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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

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

Octupole Deformation bands of πh_(11/2) in Neutron-Rich 145,147La Nuclei

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Chinese Physics Letters 1999年第3期16卷 169-171页

作者： zhU sheng-jiang WANG Mu-ge j.h.hamilton A.V.Ramayya b.R.s.babu W.C.Ma LONG Gui-lu zhU Ling-yan LI Ming A.sakhaee GAN Cui-yun YANG Li-ming j.Komicki j.D.Cole R.Aryaeinejad M.W.Drigert j.O.Rasmussen M.A.stoyer s.Y.Chu K.E.Gregorich M.F.Mohar s.G.Prussin I.Y.Lee Yu.Ts.Oganessian G.M.Ter-Akopian A.V.Daniel Department of Physics Tsinghua UniversityBeijing 100084 Department of Physics Vanderbilt UniversityNashvilleTN 37235USA Department of Physics Mississippi State UniversityMS 39762USA Idaho National Engineering Laboratory Idaho FallsID 83415USA Lawrence berkeley Laboratory BerkeleyCA 94720USA joint Institute for Nuclear Research Dubna 141980Russia

Octupole deformation bands built onπh ll/2 orbital in neutron-rich odd-z 145,147La nuclei have been investigated by measuring the promptγ-rays emitted from the 252Cf *** alternating parity band structures and strong E1 transitions observed between negative-and positive-parity bands in both nuclei indicate the octupole deformation enhanced by the h ll/2 single proton *** to observed energy displacements the octupole deformation becomes stable at the intermediate spin states.

关键词： coupling. bands parity

structure determination for small precipitates in high-strength aluminum

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Structure determination for small precipitates in high-stren...

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

全国有色金属理化检验学术报告会

作者： j.h.Chen~*,C.L.Wu~**,Y.h.jiang~***,s.b.Wang~****,j.z.Liu~***** * Center for high-Resolution Electron Microscopy,College of Materials science and Engineering,hunan University,Changsha City 410082,China

We firstly highlight some of recent techniques in modern transmission electron microscopy (TEM).These include through-focus exit-wavefunction reconstruction(TF-EWR) in high-resolution TEM(hRTEM),hRTEM with a spherical aberration(Cs) corrector for the objective lens,high-angle annular dark-field(hAADF) scanning TEM(hAADF sTEM). Then by examples,we demonstrate our practices of using these techniques,in association

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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

study of bEsIII trigger efficiencies with the 2018 j/ψ data

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Chinese Physics C 2021年第2期45卷 48-55页

作者： M.Ablikim M.N.Achasov P.Adlarson s.Ahmed M.Albrecht R.Aliberti A.Amoroso M.R.An Q.An X.h.bai Y.bai O.bakina R.baldini Ferroli I.balossino Y.ban K.begzsuren N.berger M.bertani D.bettoni F.bianchi j.bloms A.bortone I.boyko R.A.briere h.Cai X.Cai A.Calcaterra G.F.Cao N.Cao s.A.Cetin j.F.Chang W.L.Chang G.Chelkov D.Y.Chen G.Chen h.s.Chen M.L.Chen s.j.Chen X.R.Chen Y.b.Chen z.j Chen W.s.Cheng G.Cibinetto F.Cossio X.F.Cui h.L.Dai X.C.Dai A.Dbeyssi R.E.de boer D.Dedovich z.Y.Deng A.Denig I.Denysenko M.Destefanis F.De Mori Y.Ding C.Dong j.Dong L.Y.Dong M.Y.Dong X.Dong s.X.Du Y.L.Fan j.Fang s.s.Fang Y.Fang R.Farinelli L.Fava F.Feldbauer G.Felici C.Q.Feng j.h.Feng M.Fritsch C.D.Fu Y.Gao Y.Gao Y.Gao Y.G.Gao I.Garzia P.T.Ge C.Geng E.M.Gersabeck A Gilman K.Goetzen L.Gong W.X.Gong W.Gradl M.Greco L.M.Gu M.h.Gu s.Gu Y.T.Gu C.Y Guan A.Q.Guo L.b.Guo R.P.Guo Y.P.Guo A.Guskov T.T.han W.Y.han X.Q.hao F.A.harris h hüsken K.L.he F.h.heinsius C.h.heinz T.held Y.K.heng C.herold M.himmelreich T.holtmann Y.R.hou z.L.hou h.M.hu j.F.hu T.hu Y.hu G.s.huang L.Q.huang X.T.huang Y.P.huang z.huang T.hussain W.Ikegami Andersson W.Imoehl M.Irshad s.jaeger s.janchiv Q.ji Q.P.ji X.b.ji X.L.ji h.b.jiang X.s.jiang j.b.jiao z.jiao s.jin Y.jin T.johansson N.Kalantar-Nayestanaki X.s.Kang R.Kappert M.Kavatsyuk b.C.Ke I.K.Keshk A.Khoukaz P.Kiese R.Kiuchi R.Kliemt L.Koch O.b.Kolcu b.Kopf M.Kuemmel M.Kuessner A.Kupsc M.G.Kurth W.Kühn j.j.Lane j.s.Lange P.Larin A.Lavania L.Lavezzi z.h.Lei h.Leithoff M.Lellmann T.Lenz C.Li C.h.Li Cheng Li D.M.Li F.Li G.Li h.Li h.Li h.b.Li h.j.Li j.L.Li j.Q.Li j.s.Li Ke Li L.K.Li Lei Li P.R.Li s.Y.Li W.D.Li W.G.Li X.h.Li X.L.Li z.Y.Li h.Liang h.Liang h.Liang Y.F.Liang Y.T.Liang L.z.Liao j.Libby C.X.Lin b.j.Liu C.X.Liu D.Liu F.h.Liu Fang Liu Feng Liu h.b.Liu h.M.Liu huanhuan Liu huihui Liu j.b.Liu j.L.Liu j.Y.Liu K.Liu K.Y.Liu Ke Liu L.Liu M.h.Liu P.L.Liu Q.Liu Q.Liu s.b.Liu shuai Liu T.Liu W.M.Liu X.Liu Y.Liu Y.b.Liu z.A.Liu z.Q.Liu X.C.Lou F.X.Lu h.j.Lu j.D.Lu j.G.Lu X.L.Lu Y.Lu Y.P.Lu C.L.Luo M.X.Luo b P.W.Luo T.Luo X.L.Luo s Institute of high Energy Physics Beijing 100049China beihang University Beijing 100191China beijing Institute of Petrochemical Technology Beijing 102617China bochum Ruhr-University D-44780 BochumGermany Carnegie Mellon University PittsburghPennsylvania 15213USA Central China Normal University Wuhan 430079China China Center of Advanced science and Technology Beijing 100190China COMsATs University Islamabad Lahore CampusDefence RoadOff Raiwind Road54000 LahorePakistan Fudan University Shanghai 200443China GIbudker Institute of Nuclear Physics sb RAs(bINP) Novosibirsk 630090Russia GsI helmholtzcentre for heavy Ion Research Gmbh D-64291 DarmstadtGermany Guangxi Normal University Guilin 541004China Guangxi University Nanning 530004China hangzhou Normal University Hangzhou 310036China helmholtz Institute Mainz Johann-Joachim-Becher-Weg 45D-55099 MainzGermany henan Normal University Xinxiang 453007China henan University of science and Technology Luoyang 471003China huangshan College Huangshan 245000China hunan Normal University Changsha 410081China hunan University Changsha 410082China Indian Institute of Technology Madras Chennai 600036India Indiana University BloomingtonIndiana 47405USA (A)INFN Laboratori Nazionali di Frascati I-00044FrascatiItaly(B)INFN Sezione di PerugiaI-06100PerugiaItaly(C)University of PerugiaI-06100PerugiaItaly (A)INFN sezione di Ferrara I-44122FerraraItaly(B)University of FerraraI-44122FerraraItaly Institute of Modern Physics Lanzhou 730000China Institute of Physics and Technology Peace Ave54BUlaanbaatar 13330Mongolia jilin University Changchun 130012China johannes Gutenberg University of Mainz Johann-Joachim-Becher-Weg 45D-55099 MainzGermany joint Institute for Nuclear Research 141980 DubnaMoscow regionRussia justus-Liebig-Universitaet Giessen IIPhysikalisches InstitutHeinrich-Buff-Ring 16D-35392GiessenGermany KVI-CART University of GroningenNL-9747 AA GroningenThe Netherlands Lanzhou University Lanzhou 730000China Liaoning Normal Unive

Using a dedicated data sample taken in 2018 on the j/ψpeak,we perform a detailed study of the trigger efficiencies of the bEsIII *** efficiencies are determined from three representative physics processes,namely bhabha scattering,dimuon production and generic hadronic events with charged *** combined efficiency of all active triggers approaches 100%in most cases,with uncertainties small enough not to affect most physics analyses.

关键词： bEsIII trigger efficiency bhabha dimuon hadronic events

Antineutrino energy spectrum unfolding based on the Daya bay measurement and its applications

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Chinese Physics C 2021年第7期45卷 1-19页

作者： F.P.An A.b.balantekin M.bishai s.blyth G.F.Cao j.Cao j.F.Chang Y.Chang h.s.Chen s.M.Chen Y.Chen Y.X.Chen j.Cheng z.K.Cheng j.j.Cherwinka M.C.Chu j.P.Cummings O.Dalager F.s.Deng Y.Y.Ding M.V.Diwan T.Dohnal D.Dolzhikov j.Dove M.Dvorak D.A.Dwyer j.P.Gallo M.Gonchar G.h.Gong h.Gong M.Grassi W.Q.Gu j.Y.Guo L.Guo X.h.Guo Y.h.Guo z.Guo R.W.hackenburg s.hans a M.he K.M.heeger Y.K.heng Y.K.hor Y.b.hsiung b.z.hu j.R.hu T.hu z.j.hu h.X.huang j.h.huang X.T.huang Y.b.huang P.huber D.E.jaffe K.L.jen X.L.ji X.P.ji R.A.johnson D.jones L.Kang s.h.Kettel s.Kohn M.Kramer T.j.Langford j.Lee j.h.C.Lee R.T.Lei R.Leitner j.K.C.Leung F.Li h.L.Li j.j.Li Q.j.Li R.h.Li s.Li s.C.Li W.D.Li X.N.Li X.Q.Li Y.F.Li z.b.Li h.Liang C.j.Lin G.L.Lin s.Lin j.j.Ling j.M.Link26 L.Littenberg b.R.Littlejohn j.C.Liu j.L.Liu j.X.Liu C.Lu h.Q.Lu K.b.Luk b.z.Ma X.b.Ma X.Y.Ma Y.Q.Ma R.C.Mandujano C.Marshall K.T.McDonald R.D.McKeown Y.Meng j.Napolitano D.Naumov E.Naumova T.M.T.Nguyen j.P.Ochoa-Ricoux A.Olshevskiy h.-R.Pan j.Park s.Patton j.C.Peng C.s.j.Pun F.z.Qi M.Qi X.Qian N.Raper j.Ren C.Morales Reveco R.Rosero b.Roskovec X.C.Ruan h.steiner j.L.sun T.Tmej1 K.Treskov W.-h.Tse C.E.Tull b.Viren V.Vorobel C.h.Wang j.Wang M.Wang N.Y.Wang R.G.Wang W.Wang W.Wang X.Wang Y.Wang Y.F.Wang z.Wang z.Wang z.M.Wang h.Y.Wei L.h.Wei L.j.Wen K.Whisnant C.G.White h.L.h.Wong E.Worcester D.R.Wu F.L.Wu Q.Wu W.j.Wu D.M.Xia z.Q.Xie z.z.Xing h.K.Xu j.L.Xu T.Xu T.Xue C.G.Yang L.Yang Y.z.Yang h.F.Yao M.Ye M.Yeh b.L.Young h.z.Yu z.Y.Yu b.b.Yue V.zavadskyi s.zeng Y.zeng L.zhan C.zhang F.Y.zhang h.h.zhang j.W.zhang Q.M.zhang s.Q.zhang X.T.zhang Y.M.zhang Y.X.zhang Y.Y.zhang z.j.zhang z.P.zhang z.Y.zhang j.zhao R.z.zhao L.zhou h.L.zhuang j.h.zou Institute of Modern Physics East China University of Science and TechnologyShanghai 200337 University of Wisconsin MadisonWisconsin 53706 brookhaven National Laboratory UptonNew York 11973 Department of Physics Nnational Taiwan UniversityTaipei Institute of high Energy Physics Beijing 100049 National United University Miao-Li Department of Engineering Physics Tsinghua UniversityBeijing 100048 shenzhen University Shenzhen 518061 sun Yat-sen(zhongshan)University Guangzhou 510275 North China Electric Power University Beijing 102206 Chinese University of hong Kong Hongkong 999077 siena College LoudonvilleNew York 12211 Department of Physics and Astronomy University of CaliforniaIrvineCalifornia 92697 University of science and Technology of China Hefei 230022 Charles University Faculty of Mathematics and PhysicsPrague joint Institute for Nuclear Research DubnaMoscow Region Department of Physics University of Illinois at Urbana-ChampaignUrbanaIllinois 61801 Lawrence berkeley National Laboratory BerkeleyCalifornia 94720 Department of Physics Illinois Institute of TechnologyChicagoIllinois 60616 beijing Normal University Beijing 100875 Department of Nuclear science and Technology School of Energy and Power EngineeringXi'an Jiaotong UniversityXi'an 710049 Wright Laboratory and Department of Physics Yale UniversityNew HavenConnecticut 06520 China Institute of Atomic Energy Beijing 102413 shandong University Jinan 250002 Guangxi University No.100 Daxue East RoadNanning 530004 Center for Neutrino Physics Virginia TechBlacksburgVirginia 24061 Institute of Physics NCTUHsinchu Department of Physics University of CincinnatiCincinnatiOhio 45221 Department of Physics College of Science and TechnologyTemple UniversityPhiladelphiaPennsylvania 19122 Dongguan University of Technology Dongguan 523808 Department of Physics University of CaliforniaBerkeleyCalifornia 94720 Department of Physics The University of Hong KongPokfulamHongkong 999077 school of Physics Nankai UniversityTianjin 300071 Department o

The prediction of reactor antineutrino spectra will play a crucial role as reactor experiments enter the precision *** positron energy spectrum of 3.5 million antineutrino inverse beta decay reactions observed by the Daya bay experiment,in combination with the fission rates of fissile isotopes in the reactor,is used to extract the positron energy spectra resulting from the fission of specific *** information can be used to produce a precise,data-based prediction of the antineutrino energy spectrum in other reactor antineutrino experiments with different fission fractions than Daya *** positron energy spectra are unfolded to obtain the antineutrino energy spectra by removing the contribution from detector response with the Wiener-sVD unfolding *** results are obtained with other unfolding methods.A technique to construct a data-based prediction of the reactor antineutrino energy spectrum is proposed and *** the reactor fission fractions,the technique can predict the energy spectrum to a 2%*** addition,we illustrate how to perform a rigorous comparison between the unfolded antineutrino spectrum and a theoretical model prediction that avoids the input model bias of the unfolding method.

关键词： reactor antineutrino energy spectrum Daya bay application

NUCLEATION AND GROWTh OF ＜111＞ ORIENTATION hOMOEPITAXIAL DIAMOND MONOCRYsTAL

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NUCLEATION AND GROWTH OF ＜111＞ ORIENTATION HOMOEPITAXIAL D...

AN INVEsTIGATION ON（100）MONOEPITAXIAL DIAMOND MONOCRYsTALLINE FILMs

sixteenth Congress of the International Union of Crystallography

作者： z.M.zhang s.h.Li Q.Y.Cai h.M.Chen X.C.he D.L.Ling s.j.Wang z.W.hu s.s.jiang C.z.Ge N.b.Ming shanghai jiao Tong Univ. Nanjing Univ.

＜正＞It has been reported that only polycrystal diamond film could be formed on beteroepitaxial substrate by CVD method,which stimulated great interesting to grow homoepitaxial film,however, few reports concerned the growth on ＜111＞ oriented *** this paper,a successful growth of homoepitaxy on（111） natural diamond substrate is presented by using microwave PCVD method. The experimental process was almost same as that of（100） homoepitaxy reported before.

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AN INVESTIGATION ON（100）MONOEPITAXIAL DIAMOND MONOCRYSTALL...