检索结果-南通市图书馆

A dynamic range extension system for LHAASOWCDA-1

在线全文

学校读者我要写书评

暂无评论

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

Prospects for a multi-TeV gamma-ray sky survey with the LHAASO water Cherenkov detector array

维普期刊数据库评论

在线全文

维普期刊数据库

学校读者我要写书评

暂无评论

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

Performance of LHAASO-WCDA and observation of the Crab Nebula as a standard candle

在线全文

学校读者我要写书评

暂无评论

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

Reconstruction of Cherenkov image bymultiple telescopes of LHAASO-WFCTA

在线全文

学校读者我要写书评

暂无评论

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

敲除大麻素Ⅱ型受体影响APP/PS1小鼠前额叶皮质小胶质细胞功能与激活PI3K/Akt/mTOR通路有关

维普期刊数据库评论

在线全文

维普期刊数据库

学校读者我要写书评

暂无评论

中国药理学与毒理学杂志 2022年第9期36卷 649-656页

作者：袁蜜蜜刘坤璐陈美桦陈浩正史敬璞李锦孙家广王勃军事科学院军事医学研究院毒物药物研究所抗毒药物与毒理学国家重点实验室北京100850 河北医科大学第四医院麻醉科河北石家庄050000 邢台市人民医院麻醉科河北邢台054000

目的研究大麻素Ⅱ型受体(CB2R)基因敲除对阿尔茨海默病(AD)小鼠发病前期空间学习与记忆能力的影响,并从分子水平探讨可能的作用机制。方法C57BL6/J小鼠根据基因型分为野生型对照组(WT)、CB2R敲除组(CB2^(-/-)),模型组(APP/PS1)和模型+C... 详细信息

目的研究大麻素Ⅱ型受体(CB2R)基因敲除对阿尔茨海默病(AD)小鼠发病前期空间学习与记忆能力的影响,并从分子水平探讨可能的作用机制。方法C57BL6/J小鼠根据基因型分为野生型对照组(WT)、CB2R敲除组(CB2^(-/-)),模型组(APP/PS1)和模型+CB2R敲除组(APP/PS1*CB2^(-/-)),采用Morris水迷宫实验检测4月龄小鼠的空间学习与记忆能力,ELISA检测小鼠脑内β淀粉样蛋白(Aβ)1-42和Aβ_(1-40)含量,实时荧光定量PCR法检测前额叶皮质和海马脑区炎症因子白细胞介素6(IL-6),肿瘤坏死因子α(TNF-α)和诱导型一氧化氮合酶(iNOS)mRNA表达水平,免疫荧光法检测小胶质细胞形态变化,Western印迹法检测小鼠脑内炎症相关信号通路中磷酯酰肌醇3激酶(PI3K)蛋白表达水平及蛋白激酶B(Akt)、哺乳动物雷帕霉素靶蛋白(mTOR)、细胞外信号调节激酶1/2(ERK1/2)和p38丝裂原活化蛋白激酶(p38 MAPK)蛋白磷酸化水平。结果与APP/PS1组相比,APP/PS1*CB2^(-/-)组小鼠在Morris水迷宫实验中的潜伏期、目标象限停留时间和穿台次数无显著差异,提示CB2R敲除并不影响APP/PS1小鼠的空间学习与记忆能力;与APP/PS1组相比,APP/PS1*CB2^(-/-)组小鼠前额叶皮质Aβ1-42含量和IL-6 mRNA表达水平均显著性升高(P<0.05);APP/PS1组小鼠前额叶皮质小胶质细胞形态呈阿米巴状样,APP/PS1*CB2^(-/-)组小鼠小胶质细胞形态发生明显改变,呈细长分支状;与APP/PS1组小鼠相比,APP/PS1*CB2^(-/-)组小鼠前额叶皮质PI3K蛋白表达水平及Akt和mTOR蛋白磷酸化水平显著升高(P<0.05),ERK1/2和p38 MAPK蛋白磷酸化水平无显著差异。结论CB2R敲除影响APP/PS1小鼠前额叶皮质小胶质细胞的功能,可能与激活PI3K/Akt/mTOR通路有关。

关键词：大麻素Ⅱ型受体阿尔茨海默病小胶质细胞神经源性炎症

在线全文

学校读者我要写书评

暂无评论

燕山地区叶底珠萌发期耐盐性综合评价

干旱区资源与环境 2023年第4期37卷 178-185页

作者：徐宁伟路斌陈强于晓跃柴诗瑶刘子扬路丙社河北农业大学园林与旅游学院保定071001 唐山学院艺术系唐山063000 浙江工业大学之江学院绍兴312030 河北师范大学生命科学学院石家庄050024

对河北燕山地区30份叶底珠材料种子萌发期进行耐盐性综合评价,以期为叶底珠的耐盐筛选提供理论依据,同时为盐渍化地区生态修复及园林植物的选择提供参考。在人工气候箱内用200mmol/L NaCl溶液进行盐胁迫,以蒸馏水培养为对照,对30份叶底... 详细信息

对河北燕山地区30份叶底珠材料种子萌发期进行耐盐性综合评价,以期为叶底珠的耐盐筛选提供理论依据,同时为盐渍化地区生态修复及园林植物的选择提供参考。在人工气候箱内用200mmol/L NaCl溶液进行盐胁迫,以蒸馏水培养为对照,对30份叶底珠材料种子萌发期的相对发芽率、相对发芽势、相对发芽指数、相对盐害率、相对胚根长、相对鲜重进行测定与计算,通过隶属函数分析和聚类分析进行综合评价,筛选耐盐材料。结果表明:盐胁迫下叶底珠种子的发芽率、发芽势、发芽指数、胚根长、鲜重等指标均受到不同程度的抑制,30份叶底珠材料种子萌发期的耐盐性有明显差异;在6个鉴定指标中,相对盐害率、发芽率与叶底珠萌发期的耐盐性关系最为密切;根据隶属函数分析和聚类分析,可将燕山地区30份叶底珠材料划分为高度耐盐型(6个)、耐盐型(5个)、中度耐盐型(3个)、盐敏感型(8个)和高敏感型(8个)5类。200mmol/L NaCl溶液可作为叶底珠种子萌发期耐盐性鉴定的适宜盐浓度;发芽率可作为叶底珠种子萌发期耐盐性快速鉴定或初步筛选的鉴定指标;隶属函数法对叶底珠种子萌发期耐盐性综合评价具有较好的应用价值。

关键词：叶底珠种子萌发期盐胁迫耐盐性综合评价

基于图论模型的乒乓球混双技战术分析与应用研究

在线全文

学校读者我要写书评

暂无评论

广州体育学院学报 2022年第3期42卷 110-117页

作者：曹烨程陈辉郭晨北京体育大学研究生院北京100084 石家庄学院体育学院河北石家庄050035 重庆第二师范学院体育与健康管理学院重庆400065 福建师范大学体育科学学院福建福州350117

本文旨在构建乒乓球混双技战术图论模型,为乒乓球混双比赛技战术分析提供新的研究方法。方法:应用文献资料法与录像观察法构建技战术分析指标体系,运用图论模型对高水平混双比赛的373个回合为研究案例,对比赛的发球方式、技战术运用、... 详细信息

本文旨在构建乒乓球混双技战术图论模型,为乒乓球混双比赛技战术分析提供新的研究方法。方法:应用文献资料法与录像观察法构建技战术分析指标体系,运用图论模型对高水平混双比赛的373个回合为研究案例,对比赛的发球方式、技战术运用、技战术衔接进行分析,应用图论模型构建乒乓球混双动态网络G=(V(G),E(G))。结果:通过计算节点的度和网络边数,得到混双运动员使用最频繁的技战术组合与下一板最有可能采用的回击方式。结论:两对混双选手都是在女子发球轮次占优,当男女运动员双方采用逆旋转发球方式时,获胜概率较高;刘诗雯和伊藤美诚在比赛中使用较多的技术线路组合分别是正手摆短斜线和反手拉斜线;许昕和水谷隼在出台球进攻上技术线路组合应用较多的是正手侧身拉斜线。

关键词：图论模型乒乓球混双技战术分析

3~6岁儿童等效球镜屈光度、眼球生物学参数情况及屈光发育异常影响因素分析

在线全文

学校读者我要写书评

暂无评论

临床误诊误治 2020年第8期33卷 85-90页

作者：宋艳霞王建仓陈璐杨素玲杨晓格陈少华刘丽芳河北医科大学附属河北省儿童医院眼科石家庄050000

目的探讨3~6岁儿童等效球镜屈光度、眼球生物学参数情况及屈光发育异常影响因素。方法选取符合纳入及排除标准的3~6岁儿童500例作为研究对象,观察3~6岁儿童屈光发育异常检出情况,比较不同性别、年龄及屈光状态3~6岁儿童等效球镜屈光度... 详细信息

目的探讨3~6岁儿童等效球镜屈光度、眼球生物学参数情况及屈光发育异常影响因素。方法选取符合纳入及排除标准的3~6岁儿童500例作为研究对象,观察3~6岁儿童屈光发育异常检出情况,比较不同性别、年龄及屈光状态3~6岁儿童等效球镜屈光度及眼球生物学参数情况,并采用单因素和多因素Logistic回归分析对3~6岁儿童屈光发育异常的影响因素进行分析。结果500例屈光异常检出率14.00%,其中远视52例,近视18例。屈光异常检出率3~4岁明显高于5~6岁,差异有统计学意义(P<0.05)。3~6岁儿童中男孩眼轴和角膜直径均长于女孩,差异有统计学意义(P<0.01)。与3~4岁比较,4~5岁和5~6岁等效球镜屈光度降低,眼轴增长;与4~5岁比较,5~6岁等效球镜屈光度降低,眼轴增长,差异有统计学意义(P<0.01)。远视患儿等效球镜屈光度高于正视儿童和近视患儿,眼轴短于正视儿童和近视患儿;正视儿童等效球镜屈光度高于近视患儿,眼轴短于近视患儿,差异均有统计学意义(P<0.01)。单因素分析结果显示,与屈光发育正常儿童比较,屈光发育异常儿童年龄相对较小,非足月生产、出生体质量<3 kg、每天户外活动时间<2 h以及每天近距离用眼时间≥2 h所占比例较高,差异有统计学意义(P<0.05或P<0.01)。多因素Logistic回归分析结果显示,非足月生产、出生体质量<3 kg、每天户外活动时间<2 h以及每天近距离用眼时间≥2 h为3~6岁儿童屈光发育异常的独立危险因素(P<0.05或P<0.01);年龄5~6岁是3~6岁儿童屈光发育异常的保护因素(P<0.05)。结论不同性别、年龄及屈光状态下,3~6岁儿童等效球镜屈光度和眼球生物学参数分布存在差异。非足月生产、出生体质量<3 kg、每天户外活动时间<2 h以及每天近距离用眼时间≥2 h为3~6岁儿童屈光发育异常的独立危险因素。

关键词：儿童,学龄前等效球镜屈光度眼球生物学参数分布屈光不正近视远视

在线全文

学校读者我要写书评

暂无评论

柱状金属锂沉积物:电解液添加剂的影响

物理化学学报 2021年第1期37卷 136-143页

作者：杨世杰徐向群程新兵王鑫萌陈金秀肖也袁洪刘鹤陈爱兵朱万诚黄佳琦张强北京理工大学材料学院北京100081 清华大学化学工程系绿色反应工程与工艺北京市重点实验室北京100084 北京理工大学前沿交叉科学研究院北京100081 河北科技大学化学与制药工程学院石家庄050018 曲阜师范大学化学与化工学院山东曲阜273165

二次电池的能量密度已成为推动电动汽车和便携式电子产品技术向前发展的重要指标。使用石墨负极的锂离子电池正接近其理论能量密度的天花板,但仍难以满足高端储能设备的需求。金属锂负极因其极高的理论比容量和极低的电极电位,受到了广... 详细信息

二次电池的能量密度已成为推动电动汽车和便携式电子产品技术向前发展的重要指标。使用石墨负极的锂离子电池正接近其理论能量密度的天花板,但仍难以满足高端储能设备的需求。金属锂负极因其极高的理论比容量和极低的电极电位,受到了广泛关注。然而,锂沉积过程中枝晶的生长会导致电池安全性差等问题。电解液对金属锂的沉积有着至关重要的影响。本文设计了一种独特的电解槽体系来进行柱状锂的沉积,研究了不同电解液体系(1mol·L^(-1)LiPF6-碳酸乙烯酯/碳酸二乙酯(EC/DEC,体积比为1:1)、1 mol·L^(-1) LiPF6-氟代碳酸乙烯酯(FEC,体积分数5%)-EC/DEC (体积比为1:1))对金属锂沉积的影响。对两种电解液中金属锂沉积物长径比的研究表明,电解液的组分可以显著地影响金属锂的沉积形貌,在加入氟代碳酸乙烯酯(FEC)添加剂之后,柱状锂的直径从0.3–0.6μm增加到0.7–1.3μm,长径比从12.5下降到5.6。长径比的降低有助于减小金属锂和电解液的反应面积,提高金属锂负极的利用率和循环寿命。通过考察循环后锂片的表面化学性质,发现FEC的分解增加了锂表面固态电解质界面层中氟化锂(LiF)组分的比例,提高了界面层中锂离子的扩散速率,减少了锂的成核位点,从而给予锂核更大的生长空间,降低了沉积出的柱状锂的长径比。

关键词：金属锂电池柱状锂电解液氟化锂长径比