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基于3D体素增强和3Dalpha背景分离的多发性硬化症病灶分割方法

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中国医学物理学杂志 2022年第7期39卷 834-839页

作者：孙颖张吟龙王鑫曾子铭毛海霞中国医科大学附属第一医院重症医学科辽宁沈阳110001 中国科学院沈阳自动化研究所辽宁沈阳110016 沈阳建筑大学信息与控制工程学院辽宁沈阳110168 深圳职业技术学院汽车与交通学院广东深圳518055

目的:提出一种用于T_(1)加权像、T_(2.加权像和流体衰减反演恢复(Flair)磁共振图像的多发性硬化症(MS)病变分割方法。方法:首先基于3D图像增强技术,将高强度MS病变区域与其他组织区域区分开来。然后利用假阳性降低方法,去除一些强度和... 详细信息

目的:提出一种用于T_(1)加权像、T_(2.加权像和流体衰减反演恢复(Flair)磁共振图像的多发性硬化症(MS)病变分割方法。方法:首先基于3D图像增强技术,将高强度MS病变区域与其他组织区域区分开来。然后利用假阳性降低方法,去除一些强度和密度不均匀的假阳性目标区域(VOI),并利用颜色分割法去除白质之外的VOI。最后利用彩色MR技术生成3个区域,以便细化分割MS病变。结果:在CHB数据集上进行测试,得到真阳率均值为0.48,Dice相似系数均值为0.52.结论:该方法能够有效去除噪声及其他无关非病变组织,并能准确识别并分割MS病变,该方法的有效性、准确性能为后续的MS分割技术分析提供依据。同时为MS病变的预防治疗、病情跟踪提供客观、方便的诊疗方法。

关键词：多发性硬化症病灶分割 3D体素增强 3Dalpha背景分离颜色分割技术

Persistent surface states with diminishing gap in MnBi_(2.Te_(4)/Bi_(2.Te_(3) superlattice antiferromagnetic topological insulator

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Science Bulletin 2020年第24期65卷 2086-2093,M0005页

作者： Lixuan Xu Yuanhao mao Hongyuan wang Jiaheng Li Yujie Chen Yunyouyou Xia Yiwei Li Ding Pei Jing Zhang Huijun Zheng Kui Huang Chaofan Zhang Shengtao Cui Aiji Liang Wei Xia Hao Su Sungwon Jung Cephise Cacho Meixiao wang Gang Li Yong Xu Yanfeng Guo Lexian Yang Zhongkai Liu Yulin Chen Mianheng Jiang Center for Excellence in Superconducting Electronics State Key Laboratory of Functional Material for InformaticsShanghai Institute of Microsystem and Information TechnologyChinese Academy of SciencesShanghai 200050China School of Physical Science and Technology ShanghaiTech University and CAS-Shanghai Science Research CenterShanghai 201210China ShanghaiTech Laboratory for Topological physics Shanghai 200031China university of Chinese Academy of Sciences Beijing 100049China college of Advanced Interdisciplinary Studies National University of Defense TechnologyChangsha 410073China State Key Laboratory of Low Dimensional Quantum physics Department of PhysicsTsinghua UniversityBeijing 100084China Department of physics Clarendon LaboratoryUniversity of OxfordOxford 0X13PUUK Advanced Light Source Lawrence Berkeley National LaboratoryBerkeleyCA 94720USA Diamond Light Source Harwell CampusDidcot 0X11 ODEUK Frontier Science Center for Quantum information Beijing 100084China RIKEN Center for Emergent Matter Science(CEMS) WakoSaitama 351-0198Japan

Magnetic topological quantum materials(TQMs) provide a fertile ground for the emergence of fascinating topological magneto-electric effects. Recently, the discovery of intrinsic antiferromagnetic(AFM) topological insulator MnBi_(2.Te_(4) that could realize quantized anomalous Hall effect and axion insulator phase ignited intensive study on this family of TQM compounds. Here, we investigated the AFM compound Mn Bi4 Te7 where Bi_(2.Te_(3) and MnBi_(2.Te_(4) layers alternate to form a superlattice. Using spatial-and angleresolved photoemission spectroscopy, we identified ubiquitous(albeit termination dependent) topological electronic structures from both Bi_(2.Te_(3) and MnBi_(2.Te_(4) terminations. Unexpectedly, while the bulk bands show strong temperature dependence correlated with the AFM transition, the topological surface states with a diminishing gap show negligible temperature dependence across the AFM *** with the results of its sister compound MnBi_(2.Te_(4), we illustrate important aspects of electronic structures and the effect of magnetic ordering in this family of magnetic TQMs.

关键词： Spatially resolved angle-resolved photoemission spectroscopy Electronic band structure Quantum anomalous Hall effect Magnetic topological insulator

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基于球面距离的K-means聚类任务打包

嘉兴学院学报 2019年第6期31卷 83-88页

作者：林萱毛钦辉王薇嘉兴学院数理与信息工程学院

针对深圳、广州、佛山等地大量“拍照赚钱”任务点打包问题,引入了基于球面距离的K-means聚类.考虑到K值的选择困难,算法对初始聚类中心的敏感性,对K-means聚类进行改进,聚类结果给出了较好的任务分配方案.

关键词： K-means 交替迭代算法球面距离任务打包

重组酵母菌N6076的差异表达基因功能及甲羟戊酸代谢分析

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食品与发酵工业 2020年第17期46卷 22-26页

作者：王璇欧科冯光文陈福欣王婷买买提热夏提·买买提钱卫东毛培宏新疆大学物理科学与技术学院放射生态与离子束生物技术中心新疆乌鲁木齐830046 西安科技大学化学与化工学院陕西西安710054 陕西科技大学食品与生物工程学院陕西西安710032

为了解重组酵母菌N6076不同发酵时间的差异表达基因信息及甲羟戊酸(mevalonate,MVA)代谢状况,以重组酵母菌N6076及其原始菌株Kh08为研究对象,基于转录组测序和MVA测定,分析和比较了两者在3个发酵时间点(0、48和96 h)的差异表达基因的功... 详细信息

为了解重组酵母菌N6076不同发酵时间的差异表达基因信息及甲羟戊酸(mevalonate,MVA)代谢状况,以重组酵母菌N6076及其原始菌株Kh08为研究对象,基于转录组测序和MVA测定,分析和比较了两者在3个发酵时间点(0、48和96 h)的差异表达基因的功能。GO功能分析结果表明,重组菌株N6076新增了14项生物学过程、2.细胞组分和2.分子功能,涉及1140个差异表达基因。KEGG代谢分析结果表明,重组菌株N6076新增了13条代谢通路,涉及77个差异表达基因,其中新增的萜类骨架生物合成途径涉及5个差异表达基因。甲羟戊酸激酶(mevalonate kinase,MVK)基因表达与MVA的LC-MS/MS测定结果表明,在整个发酵过程中MVK基因表达量与MVA产量的变化趋势一致。该研究为进一步认识重组酵母菌N6076的基因表达与MVA代谢调控提供了依据。

关键词：重组酵母菌转录组差异表达基因甲羟戊酸代谢

基于Ar分支比方法的光谱强度响应效率标定研究

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光谱学与光谱分析 2018年第5期38卷 1375-1379页

作者：马云云王永强敏琦曹世权张正荣苏茂根孙对兄董晨钟兰州城市学院电子与信息工程学院甘肃兰州730070 甘肃省原子分子物理与功能材料重点实验室西北师范大学物理与电子工程学院甘肃兰州730070

利用Nd∶YAG激光器输出的1 064nm激光在大气压环境中产生了Ar等离子体,测量了Ar等离子体的发射光谱,从Ar等离子体发射光谱中筛选出了来自ArⅠ和ArⅡ15个上能级的35条跃迁谱线,基于分支比方法计算了光谱仪的辐射强度响应效率标定系数。此... 详细信息

利用Nd∶YAG激光器输出的1 064nm激光在大气压环境中产生了Ar等离子体,测量了Ar等离子体的发射光谱,从Ar等离子体发射光谱中筛选出了来自ArⅠ和ArⅡ15个上能级的35条跃迁谱线,基于分支比方法计算了光谱仪的辐射强度响应效率标定系数。此外,利用氘灯和卤钨灯标准光源,对光谱仪辐射强度响应效率进行了标定,得到了针对不同光栅的光谱仪的辐射效率标定系数。用分支比方法获得的辐射强度响应效率标定系数与标准光源得到辐射强度响应效率标定系数具有较好的一致性,其最大相对误差为5.4%。该研究的标定方法可以为一些大型聚变装置的光谱测量的在线标定提供借鉴和参考。

关键词：分支比激光等离子体光谱仪强度响应效率标定

基于转录组测序的异常汉逊酵母菌不同发酵时期差异表达基因功能分析

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食品与发酵工业 2019年第4期45卷 1-6页

作者：唐朝张寒玉王婷冯光文钱卫东蔡长龙毛培宏新疆大学物理科学与技术学院放射生态与离子束生物技术中心新疆乌鲁木齐830046 陕西科技大学食品与生物工程学院陕西西安710032 西安工业大学离子束生物工程与生物多样性研究中心陕西西安710032

异常汉逊酵母(Hansenula anomala)具有较强的发酵力和酯化力,并能积累色氨酸。为了进一步理解其发酵过程中的基因表达与代谢的关系,在转录组测序的基础上,利用生物信息学方法,分别对5个发酵时间点(0、2.、48、72.96 h)的异常汉逊酵母... 详细信息

异常汉逊酵母(Hansenula anomala)具有较强的发酵力和酯化力,并能积累色氨酸。为了进一步理解其发酵过程中的基因表达与代谢的关系,在转录组测序的基础上,利用生物信息学方法,分别对5个发酵时间点(0、2.、48、72.96 h)的异常汉逊酵母菌的差异表达基因的功能进行了分析。结果表明,各发酵时间点与其相邻的上一个时间点相比,发酵2.、48、72.96 h的上调表达的基因数量分别为585、487、154、615,下调表达的基因数量分别为1 112.72.、5、2.5。差异表达基因功能的GO富集和KEGG通路富集结果表明,异常汉逊酵母菌的代谢强度在0～48 h下降,48～96 h上升,并且在96 h时,具有较强的代谢活动和遗传信息处理能力。产色氨酸通路的差异基因表达矩阵分析表明,异常汉逊酵母菌合成色氨酸的速率在0～2. h下降,随后上升;而色氨酸的分解速率从0～48 h上升,随后下降。这些结果可为异常汉逊酵母菌的分子育种及其代谢调控研究提供理论依据。

关键词：异常汉逊酵母转录组差异表达基因

Observation of the Crab Nebula with LHAASO-KM2.−a performance study

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Chinese physics C 2021年第2期45卷 518-530页

作者： F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi H.Cai J.T.Cai Z.Cao J.Chang J.F.Chang X.C.Chang B.M.Chen J.Chen L.Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen X.L.Chen Y.Chen N.Cheng Y.D.Cheng S.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai D.della Volpe B.D'Ettorre Piazzoli X.J.Dong J.H.Fan Y.Z.Fan Z.X.Fan J.Fang K.Fang C.F.Feng L.Feng S.H.Feng Y.L.Feng B.Gao C.D.Gao Q.Gao W.Gao M.M.Ge L.S.Geng G.H.Gong Q.B.Gou M.H.Gu J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He S.L.He X.B.He Y.He M.Heller Y.K.Hor C.Hou X.Hou H.B.Hu S.Hu S.C.Hu X.J.Hu D.H.Huang Q.L.Huang W.H.Huang X.T.Huang Z.C.Huang F.Ji X.L.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.Levochkin B.B.Li C.Li F.Li H.B.Li H.C.Li H.Y.Li J.Li K.Li W.L.Li X.Li X.R.Li Y.Li Y.Z.Li Z.Li E.W.Liang Y.F.Liang S.J.Lin B.Liu C.Liu D.Liu H.Liu H.D.Liu J.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.N.Liu Z.X.Liu W.J.Long R.lu H.K.Lv B.Q.Ma L.L.Ma X.H.Ma J.R.mao A.Masood W.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Sáiz L.Shao O.Shchegolev X.D.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov Q.N.Sun X.N.Sun Z.B.Sun P.H.T.Tam Z.B.Tang W.W.Tian B.D.{2. C.{2. H.{2. H.G.{2. J.C.{2. J.S.{2. L.P.{2. L.Y.{2. R.N.{2. W.{2. X.G.{2. X.J.{2. X.Y.{2. Y.D.{2. Y.J.{2. Y.P.{2. Z.{2. Z.H.{2. Z.X.{2. 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),KM2. 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 KM2. array has been operating stably since the end of *** this paper,we present the KM2. 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 KM2. data of 136 live days between December 2.19 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 10-2.0 TeV fits well with a single power-law function dN/dE=(1.13±0.05stat±0.08sys)×10^(-14).(E/2. TeV)-309±0.06stat±0.02.yscm^(-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

HADAR实验对Fermi-LAT伽马射线源观测的预期研究

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物理学报 2023年第19期72卷 309-323页

作者：孙惠英钱祥利陈天禄单增罗布冯有亮高启苟全补郭义庆胡红波康明铭厉海金刘成刘茂元刘伟乔冰强王旭王振辛广广姚玉华袁强张毅山东管理学院智能工程学院济南250357 西藏大学宇宙线教育部重点实验室拉萨850000 中国科学院高能物理研究所粒子天体中心北京100049 中国科学院大学北京100049 四川大学物理学院成都610064 上海交通大学李政道研究所上海200240 苏州空天信息研究院苏州215000 重庆大学物理学院重庆401331 中国科学院紫金山天文台暗物质与空间天文重点实验室南京210023

高海拔天体辐射探测(high altitude detection of astronomical radiation,HADAR)实验是一个新型的采用纯水作为介质的大气切伦科夫望远镜实验阵列,其采用大口径半球型透镜来收集大气切伦科夫光,以实现对10 GeV—10 TeV能量段的伽马射... 详细信息

高海拔天体辐射探测(high altitude detection of astronomical radiation,HADAR)实验是一个新型的采用纯水作为介质的大气切伦科夫望远镜实验阵列,其采用大口径半球型透镜来收集大气切伦科夫光,以实现对10 GeV—10 TeV能量段的伽马射线和宇宙线的探测.HADAR具有低阈能、高灵敏度和传统成像大气切伦科夫望远镜所不具备的大视场优势,可以对天区进行连续扫描观测,因此将成为全天伽马源的理想观测仪器和爆发源、时变源的理想搜寻探测器.本文基于Fermi-LAT的最新伽马射线源表,详细研究了HADAR实验对这些源的观测能力.对银河系外的源,将这些源的能谱加入河外背景光吸收效应外推至甚高能段.通过对这些源的显著性进行模拟研究,结果显示HADAR运行一年预期有93个伽马射线源以大于5倍的显著性标准偏差被观测到,其中包括45个银河系内的源,39个银河系外的源,3个未知类型的源和6个未关联类型的源.

关键词： HADAR 大气切伦科夫望远镜伽马射线源耀变体

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