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Evidence for particle acceleration approaching PeV energies in the W51 complex

Science Bulletin 2024年第18期69卷 2833-2841页

作者： LHAASO Collaboration Zhen Cao F.Aharonian Axikegu Y.X.Bai Y.W.bao D.Bastieri X.J.Bi Y.J.Bi W.Bian A.V.Bukevich Q.Cao W.Y.Cao Zhe Cao J.Chang J.F.Chang A.M.Chen E.S.Chen H.X.Chen Liang Chen Lin Chen Long Chen M.J.Chen M.L.Chen Q.H.Chen S.Chen S.H.Chen S.Z.Chen T.L.Chen Y.Chen N.Cheng Y.D.Cheng M.Y.Cui S.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu X.Q.Dong K.K.Duan J.H.Fan Y.Z.Fan J.Fang J.H.Fang K.Fang C.F.Feng H.Feng L.Feng S.H.Feng X.T.Feng Y.Feng Y.L.Feng S.Gabici B.Gao C.D.Gao Q.Gao W.Gao W.K.Gao M.M.Ge L.S.Geng G.Giacinti G.H.Gong Q.B.Gou M.H.Gu F.L.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han M.Hasan H.H.He H.N.He J.Y.He Y.He Y.K.Hor B.W.Hou C.Hou X.Hou H.B.Hu Q.Hu S.C.Hu D.H.huang T.Q.huang W.J.huang X.T.huang X.Y.huang Y.huang X.L.Ji H.Y.Jia K.Jia K.Jiang X.W.Jiang Z.J.Jiang M.Jin M.M.Kang I.Karpikov D.Kuleshov K.Kurinov B.B.Li C.M.Li Cheng Li Cong Li D.Li F.Li H.B.Li H.C.Li Jian Li Jie Li K.Li S.D.Li W.L.Li W.L.Li X.R.Li Xin Li Y.Z.Li Zhe Li Zhuo Li E.W.Liang Y.F.Liang S.J.Lin B.liu C.liu D.liu D.B.liu H.liu H.D.liu J.liu J.L.liu M.Y.liu R.Y.liu S.M.liu W.liu Y.liu Y.N.liu Q.Luo Y.Luo H.K.Lv B.Q.Ma L.L.Ma X.H.Ma J.R.Mao Z.Min W.Mitthumsiri H.J.Mu Y.C.Nan A.Neronov L.J.Ou P.Pattarakijwanich Z.Y.Pei J.C.Qi M.Y.Qi B.Q.Qiao J.J.Qin A.Raza D.Ruffolo A.Sáiz M.Saeed D.Semikoz L.Shao O.Shchegolev X.D.Sheng F.W.Shu H.C.Song Yu.V.Stenkin V.Stepanov Y.Su D.X.Sun Q.N.Sun X.N.Sun Z.B.Sun J.Takata P.H.T.Tam Q.W.Tang R.Tang Z.B.Tang W.W.Tian C.Wang C.B.Wang G.W.Wang H.G.Wang H.H.Wang J.C.Wang Kai Wang Kai Wang L.P.Wang L.Y.Wang P.H.Wang R.Wang W.Wang X.G.Wang X.Y.Wang Y.Wang Y.D.Wang Y.J.Wang Z.H.Wang Z.X.Wang Zhen Wang Zheng Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu Q.W.Wu S.Wu X.F.Wu Y.S.Wu S.Q.Xi J.Xia G.M.Xiang D.X.Xiao G.Xiao Y.L.Xin Y.Xing D.R.Xiong Z.Xiong D.L.Xu R.F.Xu R.X.Xu W.L.Xu L.Xue D.H.Yan J.Z.Yan T.Yan C.W.Yang C.Y.Yang F.Yang F.F.Yang L.L.Yang M.J.Yang R.Z.Yang W.X.Yang Y.H.yao Z.G.yao L.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.Yue H.D.Zeng T.X.Zeng W.Zeng M.Zha B.B.Zhang F.Zhang H.Zhang 不详 Key Laboratory of Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of chinese academy of sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 103980Heidelberg 69029Germany School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Institute for Nuclear Research of Russian academy of sciences Moscow 117312Russia Hebei Normal University Shijiazhuang 050024China University of Science and Technology of China Hefei 230026China State Key Laboratory of Particle Detection and Electronics China Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Research Center for astronomical Computing Zhejiang LaboratoryHangzhou 311121China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China School of Physics and Astronomy Yunnan UniversityKunming 650091China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China national astronomical {2. Chinese Academy of SciencesBeijing 100101China School of Physics and Astronomy(Zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(Zhuhai) Sun Yat-sen UniversityZhuhai 519000&Guangzhou 510275GuangdongChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China APC UniversitéParis Cité

Theγ-ray emission from the W51 complex is widely acknowledged to be attributed to the interaction between the cosmic rays(CRs)accelerated by the shock of supernova remnant(SNR)W51C and the dense molecular clouds in the adjacent star-forming region,***,the maximum acceleration capability of W51C for CRs remains *** on observations conducted with the Large High Altitude Air Shower Observatory(LHAASO),we report a significant detection ofγrays emanating from the W51 complex,with energies from 2.to 2.0 *** LHAASO measurements,for the first time,extend theγ-ray emission from the W51 complex beyond 100 TeV and reveal a significant spectrum bending at tens of *** combining the"π^(0)-decay bump"featured data from Fermi-LAT,the broadbandγ-ray spectrum of the W51 region can be well-characterized by a simple pp-collision *** observed spectral bending feature suggests an exponential cutoff at~400 TeV or a power-law break at~2.0 TeV in the CR proton spectrum,most likely providing the first evidence of SNRs serving as CR accelerators approaching the PeV ***,two young star clusters within W51B could also be theoretically viable to produce the most energeticγrays observed by *** findings strongly support the presence of extreme CR accelerators within the W51 complex and provide new insights into the origin of Galactic CRs.

关键词： UHE c-ray Cosmic rays SNR W51C Star clusters

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Prospective study on observations of γ-ray sources in the Galaxy using the HADAR experiment

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Frontiers of physics 2022年第6期17卷 1-14页

作者： Xiangli Qian Huiying Sun Tianlu Chen Danzengluobu Youliang Feng Qi Gao Quanbu Gou Yiqing Guo Hongbo Hu Mingming Kang Haijin Li Cheng liu Maoyuan liu Wei liu Bingqiang Qiao Xu Wang Zhen Wang Guangguang Xin Yuhua yao Qiang Yuan Yi Zhang School of Intelligent Engineering Shandong Management UniversityJinan 250357China The Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of chinese academy of sciences 19 A Yuquan RoadShijingshan DistrictBeijing 100049China College of Physics Sichuan UniversityChengdu 610064China Tsung-Dao Lee Institute Shanghai Jiao Tong UniversityShanghai 200240China School of Physics and Technology Wuhan UniversityWuhan 430072China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210008China

The High Altitude Detection of astronomical Radiation(HADAR)experiment is a refracting terrestrial telescope array based on the atmospheric Cherenkov imaging *** focuses the Cherenkov light emitted by extensive air showers through a large aperture water-lens system for observing very-high-energyγ-rays and cosmic *** the advantages of a large field-of-view(FOV)and low energy threshold,the HADAR experiment operates in a large-scale sky scanning mode to observe galactic *** study presents the prospects of using the HADAR experiment for the sky survey of TeVγ-ray sources from TeVCat and provids a one-year survey of statistical *** from the simulation show that a total of 2. galactic point sources,including five supernova remnant sources and superbubbles,four pulsar wind nebula sources,and 14 unidentified sources,were detected in the HADAR FOV with a significance greater than 5 standard deviations(σ).The statistical significance for the Crab Nebula during one year of operation reached 346.0σand the one-year integral sensitivity of HADAR above 1 TeV was~1.3%–2.4%of the flux from the Crab Nebula.

关键词： HADAR Galactic sources significance gamma rays

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Pilot HI survey of Planck Galactic Cold Clumps with FAST

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Research in Astronomy and Astrophysics 2020年第5期20卷 181-192页

作者： Ning-Yu Tang Pei Zuo Di Li Lei Qian Tie liu Yue-Fang Wu Marko Krco Meng-Ting liu You-Ling Yue Yan Zhu Hong-Fei liu Dong-Jun Yu Jing-Hai Sun Peng Jiang Gao-Feng Pan Hui Li Heng-Qian Gan Rui yao Shu liu FAST Collaboration national astronomical {2. Chinese Academy of SciencesBeijing 100101China CAS Key Laboratory of FAST National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China shanghai astronomical Observatory Chinese Academy of SciencesShanghai 200030ChinaShanghai 200030China East Asian Observatory HI 96720USA Department of Astronomy School of PhysicsPeking UniversityBeijing 100871China

We present a pilot HI survey of 17 Planck Galactic Cold Clumps(PGCCs)with the Five-hundred-meter Aperture Spherical radio Telescope(FAST).HI Narrow Self-Absorption(HINSA)is an effective method to detect cold HI being mixed with molecular hydrogen H2.and improves our understanding of the atomic to molecular transition in the interstellar *** was found in 58%PGCCs that we *** column density of HINSA was found to have an intermediate correlation with that of 13CO,following log(N(HINSA))=(0.52.0.2.)log(N13CO)+(10±4.1).HI abundance relative to total hydrogen[HI]/[H]has an average value of 4.4×10-3,which is about 2.8 times of the average value of previous HINSA surveys toward molecular *** clouds with total column density NH>5×102. cm-2.an inverse correlation between HINSA abundance and total hydrogen column density is found,confirming the depletion of cold HI gas during molecular gas formation in more massive *** line width of 13CO is about 0-0.5 kms-1 larger than that of *** possible explanation of narrower non-thermal width of HINSA is that HINSA region is smaller than that of *** on an analytic model of H2.formation and H2.dissociation by cosmic ray,we found the cloud ages to be within 106.7-107.0 yr for five sources.

关键词： ISM:clouds ISM:evolution ISM:molecules

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太阳抵近探测计划——观测位置的新突破

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上海航天（中英文） 2024年第5期41卷 1-10页

作者：林隽陆希陈雨豪黄帆张珅毅张艺腾周斌葛振华刘鎏田晖何建森程鑫陈鹏飞白先勇季海生刘佳佳张晓世中国科学院云南天文台云南昆明650216 中国科学院天文大科学研究中心北京100012 中国科学院大学天文与空间科学学院北京100049 云南省太阳物理与空间目标监测重点实验室云南昆明650216 上海卫星工程研究所上海201109 中国科学院国家空间科学中心北京100190 昆明理工大学材料科学与工程学院云南昆明650031 中国科学院微小卫星创新研究院上海201203 北京大学地球与空间科学学院北京100871 南京大学天文与空间科学学院江苏南京210093 中国科学院国家天文台北京100101 中国科学院紫金山天文台江苏南京210023 中国科技大学地球与空间科学学院安徽合肥230026 云南大学物理天文学院云南昆明650500

太阳抵近探测计划(SCOPE)旨在突破高温和强辐射防护、长距离运载、远距离轨道控制和先进载荷等一系列极限技术,将探测器投送至距太阳中心仅有5个太阳半径的位置上,深入太阳大气层进行探测,研究太阳附近极亮、极热的深空探测“无人区”,... 详细信息

太阳抵近探测计划(SCOPE)旨在突破高温和强辐射防护、长距离运载、远距离轨道控制和先进载荷等一系列极限技术,将探测器投送至距太阳中心仅有5个太阳半径的位置上,深入太阳大气层进行探测,研究太阳附近极亮、极热的深空探测“无人区”,在全新的位置上对太阳进行超近距离原位探测和遥感观测,针对磁场和等离子体结构实现空间分辨率优于0.1"的观测。探测器将穿越太阳爆发磁重联电流片,显微观测太阳爆发磁结构,原位探测磁重联电流片、日冕物质抛射与激波以及各类带电粒子,以推动揭示太阳爆发理论机理。探测器将在最靠近太阳的区域显微监测和探测日冕中尺度小于0.1"的纳耀斑、光球中尺度小于0.06"的磁场和速度场结构及其演化特征,确认日冕加热机制;探测太阳风重离子电荷态,确认太阳起源及加速机制。探测器还将在最接近太阳的区域内与原位探测日冕磁场,显微观测太阳极区磁场和等离子体结构和演化特征;揭示太阳附近尘埃分布特征,进入无尘埃区,确定太阳系尘埃盘内边界。困扰太阳物理界近百年的两个科学难题,即太阳爆发机理难题和日冕加热与太阳风加速机理难题,随着该计划的顺利实施将被破解;在最接近日心的位置处实现日冕磁场,包括太阳极区磁场原位探测“0到1”的突破也将实现。本文将介绍SCOPE的背景、科学目标和预期产出、有效载荷以及卫星平台关键技术。

关键词：太阳爆发磁场磁重联中高能粒子原位探测热防护深空通信

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Multiwavelength study of nearly face-on low surface brightness disk galaxies

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Research in Astronomy and Astrophysics 2010年第12期10卷 1223-1241页

作者： Dong Gao Yan-Chun Liang Shun-Fang liu Guo-Hu Zhong Xiao-Yan Chen Yan-Bin Yang Francois Hammer Guo-Chao Yang Li-Cai Deng Jing-yao Hu national astronomical {2. Chinese Academy of Sciences Beijing 100012 China ycliang @ nao. cas. cn dgao @ nao. cas. cn Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China Graduate University of chinese academy of sciences Beijing 100049 China GEPI Observatoire de Paris-Meudon 92195 Meudon France Department of Physics Hebei Normal University Shijiazhuang 050016 China

We study the ages of a large sample （1802. of nearly face-on disk low surface brightness galaxies （LSBGs） using the evolutionary population synthesis （EPS） model PEGASE with an exponentially decreasing star formation rate to fit their mul- tiwavelength spectral energy distributions （SEDs） from far-ultraviolet （FUV） to nearinfrared （NIR）. The derived ages of LSBGs are 1-5 Gyr for most of the sample no matter if constant or varying dust extinction is adopted, which are similar to most of the previous studies on smaller samples. This means that these LSBGs formed the majority of their stars quite recently. However, a small part of the sample （~2.-3%） has larger ages of 5-8 Gyr, meaning their major star forming process may have occurred earlier. At the same time, a large sample （5886） of high surface brightness galaxies （HSBGs） are selected and studied using the same method for comparisons. The de- rived ages are 1-5 Gyr for most of the sample （97%） as well. These results probably mean that these LSBGs have not much different star formation histories from their HSBGs counterparts. However, we should notice that the HSBGs are generally about 0.2.Gyr younger, which could mean that the HSBGs may have undergone more recent star forming activities than the LSBGs.

关键词： galaxies: evolution -- galaxies: formation -- galaxies: photometry --galaxies: spiral -- galaxies: statistics -- ultraviolet: galaxies

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Observation of spectral lines in the exceptional GRB 2.1009A

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Science China(Physics,Mechanics & Astronomy) 2024年第8期67卷 187-206页

作者： Yan-Qiu Zhang Shao-Lin Xiong Ji-Rong Mao Shuang-Nan Zhang Wang-Chen Xue Chao Zheng Jia-Cong liu Zhen Zhang Xi-Lu Wang Ming-Yu Ge Shu-Xu Yi Li-Ming Song Zheng-Hua An Ce Cai Xin-Qiao Li Wen-Xi Peng Wen-Jun Tan Chen-Wei Wang Xiang-Yang Wen Yue Wang Shuo Xiao Fan Zhang Peng Zhang Shi-Jie Zheng Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of chinese academy of sciences Beijing 100049China Yunnan observatories Chinese Academy of SciencesKunming 650011China Center for astronomical Mega-Science Chinese Academy of SciencesBeijing 100012China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650216China College of Physics and Hebei Key Laboratory of Photophysics Research and Application Hebei Normal UniversityShijiazhuang 050024China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal UniversityGuiyang 550001China College of Electronic and Information Engineering Tongji UniversityShanghai 201804China

As the brightest gamma-ray burst ever observed,GRB 2.1009A provided a precious opportunity to explore spectral line *** this article,we performed a comprehensive spectroscopy analysis of GRB 2.1009A jointly with GECAM-C and Fermi/GBM data to search for emission and absorption *** the first time we investigated the line feature throughout this GRB including the most bright part where many instruments suffered problems,and identified prominent emission lines in multiple time *** central energy of the Gaussian emission line evolves from about 37 to 6 MeV,with a nearly constant ratio(about 10%)between the line width and central ***,we find that both the central energy and the energy flux of the emission line evolve with time as a power law decay with power law index of–1 and–2.*** suggest that the observed emission lines most likely origin from the blue-shifted electron positron pair annihilation 511 ke V *** find that a standard high latitude emission scenario cannot fully interpret the observation,thus we propose that the emission line comes from some dense clumps with electron positron pairs traveling together with the *** this scenario,we can use the emission line to directly,for the first time,measure the bulk Lorentz factor of the jet(Γ)and reveal its time evolution(i.e.,Γ~t^(-1))during the prompt ***,we find that the flux of the annihilation line in the co-moving frame keeps *** discoveries of the spectral line features shed new and important lights on the physics of GRB and relativistic jet.

关键词： GRB GRB 2.1009A emission line

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搜寻第二个地球——系外地球(ET)巡天计划

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空间科学学报 2024年第3期44卷 400-424页

作者：葛健陈雯陈永和宋宗玺王坚张辉李岩臧伟呈周丹张永帅陈琨阳应权毛淑德黄煦药新雨李兴隆姜海娇于涌唐正宏董峰高伟张鸿飞申超王峰涛魏传新杨宝玉李豫东文林张朋军张聪聪谢基伟马波邓洪平刘慧根段旭亮王昊宇黄江江高扬王伊菲王磊秦根健刘欣宇高婕中国科学院上海天文台上海200030 中国科学院微小卫星创新研究院上海201304 中国科学院上海技术物理研究所上海200083 中国科学院西安光学精密机械研究所西安710119 中国科学技术大学合肥230026 清华大学天文系北京100190 南昆士兰大学天体物理中心图文巴QLD4350 中国航天科技集团公司第八研究院803研究所上海201109 中国科学院新疆理化技术研究所乌鲁木齐830011 南京大学天文系南京210023 中山大学物理与天文学院珠海519082

系外地球科学卫星(ET)将通过采用空间大视场超高精度测光这一关键技术在国际上率先突破生命起源中的系外地球存在及其演化这一重大前沿科学问题. ET卫星将在日地拉格朗日L2.晕(Halo)轨道部署由6台广角凌星望远镜和1台微引力透镜望远镜... 详细信息

系外地球科学卫星(ET)将通过采用空间大视场超高精度测光这一关键技术在国际上率先突破生命起源中的系外地球存在及其演化这一重大前沿科学问题. ET卫星将在日地拉格朗日L2.晕(Halo)轨道部署由6台广角凌星望远镜和1台微引力透镜望远镜构成的空间天文台,结合凌星法和微引力透镜法,利用空间超大视场和超高精度的光学测光观测,首次发现富有重要意义、被广泛关注的系外地球,并确定其发生率,对目前了解甚少的类地行星和流浪行星进行国际上第一次大规模的种群普查,首次发现流浪地球,并确定其发生率,揭示类地行星和流浪行星起源,为地外生命探寻提供候选者和新方向. ET卫星的观测结果、统计研究以及和对理论的检验将回答系外地球在宇宙中有多普遍,类地行星是如何形成和演化的,流浪行星又是如何起源的这些亟待解决的前沿科学问题.对ET卫星发现的系外地球样本的后随观测,将精确测量其质量、密度和大气成分,有助于深入分析宜居性特征.此外,对ET新发现的大量各种系外行星样本的研究,以及对理论的检验将推动这些种类的行星形成和演化规律的更深入认识, ET的大量高精度、高频次和长基线测光数据将推动星震学、银河系考古学、时域天文学、双星和双星黑洞等领域的研究.

关键词：系外行星类地行星宜居带凌星微引力透镜测光

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The site conditions of the Guo Shou Jing Telescope

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Research in Astronomy and Astrophysics 2012年第7期12卷 772-780页

作者： Song yao Chao liu Hao-Tong Zhang Li-Cai Deng Heidi Jo Newberg Yue-Yang Zhang Jing Li Nian liu Xu Zhou Jeffrey L. Carlin Li Chen Norbert Christlieb Shuang Gao Zhan-Wen Han Jin-Liang Hou Hsu-Tai Lee Xiao-Wei liu Kai-Ke Pan Hong-Chi Wang Yan Xu Fan Yang Key Lab of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China Graduate University of chinese academy of sciences Beijing 100049 China Department of Physics Applied Physics and Astronomy Rensselaer Polytechnic Institute 1108th Street Troy NY 12180 USA : School of Physics and Electronic Information China West Normal University Nanchong 637000 China shanghai astronomical Observatory Chinese Academy of Sciences Shanghai 200030 China Center for Astronomy University of Heidelberg Landesstemwarte K6nigstuhl 12 D-69117Heidelberg Germany Yunnan astronomical Observatory Chinese Academy of Sciences Kunming 650011 China Institute of Astronomy and Astrophysics Academia Sinica P.O. Box 23-141 Taipei i06 China Department of Astronomy & Kavli Institute of Astronomy and Astrophysics Peking UniversityBeijing 100871 China Apache Point Observatory PO Box 59 Sunspot NM 88349 USA Purple Mountain Observatory Chinese Academy of Sciences Nanjing 210008 China

The weather at the Xinglong Observing Station, where the Guo Shou Jing Telescope （GSJT） is located, is strongly affected by the monsoon climate in north- east China. The LAMOST survey strategy is constrained by these weather patterns. We present statistics on observing hours from 2.04 to 2.07, and the sky brightness, seeing, and sky transparency from 1995 to 2.11 at the site. We investigate effects of the site conditions on the survey plan. Operable hours each month show a strong cor- relation with season： on average there are eight operable hours per night available in December, but only one-two hours in July and August. The seeing and the sky trans- parency also vary with season. Although the seeing is worse in windy winters, and the atmospheric extinction is worse in the spring and summer, the site is adequate for the proposed scientific program of the LAMOST survey. With a Monte Carlo simulation using historical data on the site condition, we find that the available observation hours constrain the survey footprint from 2.h to 16h in right ascension; the sky brightness allows LAMOST to obtain a limiting magnitude of V = 19.5 mag with S/N= 10.

关键词： telescopes - site testing - surveys

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Site testing campaign for the Large Optical/infrared Telescope of China:overview

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Research in Astronomy and Astrophysics 2020年第6期20卷 81-95页

作者： Lu Feng Jin-Xin Hao Zi-huang Cao Jin-Min Bai Ji Yang Xu Zhou Yong-Qiang yao Jin-Liang Hou Yong-Heng Zhao Yu {2. Teng-Fei Song Li-Yong {2. Jia Yin Hua-Lin Chen Chong Pei Ali Esamdin Lu Ma Chun-Hai Bai Peng Wei Jing Xu Guang-Xin Pu Guo-Jie Feng Xuan Zhang Liang Ming Abudusaimaitijiang Yisikandee Jian-Rong Shi Jian Li Yuan Tian Zheng Wang Xia Wang Xiao-Jun Jiang Jian-Feng Wang Jian-Feng Tian Yan-Jie Xue Jian-Sheng Chen Jing-yao Hu Zhi-Xia Shen Yun-Ying Jiang national astronomical {2. Chinese Academy of SciencesBeijing 100101China Yunnan observatories Chinese Academy of SciencesKunming 650216China Xinjiang astronomical Observatory Chinese Academy of SciencesUrumqi 830011China shanghai astronomical Observatory Chinese Academy of SciencesShanghai 200030China Nanjing Institute of astronomical Optics&Technology Chinese Academy of SciencesNanjing 210042China Purple Mountain Observatory Chinese Academy of SciencesNanjing 210033China University of chinese academy of sciences Beijing 100049China

The Large Optical/infrared Telescope(LOT)is a ground-based 12.m diameter optical/infrared telescope which is proposed to be built in the western part of China in the next *** on satellite remote sensing data,along with geographical,logistical and political considerations,three candidate sites were chosen for ground-based astronomical performance *** sites include:Ali in Tibet,Daocheng in Sichuan and Muztagh-ata in *** until now,all three sites have continuously collected data for two *** this paper,we will introduce this site testing campaign,and present its monitoring results obtained during the period between March 2.17 and March 2.19.

关键词： techniques telescope-site testing

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Detecting neutrinos from supernova bursts in PandaX-4T

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chinese Physics C 2024年第7期48卷 14-21页

作者：庞彬宇阿布都沙拉木·阿布都克力木薄子豪陈葳谌勋程晨成兆侃崔祥仪樊英杰方德清符长波付孟婷耿立升 Karl Giboni 顾琳慧郭绪元韩晨成韩柯何昶达何金荣黄迪黄彦霖黄俊挺黄周侯汝全侯钰季向东巨永林李晨翔李家富李名川李帅杰李涛林箐刘江来陆聪聪芦晓盈罗棱尹罗云阳马文博马余刚冒亚军孟月宁旭阳祁宁春钱志成任祥祥 Nasir Shaheed 尚晓凤邵熙元申国防司琳孙文良谈安迪陶奕王安庆王萌王秋红王少博王思广王为王秀丽王舟魏月环武蒙蒙邬维浩夏经铠肖梦姣肖翔谢鹏伟燕斌斌颜玺雨杨继军杨勇姚玉坤喻纯旭袁影苑哲鑫宁张丹张敏桢张鹏张世博张澍张涛张洋张瀛心张园园赵力郑其斌周济芳周宁周小朋周永周钰博 New Cornerstone Science Laboratory Tsung-Dao Lee InstituteShanghai Jiao Tong UniversityShanghai200240China Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary ScienceShandong UniversityQingdao 266237ShandongChina Key Laboratory of Particle Physics and Particle Irradiation of Ministry of Education Shandong UniversityQingdao 266237ShandongChina School of Physics and Astronomy Shanghai Jiao Tong UniversityKey Laboratory for Particle Astrophysics and Cosmology(MoE)Shanghai Key Laboratory for Particle Physics and CosmologyShanghai 200240China shanghai Jiao Tong University Sichuan Research Institute Chengdu 610213China School of Physics Sun Yat-Sen UniversityGuangzhou 510275China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen UniversityZhuhai519082China Department of Physics Yantai UniversityYantai 264005China Key Laboratory of Nuclear Physics and Ion-beam Application(MOE) Institute of Modern PhysicsFudan UniversityShanghai 200433China School of Physics Peking UniversityBeijing 100871China School of Physics Beihang UniversityBeijing 102206China International Research Center for Nuclei and Particles in the Cosmos&beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang UniversityBeijing 100191China School of Physics and Microelectronics Zhengzhou UniversityZhengzhouHenan 450001China Yalong River Hydropower Development Company Ltd.288 Shuanglin RoadChengdu 610051China School of Medical Instrument and Food Engineering University of Shanghai for Science and TechnologyShanghai 200093China School of Mechanical Engineering Shanghai Jiao Tong UniversityShanghai 200240China Department of Physics University of MarylandCollege ParkMaryland 20742USA State Key Laboratory of Particle Detection and Electronics University of Science and Technology of ChinaHefei 230026China Department of Modern Physics University of Science and Technology of ChinaHefei 230026China School of Physics Nankai UniversityTian

Neutrinos from core-collapse supernovae are essential for understanding neutrino physics and stellar ***-phase xenon dark matter detectors can be used to track explosions of galactic supernovae by detecting neutrinos through coherent elastic neutrino-nucleus *** this study,a variation of progenitor masses and explosion models are assumed to predict neutrino fluxes and spectra,which result in the number of expected neutrino events ranging from 6.6 to 13.7 at a distance of 10 kpc over a 10-s duration with negligible backgrounds at *** specialized triggering alarms for monitoring supernova burst neutrinos are *** efficiency of detecting supernova explosions at various distances in the Milky Way is *** alarms will be implemented in the real-time supernova monitoring system at PandaX-4T in the near future,which will provide supernova early warnings for the astronomical community.

关键词： core-collapse supernovae neutrinos liquid xenon detectors supernova early warnings

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