检索结果-南通市图书馆

A new lunar absolute control point: established by images from the landing camera on chang'e-3

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Research in Astronomy and Astrophysics 2014年第12期14卷 1543-1556页

作者： Fen-Fei wang Jian-Jun liu Chun-Lai li Xin Ren ling-li Mu wei yan Wen-Rui wang jing-Tao xiao Xu Tan xiao-Xia Zhang xiao-Duan Zou xing-Ye Gao Key Laboratory of Lunar and Deep Space Exploration National Astronomical ObservatoriesChinese Academy of Sciences

The establishment of a lunar control network is one of the core tasks in selenodesy, in which defining an absolute control point on the Moon is the most im- portant step. However, up to now, the number of absolute control points has been very sparse. These absolute control points have mainly been lunar laser ranging retrore- flectors, whose geographical location can be observed by observations on Earth and also identified in high resolution lunar satellite images. The chang＇e-3 （CE-3） probe successfully landed on the Moon, and its geographical location has been monitored by an observing station on Earth. Since its positional accuracy is expected to reach the meter level, the CE-3 landing site can become a new high precision absolute control point. We use a sequence of images taken from the landing camera, as well as satellite images taken by CE-1 and CE-2, to identify the location of the CE-3 lander. With its geographical location known, the CE-3 landing site can be established as a new abso- lute control point, which will effectively expand the current area of the lunar absolute control network by 22%, and can greatly facilitate future research in the field of lunar surveying and mapping, as well as selenodesy.

关键词： Moon -- methods: data analysis -- techniques: image processing

结构新颖的金属双核烯丙基试剂的合成及其芳香醛烯丙基化反应

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高等学校化学学报 2008年第4期29卷 767-771页

作者：魏晓宁柳凌艳于磊常卫星李靖南开大学元素有机化学国家重点实验室天津300071

报道了一个简捷的芳香醛的烯丙基化反应的新体系．通过使用新型的金属双核烯丙基锡试剂（含有Sn—M键，M=Mn或Fe）与醛在二氯甲烷中反应，无需使用任何辅助试剂，直接得到较高产率（42％～98％）的高烯丙基醇．实验结果证明过渡金属基团... 详细信息

报道了一个简捷的芳香醛的烯丙基化反应的新体系．通过使用新型的金属双核烯丙基锡试剂（含有Sn—M键，M=Mn或Fe）与醛在二氯甲烷中反应，无需使用任何辅助试剂，直接得到较高产率（42％～98％）的高烯丙基醇．实验结果证明过渡金属基团及M—Sn键具有相当高的活化锡原子上的烯丙基基团的作用．

关键词：金属双核烯丙基试剂烯丙基化醛

Stepped-up development of accelerator mass spectrometry method for the detection of ^(60)Fe with the HI-13 tandem accelerator

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Nuclear Science and Techniques 2024年第4期35卷 136-143页

作者： yang Zhang Sheng-Quan yan Ming He Qing-Zhang Zhao Wen-Hui Zhang Chao-Xin Kan Jian-Ming Zhou Kang-ning li xiao-Fei wang Jian-Cheng liu Zhao-Hua Peng Zhuo liang Ai-ling li Jian Zheng Qi-Wen Fan Yun-Ju li You-Bao wang Zhi-Hong li yang-Ping Shen Ding Nan wei Nan Yu-Qiang Zhang Jia-Ying-Hao li Jun-Wen Tian Jiang-lin Hou chang-Xin Guo Zhi-Cheng Zhang Ming-Hao Zhu Yu-Wen Chen Yu-Chen Jiang Tao Tian Jin-Long Ma Yi-Hui liu jing-Yu Dong Run-Long liu Mei-Yue-Nan Ma Yong-Shou Chen wei-Ping liu bing Guo China Institute of Atomic Energy P.O.Box 275(10)Beijing 102413China College of Science Southern University of Science and TechnologyShenzhen 518055China School of Physics Xi’an Jiaotong UniversityXi’an 710049China

The Moon provides a unique environment for investigating nearby astrophysical events such as *** samples retain valuable information from these events,via detectable long-lived“fingerprint”radionuclides such as^(60)*** this work,we stepped up the development of an accelerator mass spectrometry(AMS)method for detecting^(60)Fe using the HI-13tandem accelerator at the China Institute of Atomic Energy(CIAE).Since interferences could not be sufficiently removed solely with the existing magnetic systems of the tandem accelerator and the following Q3D magnetic spectrograph,a Wien filter with a maximum voltage of±60 kV and a maximum magnetic field of 0.3 T was installed after the accelerator magnetic systems to lower the detection background for the low abundance nuclide^(60)Fe.A 1μm thick Si_(3)N_(4) foil was installed in front of the Q3D as an energy *** particle detection,a multi-anode gas ionization chamber was mounted at the center of the focal plane of the ***,an^(60)Fe sample with an abundance of 1.125×10^(-10)was used to test the new AMS *** results indicate that^(60)Fe can be clearly distinguished from the isobar^(60)*** sensitivity was assessed to be better than 4.3×10^(-14)based on blank sample measurements lasting 5.8 h,and the sensitivity could,in principle,be expected to be approximately 2.5×10^(-15)when the data were accumulated for 100 h,which is feasible for future lunar sample measurements because the main contaminants were sufficiently separated.

关键词： Accelerator mass spectrometry Wien filter Isobar separation Supernovae chang'e-5 lunar samples

Measurement of the neutron total cross section of carbon at the Back-n white neutron beam of CSNS

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Nuclear Science and Techniques 2019年第9期30卷 73-82页

作者： xing-yan liu Yi-wei yang Rong liu Jie Wen Zhong-wei Wen Zi-Jie Han Zhi-Zhou Ren Qi An Huai-Yong Bai Jie Bao Ping Cao Qi-Ping Chen Yong-Hao Chen Pin-jing Cheng Zeng-Qi Cui Rui-Rui Fan chang-Qing Feng Min-Hao Gu Feng-Qin Guo chang-Cai Han Guo-Zhu He Yong-Cheng He Yue-Feng He Han-Xiong Huang wei-ling Huang Xi-Ru Huang xiao-Lu Ji Xu-yang Ji Hao-Yu Jiang wei Jiang Han-Tao jing ling Kang Ming-Tao Kang Bo li Lun li Qiang li xiao li yang li yang li Shu-Bin liu Guang-Yuan Luan Ying-lin Ma chang-Jun ning Bin-Bin Qi Jie Ren Xi-Chao Ruan Zhao-Hui Song Hong Sun xiao-yang Sun Zhi-Jia Sun Zhi-Xin Tan Hong-Qing Tang jing-Yu Tang Peng-Cheng wang Qi wang Tao-Feng wang yan-Feng wang Zhao-Hui wang Zheng wang Qing-Biao Wu xiao-Guang Wu Xuan Wu li-Kun Xie Han Yi li Yu Tao Yu Yong-Ji Yu Guo-Hui Zhang jing Zhang lin-Hao Zhang li-Ying Zhang Qing-Min Zhang Qi-wei Zhang Xian-Peng Zhang Yu-liang Zhang Zhi-Yong Zhang Ying-Tan Zhao liang Zhou Zu-Ying Zhou Dan-yang Zhu Ke-Jun Zhu Peng Zhu Institute of Nuclear Physics and Chemistry China Academy of Engineering Physics State Key Laboratory of Particle Detection and Electronics Chinese Academy of Sciences(CAS) Department of Modern Physics University of Science and Technology of China State Key Laboratory of Nuclear Physics and Technology School of PhysicsPeking University Key Laboratory of Nuclear Data China Institute of Atomic Energy Institute of High Energy Physics Chinese Academy of Sciences(CAS) Spallation Neutron Source Science Center University of South China Northwest Institute of Nuclear Technology Department of Engineering and Applied Physics University of Science and Technology of China Beihang University Xi’an Jiaotong University

To verify the performance of the neutron total cross-sectional spectrometer, the neutron total cross section of carbon is initially measured in the energy range of 1 eV to 20 MeV using the time-of-flight method. The measurement is performed at the Back-n white neutron source with a 76-m time-of-flight path using the China Spallation Neutron Source. A multilayer fast fission chamber with 235U and 238U is employed as the neutron detector. The diameter and thickness of the natural graphite sample are 70 mm and 40 mm, respectively. Signal waveforms are collected using a data acquisition system. Off-line data processing was used to obtain the neutron time-of-flight spectra and transmissions. The uncertainty of the counting statistics is generally approximately 3% for each bin in the energy range of 1–20 MeV. It is determined that the results for the neutron total cross section of carbon obtained using ^235U cells are in good agreement with the results obtained using 238U cells within limits of statistical uncertainty. Moreover, the measured total cross sections show good agreement with the broadening evaluated data.

关键词： CSNS Back-n white neutron source NTOX Neutron total cross section Carbon Multilayer fast fission chamber

Measurement of the ^(232)Th(n,f)cross section in the 1-200 MeV range at the CSNS Back-n

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Nuclear Science and Techniques 2023年第8期34卷 142-153页

作者： Zhi-Zhou Ren Yi-wei yang Yong-Hao Chen Rong liu Bang-Jiao Ye Jie Wen Hai-Rui Guo Zi-Jie Han Qi-Ping Chen Zhong-wei Wen wei-li Sun Han Yi xing-yan liu Tao Ye Jiang-Bo Bai Qi An Jie Bao Yu Bao Ping Cao Hao-Lei Chen Zhen Chen Zeng-Qi Cui Rui-Rui Fan chang-Qing Feng Ke-Qing Gao xiao-Long Gao Min-Hao Gu chang-Cai Han Guo-Zhu He Yong-Cheng He yang Hong Yi-wei Hu Han-Xiong Huang Xi-Ru Huang Hao-Yu Jiang wei Jiang Zhi-Jie Jiang Han-Tao jing ling Kang Bo li Chao li Jia-Wen li Qiang li xiao li yang li Jie liu Shu-Bin liu Ze Long Guang-Yuan Luan chang-Jun ning Meng-Chen Niu Bin-Bin Qi Jie Ren Xi-Chao Ruan Zhao-Hui Song Kang Sun Zhi-Jia Sun Zhi-Xin Tan jing-Yu Tang Xin-Yi Tang Bin-Bin Tian li-Jiao wang Peng-Cheng wang Zhao-Hui wang xiao-Guang Wu Xuan Wu li-Kun Xie xiao-Yun yang li Yu Tao Yu Yong-Ji Yu Guo-Hui Zhang lin-Hao Zhang Qi-wei Zhang Xian-Peng Zhang Yu-liang Zhang Zhi-Yong Zhang Lu-Ping Zhou Zhi-Hao Zhou Ke-Jun Zhu Department of Modern Physics University of Science and Technology of ChinaHefei 230026China Institute of Nuclear Physics and Chemistry China Academy of Engineering PhysicsMianyang 621900China Institute of High Energy Physics Chinese Academy of Sciences(CAS)Beijing 100049China Spallation Neutron Source Science Center Dongguan 523803China Institute of Applied Physics and Computational Mathematics Beijing 100088China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of ChinaHefei 230027China Key Laboratory of Nuclear Data China Institute of Atomic EnergyBeijing 102413China School of Nuclear Science and Technology University of Science and Technology of ChinaHefei 230027China State Key Laboratory of Nuclear Physics and Technology School of PhysicsPeking UniversityBeijing 100871China State Key Laboratory of Particle Detection and Electronics Institute of High Energy PhysicsChinese Academy of SciencesBeijingChina Northwest Institute of Nuclear Technology Xi’an 710024China University of Chinese Academy of Sciences Beijing 100049China Department of Engineering and Applied Physics University of Science and Technology of ChinaHefei 230026China

The ^(232)Th(n,f)cross section is very important in basic nuclear physics and applications based on the Th/U fuel *** the time-of-flight method and a multi-cell fast-fission ionization chamber,a novel measurement of the^(232)Th(n,f)cross sec-tion relative to^(235)U in the 1–200 MeV range was performed at the China Spallation Neutron Source Back-n white neutron source(Back-n).The fission event-neutron energy spectra of^(232)Th and^(235)U fission cells were measured in the single-bunch *** 232Th/235U fission cross-sectional ratios were obtained,and the measurement uncertainties were 2.5–3.7%for energies in the 2–20 MeV range and 3.6–6.2%for energies in the 20–200 MeV ***^(232)Th(n,f)cross section was obtained by introducing the standard cross section of^(235)U(n,f).The results were compared with those of previous theoreti-cal calculations,measurements,and *** measured 232Th fission cross section agreed with the main evaluation results in terms of the experimental uncertainty,and 232Th fission resonances were observed in the 1–3 MeV *** present results provide^(232)Th(n,f)cross-sectional data for the evaluation and design of Th/U cycle nuclear systems.

关键词： 232Th(n f)cross section Fast-fission ionization chamber Back-n white neutron source

The In-Flight Realtime Trigger and Localization Software of GECAM

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Research in Astronomy and Astrophysics 2024年第10期24卷 11-24页

作者： xiao-Yun Zhao Shao-lin Xiong Xiang-yang Wen Xin-Qiao li Ce Cai Shuo xiao Qi Luo Wen-Xi Peng Dong-Ya Guo Zheng-Hua An Ke Gong Jin-Yuan liao yan-Qiu Zhang Yue Huang Lu li xing Wen Fei Zhang jing Duan Chen-wei wang Dong-li Shi Peng Zhang Qi-Bin Yi Chao-yang li yan-bing Xu xiao-Hua liang Ya-Qing liu Da-li Zhang Xi-Lei Sun Fan Zhang Gang Chen Huan-Yu wang Sheng yang xiao-jing liu Min Gao Mao-Shun li Jin-Zhou wang xing Zhou Yi Zhao wang-Chen Xue Chao Zheng Jia-Cong liu xing-Bo Han Jin-ling Qi Jia Huang Ke-Ke Zhang Can Chen Xiong-Tao yang Dong-Jie Hou Yu-Sa wang Rui Qiao Xiang Ma xiao-Bo li Ping wang Xin-Ying Song li-Ming Song Shi-Jie Zheng bing li Hong-Mei Zhang Yue Zhu wei Chen Jian-Jian He Zhen Zhang Jin Hou Hong-Jun wang yan-Chao Hao Xiang-Yu wang Zong-Yuan yang Zhi-Long Wen Zhi chang Yuan-Yuan Du Rui Gao xiao-Fei Lan yan-Guo li Gang li Xu-Fang li Fang-Jun Lu Hong Lu Bin Meng Feng Shi Hui wang Hui-Zhen wang Yu-Peng Xu Jia-wei yang Xue-Juan yang Shuang-Nan Zhang Chao-Yue Zhang Cheng-Mo Zhang Zhi-Cheng Tang Cheng Cheng Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Chinese Academy of SciencesBeijing 100049China School of Information Science and Technology Southwest Jiaotong UniversityChengdu 611756China Key Laboratory of Stellar and Interstellar Physics and Department of Physics Xiangtan UniversityXiangtan 411105China Physics and Space Science College China West Normal UniversityNanchong 637002China Department of Astronomy Beijing Normal UniversityBeijing 100875China Innovation Academy for Microsatellites of CAS Shanghai 201203China changchun University of Science and Technology Changchun 130022China Chinese Academy of Sciences South America Center for Astronomy National Astronomical ObservatoriesCASBeijing 100101China

Realtime trigger and localization of bursts are the key functions of GECAM,an all-sky gamma-ray monitor launched on 2020 December *** developed a multifunctional trigger and localization software operating in the CPU of the GECAM Electronic *** onboard software has the following features:high trigger efficiency for real celestial bursts with a suppression of false triggers caused by charged particle bursts and background fluctuation,dedicated localization algorithm optimized for both short and long bursts,and low time latency of the trigger information which is downlinked through the Global Short Message Communication service of the global BeiDou navigation *** paper provides a detailed description of the design and development of the trigger and localization software system for *** covers the general design,workflow,the main functions,and the algorithms used in the *** paper also includes on-ground trigger tests using simulated gamma-ray bursts generated by a dedicated X-ray tube,as well as an overview of the performance for real celestial bursts during its in-orbit operation.

关键词： telescopes instrumentation:detectors methods:observational

The Lyman-alpha Solar Telescope(LST) for the ASO-S mission——Ⅱ. design of LST

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Research in Astronomy and Astrophysics 2019年第11期19卷 33-48页

作者： Bo Chen Hui li Ke-Fei Song Quan-Feng Guo Pei-Jie Zhang ling-Ping He Shuang Dai xiao-Dong wang Hai-Feng wang Chun-Long liu Hong-Ji Zhang Guang Zhang Yunqi wang Shi-Jie liu Hong-Xin Zhang Lei liu Shi-Lei Mao yang liu Jia-Hao Peng Peng wang liang Sun yang liu Zhen-wei Han yan-Long wang Kun Wu Guang-xing Ding Peng Zhou Xin Zheng Ming-Yi Xia Qing-Wen Wu Jin-Jiang Xie Ya Chen Shu-Mei Song Hong wang Bo Zhu chang-Bo Chu Wen-Gang yang li Feng Yu Huang wei-Qun Gan Ying li jing-wei li Lei Lu Jian-Chao Xue Bei-li Ying Ming-Zhe Sun Cheng Zhu wei-Min Bao Lei Deng Zeng-Shan Yin changchun Institute of Optics FineMechanics and PhysicsChinese Academy of SciencesChangchun 130033China State Key Laboratory of Applied Optics Changchun 130033China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210034China School of Astronomy and Space Science University of Science and Technology of ChinaHefei 230026China Xi’an Institute of Optics and Precision Mechanics Chinese Academy of SciencesXi’an 710119China Shandong University Weihai 264209China Innovation Academy for Microsatellites Chinese Academy of SciencesShanghai 201210China

As one of the three payloads for the Advanced Space-based Solar Observatory(ASO-S)mission,the Lyman-alpha(Lyα)Solar Telescope(LST)is composed of three instruments:a Solar Corona Imager(SCI),a LyαSolar Disk Imager(SDI)and a full-disk White-light Solar Telescope(WST).When working in-orbit,LST will simultaneously perform high-resolution imaging observations of all regions from the solar disk to the inner corona up to 2.5 R⊙(R⊙stands for the mean solar radius)with a spatial resolution of 4.8′′and 1.2′′for coronal and disk observations,respectively,and a temporal resolution of 30–120 s and 1–120 s for coronal and disk observations,*** maximum exposure time can be up to20 s due to precise pointing and image stabilization *** the three telescopes of LST,SCI is a dual-waveband coronagraph simultaneously and independently observing the inner corona in the HI Lyα(121.6±10 nm)line and white light(WL)(700±40 nm)wavebands by using a narrowband Lyαbeam splitter and has a field of view(FOV)from 1.1 to 2.5 R⊙.The stray-light suppression level can attainline and 360.0 nm wavebands,respectively,which adopt an off-axis two-mirror reflective structure with an FOV up to 1.2 R⊙,covering the inner coronal edge area and relating to coronal *** present the up-to-date design for the LST payload.

关键词： telescopes—instrumentation high angular resolution—Sun flares—Sun coronal mass ejections(CMEs)—Sun UV radiation

Back-n white neutron source at CSNS and its applications

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Nuclear Science and Techniques 2021年第1期32卷 95-104页

作者： jing-Yu Tang Qi An Jiang-Bo Bai Jie Bao Yu Bao Ping Cao Hao-Lei Chen Qi-Ping Chen Yong-Hao Chen Zhen Chen Zeng-Qi Cui Rui-Rui Fan chang-Qing Feng Ke-Qing Gao xiao-Long Gao Min-Hao Gu chang-Cai Han Zi-Jie Han Guo-Zhu He Yong-Cheng He yang Hong Yi-wei Hu Han-Xiong Huang Xi-Ru Huang Hao-Yu Jiang wei Jiang Zhi-Jie Jiang Han-Tao jing ling Kang Bo li Chao li Jia-Wen li Qiang li xiao li yang li Jie liu Rong liu Shu-Bin liu xing-yan liu Ze Long Guang-Yuan Luan chang-Jun ning Meng-Chen Niu Bin-Bin Qi Jie Ren Zhi-Zhou Ren Xi-Chao Ruan Zhao-Hui Song Kang Sun Zhi-Jia Sun Zhi-Xin Tan Xin-Yi Tang Bin-Bin Tian li-Jiao wang Peng-Cheng wang Zhao-Hui wang Zhong-wei Wen xiao-Guang Wu Xuan Wu li-Kun Xie xiao-Yun yang Yi-wei yang Han Yi li Yu Tao Yu Yong-Ji Yu Guo-Hui Zhang lin-Hao Zhang Qi-wei Zhang Xian-Peng Zhang Yu-liang Zhang Zhi-Yong Zhang Lu-Ping Zhou Zhi-Hao Zhou Ke-Jun Zhu 无 State Key Laboratory of Particle Detection and Electronics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Department of Modern Physics University of Science and Technology of ChinaHefei 230026China Institute of Nuclear Physics and Chemistry China Academy of Engineering PhysicsMianyang 621900China Key Laboratory of Nuclear Data China Institute of Atomic EnergyBeijing 102413China Institute of High Energy Physics Chinese Academy of SciencesBeijing 100049China Spallation Neutron Source Science Center Dongguan 523803China State Key Laboratory of Nuclear Physics and Technology School of PhysicsPeking UniversityBeijing 100871China Northwest Institute of Nuclear Technology Xi’an 710024China University of Chinese Academy of Sciences Beijing 100049China Department of Engineering and Applied Physics University of Science and Technology of ChinaHefei 230026China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of ChinaHefei 230026China The CSNS Back-n Collaboration

Back-streaming neutrons from the spallation target of the China Spallation Neutron Source(CSNS)that emit through the incoming proton channel were exploited to build a white neutron beam facility(the so-called Back-n white neutron source),which was completed in March *** Back-n neutron beam is very intense,at approximately 29107 n/cm2/s at 55 m from the target,and has a nominal proton beam with a power of 100 kW in the CSNS-I phase and a kinetic energy of 1.6 GeV and a thick tungsten target in multiple slices with modest moderation from the cooling water through the *** addition,the excellent energy spectrum spanning from 0.5 eV to 200 MeV,and a good time resolution related tothe time-of-flight measurements make it a typical white neutron source for nuclear data measurements;its overall performance is among that of the best white neutron sources in the *** with advanced spectrometers,detectors,and application utilities,the Back-n facility can serve wide applications,with a focus on neutron-induced cross-sectional *** article presents an overview of the neutron beam characteristics,the experimental setups,and the ongoing applications at Backn.

关键词： White neutron source Nuclear data measurements Experimental setups Neutron applications

The first data release(DR1) of the LAMOST regular survey

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Research in Astronomy and Astrophysics 2015年第8期15卷 1095-1124页

作者： A-li Luo Yong-Heng Zhao Gang Zhao li-Cai Deng xiao-wei liu Yi-Peng jing Gang wang Hao-Tong Zhang Jian-Rong Shi Xiang-Qun Cui Yao-Quan Chu Guo-Ping li Zhong-Rui Bai Yue Wu yan Cai Shu-Yun Cao Zi-Huang Cao Jeffrey L.Carlin Hai-Yuan Chen Jian-Jun Chen Kun-Xin Chen li Chen Xue-Lei Chen xiao-yan Chen Ying Chen Norbert Christlieb Jia-Ru Chu Chen-Zhou Cui Yi-Qiao Dong bing Du Dong-wei Fan Lei Feng Jian-ning Fu Peng Gao Xue-Fei Gong Bo-Zhong Gu yan-Xin Guo Zhan-Wen Han Bo-liang He Jin-liang Hou Yong-Hui Hou Wen Hou Hong-Zhuan Hu ning-Sheng Hu Zhong-Wen Hu Zhi-Ying Huo Lei Jia Fang-Hua Jiang Xiang Jiang Zhi-Bo Jiang Ge Jin xiao Kong Xu Kong Ya-Juan Lei Ai-Hua li chang-Hua li Guang-wei li Hai-ning li Jian li Qi li Shuang li Sha-Sha li Xin-Nan li yan li Yin-Bi li Ye-Ping li Yuan liang Chien-Cheng lin Chao liu Gen-Rong liu Guan-Qun liu Zhi-Gang liu Wen-Zhi Lu Yu Luo Yin-Dun Mao Heidi Newberg Ji-Jun Ni Zhao-Xiang Qi Yong-Jun Qi Shi-Yin Shen Huo-Ming Shi jing Song Yi-Han Song Ding-Qiang Su Hong-Jun Su Zheng-Hong Tang Qing-Sheng Tao Yuan Tian Dan wang Da-Qi wang Feng-Fei wang Guo-Min wang Hai wang Hong-Chi wang Jian wang Jia-ning wang Jian-ling wang Jian-Ping wang Jun-Xian wang Lei wang Meng-Xin wang Shou-Guan wang Shu-Qing wang Xia wang Ya-Nan wang You wang Yue-Fei wang You-Fen wang Peng wei Ming-Zhi wei Hong Wu Ke-Fei Wu Xue-bing Wu Yu-Zhong Wu xiao-Zheng xing ling-Zhe Xu Xin-Qi Xu yan Xu Tai-Sheng yan De-Hua yang Hai-Feng yang Hui-Qin yang Ming yang Zheng-Qiu Yao Yong Yu Hui Yuan Hai-Bo Yuan Hai-Long Yuan wei-Min Yuan Chao Zhai En-Peng Zhang Hua-wei Zhang Jian-Nan Zhang li-Pin Zhang wei Zhang Yong Zhang yan-Xia Zhang Zheng-Chao Zhang Ming Zhao Fang Zhou Xu Zhou Jie Zhu Yong-Tian Zhu Si-Cheng Zou Fang Zuo National Astronomical Observatories Chinese Academy of Sciences Department of Astronomy Peking University Shanghai Astronomical Observatory Chinese Academy of Sciences Nanjing Institute of Astronomical Optics & Technology National Astronomical ObservatoriesChinese Academy of Sciences University of Science and Technology of China Department of Physics Applied Physics and AstronomyRensselaer Polytechnic InstituteTroyNY 12180USA Department of Physics and Astronomy Earlham CollegeRichmondIN 47374USA Universitt Heidelberg Zentrum für AstronomieLandessternwarteKnigstuhl 1269117 HeidelbergGermany Department of Astronomy Beijing Normal University Yunnan Observatories Chinese Academy of Sciences Purple Mountain Observatory Chinese Academy of Sciences

The Large sky Area Multi-Object Fiber Spectroscopic Telescope（LAMOST） general survey is a spectroscopic survey that will eventually cover approximately half of the celestial sphere and collect 10 million spectra of stars, galaxies and QSOs. Objects in both the pilot survey and the first year regular survey are included in the LAMOST DR1. The pilot survey started in October 2011 and ended in June 2012, and the data have been released to the public as the LAMOST Pilot Data Release in August 2012. The regular survey started in September 2012, and completed its first year of operation in June 2013. The LAMOST DR1 includes a total of 1202 plates containing 2 955 336 spectra, of which 1 790 879 spectra have observed signalto-noise ratio（SNR） ≥ 10. All data with SNR ≥ 2 are formally released as LAMOST DR1 under the LAMOST data policy. This data release contains a total of 2 204 696 spectra, of which 1 944 329 are stellar spectra, 12 082 are galaxy spectra and 5017 are quasars. The DR1 not only includes spectra, but also three stellar catalogs with measured parameters： late A,FGK-type stars with high quality spectra（1 061 918 entries）, A-type stars（100 073 entries）, and M-type stars（121 522 entries）. This paper introduces the survey design, the observational and instrumental limitations, data reduction and analysis, and some caveats. A description of the FITS structure of spectral files and parameter catalogs is also provided.

关键词： techniques: spectroscopic survey—data release—catalog