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Observation of the Crab Nebula with LhAASO-KM2A−a performance study

1996 3rd International Conference on Signal Processing(ICSP’96)

作者： h.r.wu M.Yuen B.Qiu Department of Digital Systems Monash UniversityWellington RoadClayton 3168Australia.

(Invited Paper) *** Currently,various video compression and coding standards have adopted the hybrid algorithm which deploys motion compensation,temporal differential pulse code modulation and the block discrete cosine transform(MC/DPCM/DCT) with associated adaptive quantization and entropy coding algorithms[1]. Video sequences coded by either hardware or software

关键词： Video coding Code standards Pulse modulation Discrete cosine transforms Image reconstruction Video compression Motion compensation Pulse compression methods Modulation coding Quantization

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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

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

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

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

reconstruction of Cherenkov image bymultiple telescopes of LhAASO-WFCTA

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radiation Detection Technology and Methods 2022年第4期6卷 544-557页

作者： F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi J.T.Cai Zhe Cao Zhen Cao J.Chang J.F.Chang E.S.Chen Liang Chen Liang Chen Long Chen M.J.Chen M.L.Chen Q.h.Chen S.h.Chen S.Z.Chen T.L.Chen Y.Chen h.L.Cheng N.Cheng Y.D.Cheng S.W.Cui X.h.Cui Y.D.Cui B.D’Ettorre Piazzoli B.Z.Dai h.L.Dai Z.G.Dai Danzengluobu Ddella Volpe K.K.Duan J.h.Fan Y.Z.Fan Z.X.Fan J.Fang K.Fang C.F.Feng L.Feng S.h.Feng X.T.Feng Y.L.Feng B.Gao C.D.Gao L.Q.Gao Q.Gao W.Gao W.K.Gao M.M.Ge L.S.Geng G.h.Gong Q.B.Gou M.h.Gu F.L.Guo J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.han h.h.he h.N.he S.L.he X.B.he Y.he M.heller Y.K.hor C.hou X.hou h.B.hu Q.hu S.hu S.C.hu X.J.hu D.h.huang W.h.huang X.T.huang X.Y.huang Y.huang Z.C.huang X.L.Ji h.Y.Jia K.Jia K.Jiang Z.J.Jiang M.Jin M.M.Kang T.Ke D.Kuleshov K.Levochkin B.B.Li Cheng Li Cong Li F.Li h.B.Li h.C.Li h.Y.Li J.Li Jian Li Jie Li K.Li WLLi XrLi Xin Li Xin Li YZLi Zhe Li Zhuo Li E.W.Liang Y.F.Liang S.J.Lin B.Liu C.Liu D.Liu h.Liu h.D.Liu J.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu r.Y.Liu S.M.Liu W.Liu Y.Liu Y.N.Liu W.J.Long r.Lu Q.Luo h.K.Lv B.Q.Ma L.L.Ma X.h.Ma J.r.Mao A.Masood Z.Min W.Mitthumsiri Y.C.Nan Z.W.Ou B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi Y.Q.Qi B.Q.Qiao J.J.Qin D.ruffolo A.Sáiz C.Y.Shao L.Shao O.Shchegolev X.D.Sheng J.Y.Shi h.C.Song Yu.V.Stenkin V.Stepanov Y.Su Q.N.Sun X.N.Sun Z.B.Sun P.h.T.Tam Z.B.Tang W.W.Tian B.D.Wang C.Wang h.Wang h.G.Wang J.C.Wang J.S.Wang L.P.Wang L.Y.Wang r.Wang r.N.Wang W.Wang X.G.Wang X.Y.Wang Y.Wang Y.D.Wang Y.J.Wang Y.P.Wang Z.h.Wang Z.X.Wang Zhen Wang Zheng Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.wu h.r.wu S.wu X.F.wu Y.S.wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang D.X.Xiao G.Xiao G.G.Xin Y.L.Xin Y.Xing Z.Xiong D.L.Xu r.X.Xu L.Xue D.h.Yan J.Z.Yan C.W.Yang F.F.Yang h.W.Yang J.Y.Yang L.L.Yang M.J.Yang r.Z.Yang S.B.Yang Y.h.Yao Z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.h.You Z.Y.You Y.h.Yu Q.Yuan h.Yue h.D.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha X.X.Zhai B.B.Zhang F.Zhang h.M.Zhang h.Y.Zhang J.L.Zhang L.X.Zhang Li Zhang Lu Zhang P.F.Zhang P.P.Zhang r.Zhang S.B.Zhang S.r.Zhang S. Key Laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic ray research Center ChengduSichuanChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 10398069029 HeidelbergGermany State Key Laboratory of Particle Detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Key Laboratory for research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Cosmic rays(Tibet University) Ministry of EducationLhasa 850000TibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and Astronomy(Zhuhai)&Sino-French Institute of Nuclear Engineering and Technology(Zhuhai) Sun Yat-sen UniversityZhuhai 519000China School of Physics(Guangzhou) Sun Yat-sen UniversityGuangzhou 510275GuangdongChina Dipartimento di Fisica dell’Universitàdi Napoli“Federico II” Complesso Universitario di Monte Sant’Angelovia Cinthia80126 NapoliItaly School of Physics and Astronomy Yunnan UniversityKunming 650091YunnanChina Département de Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève

Introduction One of main scientiﬁc goals of the Large high Altitude Air Shower Observatory(LhAASO)is to accurately measure the energy spectra of different cosmic ray compositions around the‘knee’*** Wide Field-of-View(FoV)Cherenkov Telescope Array(WFCTA),which is one of the main detectors of LhAASO and has 18 telescopes,is built to achieve this *** telescopes are put together and point to connected directions for a larger *** Telescopes are deployed spatially as close as possible,but due to their own size,the distance between two adjacent telescopes is about 10 ***,the Cherenkov lateral distribution and the parallax between the two telescopes should be considered in the event building process for images crossing over the boundaries of FoVs of the *** event building method for Cherenkov images measured by multiple telescopes of WFCTA is *** performance of the shower measurements using the combined images is evaluated by comparing with showers that are fully contained by a virtual telescope in *** and conclusion It is proved that the developed event building process can help to increase the FoV of WFCTA by 30%while maintaining the same reconstruction quality,compared to the separate telescope reconstruction method.

关键词： method directions conclusion

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： Zhen 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 Zhe 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 Danzengluobu X.Q.Dong K.K.Duan J.h.Fan Y.Z.Fan J.Fang K.Fang C.F.Feng L.Feng S.h.Feng X.T.Feng Y.L.Feng 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.Ji h.Y.Jia K.Jia K.Jiang X.W.Jiang Z.J.Jiang M.Jin 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 Jian Li Jie Li K.Li W.L.Li W.L.Li X.r.Li Xin Li Y.Z.Li Zhe Li Zhuo Li E.W.Liang Y.F.Liang S.J.Lin B.Liu 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.Luo h.K.Lv B.Q.Ma L.L.Ma X.h.Ma J.r.Mao Z.Min W.Mitthumsiri h.J.Mu Y.C.Nan A.Neronov 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 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 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.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.Zeng T.X.Zeng W.Zeng M.Zha B.B.Zhang F.Zhang h.M.Zhang h.Y.Zhang J.L.Zhang L.X.Zhang Li Zhang P.F.Zhang P.P.Zhang r.Zhang S.B.Zh 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 TIANFU Cosmic ray research Center ChengduSichuanChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institute for 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 Information Science and Technology Southwest Jiaotong UniversityChengdu610031SichuanChina School of Astronomy and Space Science Nanjing UniversityNanjing210023JiangsuChina Center for 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 for research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Cosmic rays(Tibet University) Ministry of EducationLhasa 850000TibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Physics and Astronomy(Zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(Zhuhai) Sun Yat-sen UniversityGuangzhouZhuhai 510275519000GuangdongChina School of Physics and Astronomy Yunnan UniversityKunming 650091YunnanChina Institute of Frontier 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 foundation for estimating detector performance and data *** is a big challenge to simulate the KM2A detector in the framework of Geant4 due to the need to track numerous photons from a large number of detector units(>6000)with large altitude difference(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 optimized mainly in memory consumption to avoid memory *** simplifications are used to significantly speed up the execution of *** running time is reduced by at least 30 times compared to full detector *** particle distributions and the core/angle resolution comparison between simulation and experimental data of the full KM2A array are also presented,which show good agreement.

关键词： LhAASO KM2A Simulation GEANT4

Nanostructured ZnO/BiVO_(4)I-scheme heterojunctions for piezocatalytic degradation of organic dyes via harvesting ultrasonic vibration energy

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International Journal of Minerals,Metallurgy and Materials 2025年第2期32卷 488-497页

作者： Yiling Li Xiaoyao Yu Yingjie Zhou Yao Lin Ying wu Key Laboratory of the Ministry of Education for Advanced Catalysis Materials College of Chemistry and Materials ScienceZhejiang Normal UniversityJinhua 321004China

BiVO_(4)porous spheres modified by ZnO were designed and synthesized using a facile two-step *** resulting ZnO/BiVO_(4)composite catalysts have shown remarkable efficiency as piezoelectric catalysts for degrading rhodamine B(rhB)unde mechanical vibrations,they exhibit superior activity compared to pure *** 40wt%ZnO/BiVO_(4)heterojunction composite displayed the highest activity,along with good stability and *** enhanced piezoelectric catalytic activity can be attributed to the form ation of an I-scheme heterojunction structure,which can effectively inhibit the electron-hole ***,hole(h+)and superoxide radical(·O_(2)^(-))are proved to be the primary active ***,ZnO/BiVO_(4)stands as an efficient and stable piezoelectric catalyst with broad potential application in the field of environmental water pollution treatment.

关键词： piezoelectric catalytic heterojunction dye degradation ultrasonic vibration