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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

Comparison of remote magnetic versus manual catheter navigation for ablation of atrioventricular nodal reentry tachycardia

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Journal of Geriatric Cardiology 2010年第1期7卷 11-13页

作者： lei gao cai-yi lu shi-wen wang qiao xue wei yan sheng-hua zhou rui chen peng liu jin-yue zhai Institute of Geriatric Cardiology Chinese PLA General Hospital Beijing 100853 China

Objective The purpose of this study was to compare remote magnetic catheter navigation with manual navigation for the ablation of atrioventricular nodal reentry tachycardia （AVNRT）. Methods From November 2007 to November 2009, 30 consecutive patients with AVNRT received radiofrequency ablation in the Institute of Geriatric Cardiology. Of them, 14 were treated with remote magnetic navigation （RMN） and 16 with manual catheter navigation （MCN）. Total fluoroscopic time,procedure time, procedural success rate, and complication rate were compared between the two groups. Results Total fluoroscopy time and precise orientation time were reduced in RMN group compared to MCN group （7.5＋0.3 min vs 13.9~5.3 rain, and 1.0-x-0.3 min vs 3.2：~0.6 min, respectively, both P〈0.05）. Procedural success rates in both groups were 100% and no AVNRT recurred in all patients during 3 months＇ follow-up. The number of lesions delivered was less for RMN group （3.4~1.1 vs 6.3＋2.2, P〈0.05）. Total procedure time （25.6~7.5 rain vs 27.5a：6.2 rain,/〉〉0.05） was similar between the 2 groups. No procedural complications occurred in both groups. Conclusions RMN for mapping and ablation of AVNRT significantly reduce precise orientation time, total fluoroscopy time and number of lesions delivered compared to the conventional technique of manual steering of deflectable catheters. Remote magnetic control mapping and ablation of AVNRT is more safe and feasible （J Geriatr Cardio12010; 7：7-9）.

关键词： magnetic navigation radiofrequency ablation atrioventricular nodal reentry tachycardia

CEPC Technical Design Report

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Radiation Detection Technology and Methods 2024年第1期8卷 I0003-I0016,1-1091页

作者： Waleed Abdallah Tiago Carlos Adorno de Freitas Konstantin Afanaciev Shakeel Ahmad Ijaz Ahmed Xiaocong Ai Abid Aleem Wolfgang Altmannshofer Fabio Alves weiming An rui An Daniele Paolo Anderle Stefan Antusch Yasuo Arai Andrej Arbuzov Abdesslam Arhrib Mustafa Ashry Sha Bai Yu Bai yang Bai Vipul Bairathi Csaba Balazs Philip Bambade Yong Ban Tripamo Bandyopadhyay Shou-Shan Bao Desmond P.Barber Ayse Bat Varvara Batozskaya Subash Chandra Behera Alexander Belyaev Michele Bertucci Xiao-Jun Bi Yuanjie Bi Tianjian Bian Fabrizio Bianchi Thomas Biekotter Michela Biglietti Shalva Bilanishvili Deng Binglin Denis Bodrov Anton Bogomyagkov Serge Bondarenko Stewart Boogert Maarten Boonekamp Marcello Borri Angelo Bosotti Vincent Boudry Mohammed Boukidi Igor Boyko Ivanka Bozovic Giuseppe Bozzi Jean-Claude Brient Anastasiia Budzinskaya Masroor Bukhari Vladimir Bytev Giacomo Cacciapaglia hua cai wenyong cai Wujun cai yijian cai yizhou cai Yuchen cai Haiying cai huacheng cai Lorenzo Calibbi Junsong Cang Guofu Cao Jianshe Cao Antoine Chance xuejun Chang yue Chang Zhe Chang Xinyuan Chang wei Chao Auttakit Chatrabhuti yimin Che Yuzhi Che Bin chen Danping chen Fuqing chen Fusan chen Gang chen Guoming chen hua-Xing chen Huirun chen jinhui chen Ji-Yuan chen Kai chen Mali chen Mingjun chen Mingshui chen Ning chen Shanhong chen Shanzhen chen Shao-Long chen Shaomin chen shiqiang chen Tianlu chen wei chen Xiang chen Xiaoyu chen Xin chen Xun chen Xurong chen Ye chen ying chen Yukai chen Zelin chen Zilin chen Gang chen Boping chen Chunhui chen Hok Chuen cheng huajie cheng Shan cheng Tongguang cheng Yunlong Chi Pietro Chimenti wen Han Chiu Guk Cho Ming-Chung Chu Xiaotong Chu Ziliang Chu Guglielmo Coloretti Andreas Crivellin Hanhua Cui Xiaohao Cui Zhaoyuan Cui Brunella D'Anzi Ling-Yun Dai Xinchen Dai Xuwen Dai Antonio De Maria Nicola De Filippis Christophe De La Taille Francesca De Mori Chiara De Sio Elisa Del Core Shuangxue Deng wei-Tian Deng Zhi Deng Ziyan Deng Bhupal Dev Tang Dewen Biagio Di Micco Ran Ding Siqin Dingl Yadong Ding Haiyi Dong Jianin AGH University of Science and Technology Faculty of Physics and Applied Computer ScienceKrakow Anhui University HefeiAnhui Applied Physics Department Federal Urdu University of ArtsScience and TechnologyIslamabad Banaras Hindu University Institute of ScienceVaranasi Bandirma Onyedi Eylul University Bandirma Beihang University Beijing Beijing Computational Science Research Center Beijing Beijing Conveyi LTD Beijing Beijing Glass Research Institute Co. LtdBeijing Beijing Institute of Technology Beijing Beijing Normal University Beijing Brown University ProvidenceRI Budker Institute of Nuclear Physics Novosibirsk Cadi Ayyad University Laboratory of Fundamental and Applied PhysicsPolydisciplinary FacultyMarrakech cairo University Giza Center for Theory and Computation National Tsing Hua UniversityHsinchu Central China Normal University WuhanHubei Central South University ChangshaHunan Centro de Fisica Teorica de Particulas Universidade Tecnica de LisboaLisboa chengdu KaitengSifang Digital Radio&TV Equipment Co. LtdChengduSichuan China academy of engineering physics MianyangSichuan China building materials academy Beijing China Center of Advanced Science and Technology Beijing China Institute of Atomic Energy Beijing China Jiliang University HangzhouZhejiang China Nuclear Instrument CO. LTDBeijing China University of Geosciences Beijing China University of Geosciences WuhanHubei China University of Mining and Technology XuzhouJiangsu China West Normal University NanchongSichuan Chongqing University Department of PhysicsChongqing Chulalongkorn University Bangkok City University of Hong Kong Department of PhysicsHong Kong Cockcroft Institute Daresbury Cornell University IthacaNY CPPM(AMU/IPhU&CNRS/INP) Marseille Dalian Minzu University DalianLiaoning Dalian University of Technology Department of PhysicsDalian Deutsches Elektronen-Synchrotron DESY Hamburg Dzhelepov Laboratory of Nuclear Problems of Joint Institute for Nuclear Research(DLNP jinR) Dubna East China University Of Science And Technol

The Circular Electron Positron Collider(CEPC)is a large scientific project initiated and hosted by China,fostered through extensive collaboration with international *** complex comprises four accelerators:a 30 GeV Linac,a 1.1 GeV Damping Ring,a Booster capable of achieving energies up to 180 GeV,and a Collider operating at varying energy modes(Z,W,H,and tt).The Linac and Damping Ring are situated on the surface,while the subterranean Booster and Collider are housed in a 100 km circumference underground tunnel,strategically accommodating future expansion with provisions for a potential Super Proton Proton Collider(SPPC).The CEPC primarily serves as a Higgs *** its baseline design with synchrotron radiation(SR)power of 30 MW per beam,it can achieve a luminosity of 5×10^(34)cm^(-2)s^(-1)per interaction point(IP),resulting in an integrated luminosity of 13 ab^(-1)for two IPs over a decade,producing 2.6 million Higgs *** the SR power to 50 MW per beam expands the CEPC's capability to generate 4.3 million Higgs bosons,facilitating precise measurements of Higgs coupling at sub-percent levels,exceeding the precision expected from the HL-LHC by an order of *** Technical Design Report(TDR)follows the Preliminary Conceptual Design Report(Pre-CDR,2015)and the Conceptual Design Report(CDR,2018),comprehensively detailing the machine's layout,performance metrics,physical design and analysis,technical systems design,R&D and prototyping efforts,and associated civil engineering ***,it includes a cost estimate and a preliminary construction timeline,establishing a framework for forthcoming engineering design phase and site selection *** is anticipated to begin around 2027-2028,pending government approval,with an estimated duration of 8 *** commencement of experiments and data collection could potentially be initiated in the mid-2030s.

关键词： initiated exceeding precise

Paired quasi-periodic pulsations of hard X-ray emission in a solar flare

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Science China(Physics,Mechanics & Astronomy) 2023年第5期66卷 195-206页

作者： Hai-sheng Zhao Dong Li Shao-Lin Xiong yan-Qiu Zhang yang Su wei chen yi Zhao Xiao-Bo Li Jia-Cong liu wen-Xi peng rui qiao Xin-qiao Li Xiang-yang wen Li-Ming Song shi-Jie Zheng Xin-ying Song Xiao-Yun Zhao yue huang Shuang-Nan Zhang Shuo Xiao Ce cai Zheng-hua An Can chen Gang chen wei chen yan-Qi Du Min gao Ke Gong Dong-Ya Guo Zhi-wei Guo Jian-Jian He Bin Li Chao Li Chao-yang Li Gang Li Jian-Hui Li lu Li Qing-Xin Li yan-Guo Li jing Liang Xiao-hua Liang jin-Yuan Liao Xiao-jing liu Ya-Qing liu Qi luo Xiang Ma Bin Meng Ge Ou Dong-Li shi jing-yan shi Gong-Xing Sun Xi-lei Sun You-Li Tuo chen-wei wang Hui wang jin wang jin-zhou wang Ping wang wen-Shuai wang Hong Wu sheng-lun Xie yan-Bing Xu Yu-peng Xu wang-chen xue sheng yang Min Yao Jian-ying Ye Qi-Bin yi Chao-yue Zhang Da-Li Zhang Fan Zhang Fei Zhang Hong-Mei Zhang Kai Zhang peng Zhang Xiao-lu Zhang Zhen Zhang Guo-ying Zhao shi-yi Zhao Chao Zheng Xing zhou yue Zhu Key Laboratory for Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Purple Mountain Observatory Chinese Academy of SciencesNanjing 210023China University of Chinese Academy of Sciences Beijing 100049China Department of Astronomy Beijing Normal UniversityBeijing 100875China School of Computing and Artificial Intelligence Southwest Jiaotong UniversityChengdu 611756China Physics and Space Science College China West Normal UniversityNanchong 637002China Key Laboratory of Stellar and Interstellar Physics and Department of Physics Xiangtan UniversityXiangtan 411105China Institute of Astrophysics Central China Normal UniversityWuhan 430079China School of Physics Changchun University of Science and TechnologyChangchun 130022China College of Physics and Engineering Qufu Normal UniversityQufu 273165China College of Physics Sciences&Technology Hebei UniversityBaoding 071002China

We investigate high time resolution data obtained by the Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor(GECAM)during the flare event on 2022 April 21 at 01:52 *** subpeaks with durations of 4-6 s have been detected in the hard X-ray precursor phase,and the key feature is that they appear in pairs and seem like double-peak *** subpeaks are rarely observed in hard X-ray band and confirmed by the microwave obtained by Nobeyama Radio Polarimeters(NoRP)and Radio Solar Telescope Network(RSTN).While an exponential function can describe the continuum component of the time profile from the precursor to part of the impulsive *** periods of quasi-periodic pulsations(QPPs)are detected to be about 7.3 and 12.8 s for the precursor and impulsive phase,respectively,with at least 95%confidence *** paired QPPs are assumed to be double-peak QPPs and then the scenario of current loop coalescence model is found to be in good agreement with our *** precursor phase can be interpreted as the oscillating coalescence of two islands,while the impulsive phase can be interpreted as more islands to coalesce one by one to form larger islands.

关键词： solar flare QPPs loop coalescence circular-ribbon flare

STCF conceptual design report (Volume 1): Physics & detector

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Frontiers of physics 2024年第1期19卷 1-154页

作者： M.Achasov X.C.Ai L.P.An R.Aliberti Q.An X.Z.Bai Y.Bai O.Bakina A.Barnyakov V.Blinov V.Bobrovnikov D.Bodrov A.Bogomyagkov A.Bondar I.Boyko Z.H.Bu F.M.cai H.cai J.J.Cao Q.H.Cao X.Cao Z.Cao Q.Chang K.T.Chao D.Y.chen H.chen H.X.chen J.F.chen K.chen L.L.chen P.chen S.L.chen S.M.chen S.chen S.P.chen W.chen X.chen X.F.chen X.R.chen Y.chen Y.Q.chen H.Y.cheng J.cheng S.cheng T.G.cheng J.P.Dai L.Y.Dai X.C.Dai D.Dedovich A.Denig I.Denisenko J.M.Dias D.Z.Ding L.Y.Dong W.H.Dong V.Druzhinin D.S.Du Y.J.Du Z.G.Du L.M.Duan D.Epifanov Y.L.Fan S.S.Fang Z.J.Fang G.Fedotovich C.Q.Feng X.Feng Y.T.Feng J.L.Fu J.gao Y.N.gao P.S.Ge C.Q.Geng L.S.Geng A.Gilman L.Gong T.Gong B.Gou W.Gradl J.L.Gu A.Guevara L.C.Gui A.Q.Guo F.K.Guo J.C.Guo J.Guo Y.P.Guo Z.H.Guo A.Guskov K.L.Han L.Han M.Han X.Q.Hao J.B.He S.Q.He X.G.He Y.L.He Z.B.He Z.X.Heng B.L.Hou T.J.Hou Y.R.Hou C.Y.Hu H.M.Hu K.Hu R.J.Hu W.H.Hu X.H.Hu Y.C.Hu J.hua G.S.huang J.S.huang M.huang Q.Y.huang W.Q.huang X.T.huang X.J.huang Y.B.huang Y.S.huang N.Hüsken V.Ivanov Q.P.Ji J.J.Jia S.Jia Z.K.Jia H.B.Jiang J.Jiang S.Z.Jiang J.B.Jiao Z.Jiao H.J.jing X.L.Kang X.S.Kang B.C.Ke M.Kenzie A.Khoukaz I.Koop E.Kravchenko A.Kuzmin Y.lei E.Levichev C.H.Li C.Li D.Y.Li F.Li G.Li G.Li H.B.Li H.Li H.N.Li H.J.Li H.L.Li J.M.Li J.Li L.Li L.Li L.Y.Li N.Li P.R.Li R.H.Li S.Li T.Li W.J.Li X.Li X.H.Li X.Q.Li X.H.Li Y.Li Y.Y.Li Z.J.Li H.Liang J.H.Liang Y.T.Liang G.R.Liao L.Z.Liao Y.Liao C.X.Lin D.X.Lin X.S.Lin B.J.liu C.W.liu D.liu F.liu G.M.liu H.B.liu J.liu J.J.liu J.B.liu K.liu K.Y.liu K.liu L.liu Q.liu S.B.liu T.liu X.liu Y.W.liu Y.liu Y.L.liu Z.Q.liu Z.Y.liu Z.W.liu I.Logashenko Y.Long C.G.lu J.X.lu N.lu Q.F.Lü Y.lu Y.lu Z.lu P.lukin F.J.luo T.luo X.F.luo Y.H.luo H.J.Lyu X.R.Lyu J.P.Ma P.Ma Y.Ma Y.M.Ma F.Maas S.Malde D.Matvienko Z.X.Meng R.Mitchell A.Nefediev Y.Nefedov S.L.Olsen Q.Ouyang P.Pakhlov G.Pakhlova X.Pan Y.Pan E.Passemar Y.P.Pei H.P.peng L.peng X.Y.peng X.J.peng K.Peters S.Pivovarov E.Pyata B.B.Qi Y.Q.Qi W.B.Qian Y.Qian C.F.qiao J.J.Qin J.J.Qin L.Q.Qin X.S.Qin T.L.Qiu J.Rademacker C.F.Redmer H.Y.Sang Anhui University Hefei 230039China Beihang University Beijing 100191China Budker Institute of Nuclear Physics Novosibirsk 630090Russia CAS Key Laboratory of Theoretical Physics Institute of Theoretical PhysicsChinese Academy of SciencesBeijing 100190China Cavendish Laboratory University of CambridgeJJ Thomson AveCambridge CB30HEUnited Kingdom Central China Normal University Wuhan 430079China Central South University Changsha 410083China China University of Geosciences Wuhan 430074China China University of Mining and Technology Xuzhou 221116China École Polytechnique Fédérale de Lausanne(EPFL) LausanneSwitzerland Fudan University Shanghai 200433China Goethe University Frankfurt D-60325 Frankfurt am MainGermany Guangxi Normal University Guilin 541004China Guangxi Uninversity Nanning 530004China Hangzhou Institute for Advanced Study UCASHangzhou 310024China Hebei Normal University Shijiazhuang 050024China Hebei University Baoding 071002China Hefei University of Technology Hefei 230601China Helmholtz Institute Mainz Staudinger Weg 18D-55099 MainzGermany Henan Normal University Xinxiang 453007China Henan University Kaifeng 475004China High Energy Physics Center Chung-Ang UniversitySeoul 06974Korea Higher School of Economy 11 Pokrovsky Bulvar Moscow 109028Russia huangshan University Huangshan 245000China Hubei University of Automotive Technology Shiyan 442002China Hunan Normal University Changsha 410081China Hunan University of Science and Technology Xiangtan 411201China Hunan University Changsha 410082China Indiana University BloomingtonIndiana 47405USA Inner Mongolia University Hohhot 010021China Institute of Advanced Science Facilities Shenzhen 518107China Institute of High Energy Physics Chinese Academy of SciencesBeijing 100049China Institute of Modern Physics Chinese Academy of SciencesLanzhou 730000China Institute of Physics Academia SinicaTaipeiTaiwan 11529China Institute of Theoretical Physics Chinese Academy of SciencesBeijing 100190China Jilin University Changch

The superτ-charm facility(STCF)is an electron–positron collider proposed by the Chinese particle physics *** is designed to operate in a center-of-mass energy range from 2 to 7 GeV with a peak luminosity of 0.5×10^(35) cm^(–2)·s^(–1) or *** STCF will produce a data sample about a factor of 100 larger than that of the presentτ-charm factory—the BEPCII,providing a unique platform for exploring the asymmetry of matter-antimatter(charge-parity violation),in-depth studies of the internal structure of hadrons and the nature of non-perturbative strong interactions,as well as searching for exotic hadrons and physics beyond the Standard *** STCF project in China is under development with an extensive R&D *** document presents the physics opportunities at the STCF,describes conceptual designs of the STCF detector system,and discusses future plans for detector R&D and physics case studies.

关键词： electron–positron collider tau-charm region high luminosity STCF detector conceptual design

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

Timing analysis of the black hole candidate EXO 1846–031 with Insight-HXMT monitoring

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Research in Astronomy and Astrophysics 2021年第3期21卷 193-204页

作者： He-Xin liu yue huang Guang-cheng Xiao Qing-Cui Bu jin-lu Qu Shu Zhang Shuang-Nan Zhang Shu-Mei Jia Fang-Jun lu Xiang Ma Lian Tao wei Zhang Li chen Li-Ming Song Ti-Pei Li Yu-peng Xu xue-lei Cao Yong chen Cong-Zhan liu Ce cai Zhi Chang Gang chen Tian-Xiang chen yi-Bao chen Yu-peng chen wei Cui wei-wei Cui jing-Kang Deng Yong-wei Dong Yuan-Yuan Du Min-xue Fu Guan-hua gao He gao Min gao Ming-Yu Ge Yu-Dong Gu Ju Guan cheng-cheng Guo Da-wei Han Jia Huo lu-hua Jiang wei-Chun Jiang jing jin Yong-Jie jin Ling-Da Kong Bing Li cheng-Kui Li Gang Li Mao-Shun Li wei Li Xian Li Xiao-Bo Li Xu-Fang Li yang-Guo Li Zheng-wei Li Xiao-hua Liang jing-Yuan Liao Bai-sheng liu Guo-Qing liu Hong-wei liu Xiao-jing liu yi-Nong liu Bo lu xue-Feng lu Qi luo Tao luo Bin Meng yi Nang Jian-yin Nie Ge Ou Na Sai Ren-cheng Shang Xin-ying Song Liang Sun ying Tan You-Li Tuo chen wang Guo-Feng wang Juan wang Ling-Jun wang weng-Shuai wang Yu-Sa wang Xiang-yang wen Bai-yang Wu Bo-Bing Wu Mei Wu Shuo Xiao Shao-Lin Xiong He Xu Jia-wei yang sheng yang yan-Ji yang yi-Jung yang Qi-Bin yi Qian-Qing yin Yuan You Ai-Mei Zhang cheng-Mo Zhang Fan Zhang Hong-Mei Zhang Juan Zhang Tong Zhang Wan-Chang Zhang wen-Zhao Zhang yi Zhang yi-Fei Zhang Yong-Jie Zhang Yuan-Hang Zhang yue Zhang Zhao Zhang Zhi Zhang Zi-Liang Zhang Hai-sheng Zhao Xiao-Fan Zhao shi-Jie Zheng Yao-Guang Zheng Deng-Ke zhou Jian-Feng zhou Yu-Xuan Zhu Ren-Lin Zhuang yue Zhu 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 Institut fur Astronomie und Astrophysik Kepler Center for Astro and Particle PhysicsEberhard Karls Universität72076 TubingenGermany Department of Astronomy Beijing Normal UniversityBeijing 100088China Department of Astronomy Tsinghua UniversityBeijing 100084China Department of Physics Tsinghua UniversityBeijing 100084China Department of Engineering Physics Tsinghua UniversityBeijing 100084China Key Laboratory of Space Astronomy and Technology National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China College of Physics Sciences&Technology Hebei UniversityBaoding 071002Hebei ProvinceChina

We present the observational results from a detailed timing analysis of the black hole candidate EXO 1846-031 during its outburst in 2019 with the observations of Insight-HXMT,NICER and *** outburst can be classified roughly into four different ***-C quasi-periodic oscillations(QPOs)observed by NICER(about 0.1-6 Hz)and Insight-HXMT(about 0.7-8 Hz)are also reported in this ***,we study various physical quantities related to QPO *** QPO rms-frequency relationship in the energy band 1-10 keV indicates that there is a turning pointing in frequency around2 Hz,which is similar to that of GRS 1915+105.A possible hypothesis for the relationship above may be related to the inclination of the source,which may require a high inclination to explain *** relationships between QPO frequency and QPO rms,hardness,total fractional rms and count rate have also been found in other transient sources,which can indicate that the origin of type-C QPOs is non-thermal.

关键词： X-ray binaries black hole candidate QPO EXO 1846–031

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Science Bulletin 2024年第4期69卷 449-457页

作者： LHAASO Collaboration Zhen Cao Chuandong gao Cong Li Ruo-Yu liu ruizhi yang 不详 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 ChengduChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China University of Science and Technology of China Hefei 230026China

We report the detection of aγ-ray bubble spanning at least 100deg2 in ultra-high energy(UHE)up to a few PeV in the direction of the star-forming region Cygnus X,implying the presence super PeVatron(s)accelerating protons to at least 10 PeV.A log-parabola form with the photon indexΓ(E)=(2.71±0.02)+(0.11±0.02)×log10(E/10 TeV)is found fitting the gamma-ray energy spectrum of the bubble *** sources,“hot spots”correlated with very massive molecular clouds,and a quasi-spherical amorphousγ-ray emitter with a sharp central brightening are observed in the *** the core of~0.5°,spatially associating with a region containing massive OB association(Cygnus OB2)and a microquasar(Cygnus X-3),as well as previously reported multi-TeV sources,an enhanced concentration of UHEγ-rays is observed with 2 photons at energies above 1 *** general feature of the bubble,the morphology,and the energy spectrum,are reasonably reproduced by the assumption of a particle accelerator in the core,continuously injecting protons into the ambient medium.

关键词： Cosmic rays γ-rays Interstellar medium Star cluster

Amplitude analysis of the decays D^(0)→π^(+)π^(−)π^(+)π^(−)and D^(0)→π^(+)π^(−)π^(0)π^(0)

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Chinese Physics C 2024年第8期48卷 6-33页

作者： M.Ablikim M.N.Achasov P.Adlarson O.Afedulidis X.C.Ai R.Aliberti A.Amoroso Q.An Y.Bai O.Bakina I.Balossino Y.Ban H.-R.Bao V.Batozskaya K.Begzsuren N.Berger M.Berlowski M.Bertani D.Bettoni F.Bianchi E.Bianco A.Bortone I.Boyko R.A.Briere A.Brueggemann H.cai X.cai A.Calcaterra G.F.Cao N.Cao S.A.Cetin J.F.Chang W.L.Chang G.R.Che G.Chelkov C.chen C.H.chen Chao chen G.chen H.S.chen M.L.chen S.J.chen S.L.chen S.M.chen T.chen X.R.chen X.T.chen Y.B.chen Y.Q.chen Z.J.chen Z.Y.chen S.K.Choi X.Chu G.Cibinetto F.Cossio J.J.Cui H.L.Dai J.P.Dai A.Dbeyssi R.E.de Boer D.Dedovich C.Q.Deng Z.Y.Deng A.Denig I.Denysenko M.Destefanis F.De Mori B.Fang S.S.Fang W.X.Fang Y.Fang Y.Q.Fang R.Farinelli L.Fava F.Feldbauer G.Felici C.Q.Feng J.H.Feng Y.T.Feng K.Fischer M.Fritsch C.D.Fu J.L.Fu Y.W.Fu H.gao Y.N.gao yang gao S.Garbolino I.Garzia P.T.Ge Z.W.Ge C.Geng E.M.Gersabeck B.Ding X.X.Ding Y.Ding Y.Ding J.Dong L.Y.Dong M.Y.Dong X.Dong M.C.Du S.X.Du Z.H.Duan P.Egorov Y.H.Fan J.Fang JA.Gilman K.Goetzen L.Gong W.X.Gong W.Gradl S.Gramigna M.Greco M.H.Gu Y.T.Gu C.Y.Guan Z.L.Guan A.Q.Guo L.B.Guo M.J.Guo R.P.Guo Y.P.Guo A.Guskov J.Gutierrez K.L.Han T.T.Han X.Q.Hao F.A.Harris K.K.He K.L.He F.H.Heinsius C.H.Heinz Y.K.Heng C.Herold T.Holtmann P.C.Hong G.Y.Hou X.T.Hou Y.R.Hou Z.L.Hou B.Y.Hu H.M.Hu J.F.Hu T.Hu Y.Hu G.S.huang K.X.huang L.Q.huang X.T.huang Y.P.huang T.Hussain F.H\"olzken N.H\"usken N.in der Wiesche M.Irshad J.Jackson S.Janchiv J.H.Jeong Q.Ji Q.P.Ji W.Ji X.B.Ji X.L.Ji Y.Y.Ji X.Q.Jia Z.K.Jia D.Jiang H.B.Jiang P.C.Jiang S.S.Jiang T.J.Jiang X.S.Jiang Y.Jiang J.B.Jiao J.K.Jiao Z.Jiao S.jin Y.jin M.Q.jing X.M.jing T.Johansson S.Kabana N.Kalantar-Nayestanaki X.L.Kang X.S.Kang M.Kavatsyuk B.C.Ke V.Khachatryan A.Khoukaz R.Kiuchi O.B.Kolcu B.Kopf M.Kuessner X.Kui A.Kupsc W.K\"uhn J.J.Lane P.Larin L.Lavezzi T.T.lei Z.H.lei H.leithoff M.Lellmann T.Lenz C.Li C.Li C.H.Li cheng Li D.M.Li F.Li G.Li H.Li H.B.Li H.J.Li H.N.Li Hui Li J.R.Li J.S.Li K.Li L.J.Li L.K.Li lei Li M.H.Li P.R.Li Q.M.Li Q.X.Li R.Li S.X.Li T.Li W.D.Li W.G.Li X.Li X.H.Li X.L.Li X.Y.Li Y Institute of High Energy Physics Chinese Academy of SciencesBeijing 100049China Beihang University Beijing 100191China Bochum Ruhr-University D-44780 BochumGermany Budker Institute of Nuclear Physics SB RAS(BINP) Novosibirsk 630090Russia Carnegie Mellon University PittsburghPennsylvania 15213USA Central China Normal University Wuhan 430079China Central South University Changsha 410083China China Center of Advanced Science and Technology Beijing 100190China China University of Geosciences Wuhan 430074China Chung-Ang University Seoul06974Republic of Korea COMSATS University Islamabad Lahore CampusDefence RoadOff Raiwind Road54000 LahorePakistan Fudan University Shanghai 200433China GSI Helmholtzcentre for Heavy Ion Research GmbH D-64291 DarmstadtGermany Guangxi Normal University Guilin 541004China Guangxi University Nanning 530004China Hangzhou Normal University Hangzhou 310036China Hebei University Baoding 071002China Helmholtz Institute Mainz Staudinger Weg 18D-55099 MainzGermany Henan Normal University Xinxiang 453007China Henan University Kaifeng 475004China Henan University of Science and Technology Luoyang 471003China Henan University of Technology Zhengzhou 450001China huangshan College Huangshan 245000China Hunan Normal University Changsha 410081China Hunan University Changsha 410082China Indian Institute of Technology Madras Chennai 600036India Indiana University BloomingtonIndiana 47405USA INFN Laboratori Nazionali di Frascati INFN Laboratori Nazionali di FrascatiI-00044FrascatiItaly INFN Laboratori Nazionali di Frascati INFN Sezione di PerugiaI-06100PerugiaItaly INFN Laboratori Nazionali di Frascati University of PerugiaI-06100PerugiaItaly INFN Sezione di Ferrara INFN Sezione di FerraraI-44122FerraraItaly INFN Sezione di Ferrara University of FerraraI-44122FerraraItaly Inner Mongolia University Hohhot 010021China Institute of Modern Physics Lanzhou 730000China Institute of Physics and Technology Peace Avenue 54BUlaanbaatar 13330Mongolia Instituto de A

Using e^(+)e^(−)annihilation data corresponding to an integrated luminosity of 2.93 fb^(−1)taken at the center-of-mass energy√s=3.773 GeV with the BESIII detector,a joint amplitude analysis is performed on the decays D^(0)→π^(+)π^(−)π^(+)π^(−)and D^(0)→π^(+)π^(−)π^(0)π^(0)(non-η).The fit fractions of individual components are obtained,and large interferences among the dominant components of the decays D^(0)→a_(1)(1260)π,D^(0)→π(1300)π,D^(0)→ρ(770)ρ(770),and D^(0)→2(ππ)_(S)are observed in both *** the obtained amplitude model,the CP-even fractions of D^(0)→π^(+)π^(−)π^(+)π^(−)and D^(0)→π^(+)π^(−)π^(0)π^(0)(non-η)are determined to be(75.2±1.1_(stat).±1.5_(syst.))%and(68.9±1.5_(stat).±2.4_(syst.))%,*** branching fractions of D^(0)→π^(+)π^(−)π^(+)π^(−)and D^(0)→π^(+)π^(−)π^(0)π^(0)(non-η)are measured to be(0.688±0.010_(stat.)±0.010_(syst.))%and(0.951±0.025_(stat.)±0.021_(syst.))%,*** amplitude analysis provides an important model for the binning strategy in measuring the strong phase parameters of D^(0)→4πwhen used to determine the CKM angleγ(ϕ_(3))via the B^(−)→DK^(−)decay.

关键词： BESIII D^(0)meson decays amplitude analysis CP-even fraction