检索结果-南通市图书馆

Geometrical reconstruction of fluorescence events observed by the LhAASO experiment

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

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

Cluster星簇对中磁尾尾瓣持续磁重联观测研究

引用

科学通报 2005年第18期50卷 2015-2021页

作者：曹馨濮祖荫张辉傅绥燕肖池阶刘振兴 A.Korth M.Frazen q.G.Zong h.Reme K.h.Glassmeier 北京大学地球与空间科学学院北京100871 中国科学院国家天文台北京100081 中国科学院空间科学与应用研究中心北京100080 max-Planck-Institute for Solar System Research Germany CSP Boston UniversityUS CNSR France IGM TU BraunschweigGermany

当行星际磁场持续南向时, 磁尾尾瓣区积蓄大量的磁能, 出现强的晨昏电场.此时中磁尾磁重联进行得深入持久, 在等离子体片闭合磁场和等离子体被带出重联区之后, 尾瓣区的磁场和等离子体不断进入重联区, 这种重联过程称之为'持续尾瓣重联'... 详细信息

当行星际磁场持续南向时, 磁尾尾瓣区积蓄大量的磁能, 出现强的晨昏电场.此时中磁尾磁重联进行得深入持久, 在等离子体片闭合磁场和等离子体被带出重联区之后, 尾瓣区的磁场和等离子体不断进入重联区, 这种重联过程称之为'持续尾瓣重联'(CLR).分析2001～2003年期间欧空局Cluster星簇对中磁尾的观测数据, 发现CLR除导致磁场形态改变和产生高速流外, 重联区出现空泡, 多数空泡中等离子体密度和温度下降两个数量级(少数为一个数量级).空泡结束后, 密度较重联前低, 温度略有升高.CLR的持续时间一般为几十分钟, 它同行星际磁场持续南向发生的强亚暴有很好的相关性.

关键词：尾瓣重联亚暴空泡高速流 Cluster 磁重联磁尾观测研究对中行星际磁场

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

Reconstruction of Cherenkov image bymultiple telescopes of LhAASO-WFCTA

引用

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

来源：

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

一次磁层亚暴期间磁场偶极化的尾向传播

引用

地球物理学报 2007年第4期50卷 995-1004页

作者：曹馨濮祖荫张辉傅绥燕马志伟肖池阶刘振兴谢伦 Dunlpo M.W. Korth A. Frazen M. Zong q.G. Lueck E. Carr C. Reme h. Glassmeier K.h. 北京大学地球与空间科学学院北京100871 中国科学院等离子体物理研究所合肥230026 中国科学院国家天文台北京100012 中国科学院空间科学与应用研究中心北京100080 Space Science and Technology Department Rutherford Appleton LaboratoryUK max-Planck-Institute for Solar System Research Germany CSP Boston UniversityUS The Blackett Laboratory Imperial College LondonUK CNSR France IGM TUBraunschweigGermany

利用TC1、Cluster和Polar结合极光和同步高度及地磁的观测,研究了2004年9月14日1730～1930UT时间段的亚暴偶极化过程.此前行星际磁场持续南向几个小时.亚暴初发(Onset)开始于1823UT.2min之后,同步高度的LANL-02A在子夜附近观测到了明显... 详细信息

利用TC1、Cluster和Polar结合极光和同步高度及地磁的观测,研究了2004年9月14日1730～1930UT时间段的亚暴偶极化过程.此前行星际磁场持续南向几个小时.亚暴初发(Onset)开始于1823UT.2min之后,同步高度的LANL-02A在子夜附近观测到了明显的能量电子增强(Injection)事件,而TC1在1827UT左右在磁尾(-10,-2,0)RE(GSE)观测到了磁场BX的突然下降,伴随着等离子体压强和温度的突然增加及磁场的强烈扰动.在(-16,1,3)RE(GSE)的Cluster上相同的仪器观测到相同的现象,只是比TC1观测到的晚大约23min,在1850UT左右.虽然Polar在更靠近地球的较高纬度(-7.5,3.5,-4.0)RE(GSE)附近,也在1855UT左右观测到了这种磁场偶极化现象.以上的观测时序表明TC1、Cluster观测到的磁场偶极化比亚暴偶极化初始发生分别晚4min和27min.说明偶极化由近磁尾向中磁尾传播.详细计算表明偶极化源区的位置大约在X=-7.7RE～-8.6RE,而传播速度大约为70km.s-1.在这个事件中亚暴的物理图像可能是中磁尾的近地重联产生的地向高速流到达近磁尾,为近磁尾的亚暴触发创造了条件;亚暴在近磁尾触发之后,磁场偶极化峰面向中磁尾传播.

关键词：偶极化亚暴近地重联持续尾瓣重联 Pi2

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

SMM观测到的白光耀斑

引用

天文学报 1993年第4期34卷 430-435页

作者： Rieger E. 甘为群马普地外物理研究所中国科学院紫金山天文台南京210008

本文收集了SMM运行期间(1980.2—1989.11)与地面观测相对应的太阳白光耀斑hXRBS和GRS观测资料,就白光耀斑与硬X-射线发射及伽玛射线发射之间的关系进行了初步的统计研究.结果表明:白光耀斑与伽玛射线发射之间不存在对应关系;白光耀斑也... 详细信息

本文收集了SMM运行期间(1980.2—1989.11)与地面观测相对应的太阳白光耀斑hXRBS和GRS观测资料,就白光耀斑与硬X-射线发射及伽玛射线发射之间的关系进行了初步的统计研究.结果表明:白光耀斑与伽玛射线发射之间不存在对应关系;白光耀斑也并非全具有强硬X-射线发射.对那些只具有相对较弱的硬X-射线发射的白光耀斑,我们发现低能粒子具有足够的能量驱动连续发射,因而它们可能起源于色球.而对那些具有特别强高能发射的白光耀斑,我们发现注入大气深层的高能粒子可使那里受到部分加热,从而可直接产生部分光球连续谱增强.

关键词：白光耀斑 γ射线事件非热电子

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

Ergonomics Design Research of an Office Desks and Chairs Based on CAD

Ergonomics Design Research of an Office Desks and Chairs Bas...

引用

International Conference on Industrial Technology and Management Science(ITMS 2015)

作者： L.A.Pan q.L.Du Y.q.Wu College of Mechanical and Vehicle Engineering Changchun University Naval Aeronautical Engineering Institute

Office leisure is the common pursuit of the enterprise, government, leadership and staff. The relaxed, happy, free and comfortable life is people always wish, also is inevitable to era development and social progress. So, according to the demand, indoor and outdoor dual-use multi-function folding leisure office furniture has been designed in the paper. First of all, through a large number of research and decisions, the structure of the product portfolio has been determined. In order to be convenient and quick, the characteristics of the furniture on the market have been collected and analyzed, especially the table, chairs and a bed. According to ergonomics, the parameters of the outdoor leisure office desks and chairs have been determined. The rhino software has been used to establish the combination of desk and chair to make the products comply with ergonomics, human psychology and aesthetic principles of the product.

关键词： Office desks and chairs CAD Ergonomics 3D max

来源： cnki会议评论

在线全文

cnki会议

学校读者我要写书评

暂无评论

On Some Inequalities Concerning Rate of Growth of Polynomials

引用

Analysis in Theory and Applications 2014年第3期30卷 290-295页

作者： Abdullah Mir Imtiaz hussain q.M.Dawood Department of Mathematics University of Kashmir

In this paper we consider a class of polynomials P（z）=a0＋∑v^n=tavZv, t≥ 1, not vanishing in ｜z｜〈k, k≥1 and investigate the dependence of max｜z｜=1 ｜P（Rz） -P（rz）] on max｜z｜=1｜P（z）｜, where 1≤ r 〈... 详细信息

关键词： Polynomial zero inequalitiy.

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

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

引用

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

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

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

引用

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

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

New continuum and polarization observations of the Cygnus Loop with FAST *** processing and verification

引用

Research in Astronomy and Astrophysics 2021年第11期21卷 105-118页

作者： Xiao-hui Sun Mei-Niang meng Xu-Yang Gao Wolfgang Reich Peng Jiang Di Li hui-Rong Yan Xiang-hua Li Department of Astronomy Yunnan UniversityKunming 650500China National Astronomical Observatories Chinese Academy of Sciences20A Datun RoadChaoyang DistrictBeijing 100101China CAS Key Laboratory of FAST National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China max-Planck-Institut fur Radioastronomie Auf dem Hugel 6953121 BonnGermany Deutsches Elektronen-Synchrotron DESY Platanenallee 6D-15738 ZeuthenGermany Institut fur Physik und Astronomie Universitat PotsdamHaus 28Karl-Liebknecht-Str.24/25D-14476 PotsdamGermany

We report on the continuum and polarization observations of the Cygnus Loop supernova remnant(SNR)conducted by the Five-hundred-meter Aperture Spherical radio Telescope(FAST).FAST observations provide high angular resolution and high sensitivity images of the SNR,which will help to disentangle its *** obtained Stokes I,q and U maps over the frequency range of 1.03-1.46 Ghz split into channels of 7.63 *** original angular resolution is in the range of~3’-~3.’8,and we combined all the data at a common resolution of 4’.The temperature scale of the total intensity and the spectral index from the in-band temperature-temperature plot are consistent with previous observations,which validates the data calibration and map-making *** rms sensitivity for the band-averaged total-intensity map is about 20 mK in brightness temperature,which is at the level of confusion *** the first time,we apply rotation measure(RM)synthesis to the Cygnus Loop to obtain the polarization intensity and RM *** rms sensitivity for polarization is about 5 mK,far below the total-intensity confusion *** also obtained RMs of eight extragalactic sources,and demonstrate that the wide-band frequency coverage helps to overcome the ambiguity of RM determinations.

关键词： ISM:supernova remnants ISM:magnetic fields polarization techniques:polarimetric

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

欢迎您,

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

请选择保存的检索档案：

请选择收藏分类：

通借通还

欢迎您,

建议与咨询 留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

请选择保存的检索档案： 新增检索档案 确定 取消

请选择收藏分类： 新增自定义分类 确定 取消

通借通还

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

请选择保存的检索档案：

请选择收藏分类：