV γ-ray sources from TeVcat using an all-sky approach. Out of 128 TeVcat sources observable by WcDA up to a zenith 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

Nano high-entropy oxide cathode with enhanced stability for direct borohydride fuel cells

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journal of Energy chemistry 2025年第1期100卷 309-316页

作者： Lei Zhang Lingfeng Kuang Lianke Zhang Wen chu Haiying Qin jing Zhang junjing he Hualiang Ni Hongzhong chi New Energy Materials Research center College of Materials and Environmental Engineering Hangzhou Dianzi University School of Materials Science and Engineering Zhejiang University Key Laboratory of MEMS of Ministry of Education School of Integrated Circuits Southeast University

High-entropy materials have become high-activity electrocatalysis owing to their high-entropy effect and multiple active ***,we synthesize a series of carbon-supported nano high-entropy oxides（heOs/c）,specifically （PtFecoNicu）O/c,using a carbothermal shock （cTS） method for application as a cathode catalyst in direct borohydride fuel cells （DBFcs）.The microstructure of the prepared catalysts was characterized by X-ray photoelectron spectroscopy,X-ray absorption fine structure,and transmission electron *** prepared （PtFecoNicu）O/c,with particle sizes ranging from 2 to 4 nm,demonstrates 3.94 transferred electrons towards the oxygen reduction reaction in an alkaline environment,resulting in a minimal H2O2yield of 2.6%.Additionally,it exhibits a Tafel slope of 61 mV dec-1,surpassing that of commercial Pt/c (82 mV dec-1).Furthermore,after 40,000 cycles of cyclic voltammetry（cV） testing,the half-wave potential of （PtFecoNicu）O/c shows a positive shift of 3 mV,with no notable decline in the limiting current *** （PtFecoNicu）O/c is used as a cathode catalyst in DBFcs,the DBFc achieves a maximum power density of 441 mW cm-2at 60°c and sustains a cell voltage of approximately 0.73 V after 52 h at 30°*** findings confirm that heO/c is a promising cathode catalyst for DBFcs.

关键词： Direct borohydride fuel cells (DBFc)

Preparation and study of novel mid-to-low-temperature phase-change molten salts

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Science china Technological Sciences 2025年

作者： chenxing REN Yifan WANG Xin he chenghang ZheNG Xiang GAO State Key Laboratory of clean Energy Utilization Zhejiang University Institute of carbon Neutrality Zhejiang University Baima Lake Laboratory Zhejiang University

Molten salts is a promising medium for heat storage and heat transfer due to their advantages of low cost, low steam pressure, high energy storage density and wide temperature range. In this paper, a new phase change mixture of molten salts with KNO3, NaNO3, Zncl2, NaF, Na2cO3, Nacl, and MgO as materials has been prepared through a plenty of experiments. The experimental results show that the melting point of some molten salts can be reduced to 202.9°c, and the decomposition temperature can reach 701.3°c. In addition, its thermophysical properties, including specific heat, viscosity and thermal stability, were measured and analyzed. The average specific heat of some molten salts is as high as 2.53 j/（g K）, and the average thermal conductivity is as high as 0.77 W/（m K）. In the 4-day short-term thermal stability test, the fluctuation of each parameter is minimal, and the overall thermal physical property is relatively stable. compared with the traditional phase change molten salt, the new hybrid molten salt has a significantly lower melting point, a further improvement in the decomposition temperature, specific heat and other comprehensive thermophysical properties, and a better overall economy, which has important application value in heat transfer and energy storage.

关键词：

A functional tacrolimus-releasing nerve wrap for enhancing nerve regeneration following surgical nerve repair

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Neural Regeneration Research 2025年第1期20卷 291-304页

作者： Simeon c.Daeschler Katelyn j.W.So Konstantin Feinberg Marina Manoraj jenny cheung jennifer Zhang Kaveh Mirmoeini jPaul Santerre Tessa Gordon Gregory HBorschel SickKids Research Institute Neuroscience and Mental Health ProgramTorontoONCanada Institute of Biomaterials and Biomedical Engineering University of TorontoTorontoONCanada Indiana University School of Medicine IndianapolisINUSA Division of Plastic and Reconstructive Surgery the Hospital for Sick ChildrenTorontoONCanada Translational Biology and Engineering Program Ted Rogers Centre for Heart ResearchInstitute of Biomedical EngineeringFaculty of DentistryUniversity of TorontoTorontoONCanada

Axonal regeneration following surgical nerve repair is slow and often incomplete,resulting in poor functional recovery which sometimes contributes to lifelong ***,there are no FDA-approved therapies available to promote nerve *** accelerates axonal regeneration,but systemic side effects presently outweigh its potential benefits for peripheral nerve *** authors describe herein a biodegradable polyurethane-based drug delivery system for the sustained local release of tacrolimus at the nerve repair site,with suitable properties for scalable production and clinical application,aiming to promote nerve regeneration and functional recovery with minimal systemic drug *** is encapsulated into co-axially electrospun polycarbonate-urethane nanofibers to generate an implantable nerve wrap that releases therapeutic doses of bioactive tacrolimus over 31 *** and drug loading are adjustable for applications in small and large caliber nerves,and the wrap degrades within 120 days into biocompatible *** released from the nerve wrap promotes axon elongation in vitro and accelerates nerve regeneration and functional recovery in preclinical nerve repair models while off-target systemic drug exposure is reduced by 80%compared with systemic *** its surgical suitability and preclinical efficacy and safety,this system may provide a readily translatable approach to support axonal regeneration and recovery in patients undergoing nerve surgery.

关键词： biodegradable local drug delivery nerve injury nerve regeneration nerve wrap tacrolimus