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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

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

SAPT:a synchrotron-based proton therapy facility in Shanghai

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Nuclear Science and Techniques 2023年第10期34卷 36-46页

作者： Man-zhou zhang De-Ming li li-Ren Shen Hai-Rong zhang Zhi-ling Chen Han-Wen Du Ming Gu Rui li De-Kang liu Yue-Hu Pu Jun-Feng Yu Jian-Feng Chen chu Chen chun-long Guo hao Guo Ge-Yang Jiang Zhi-Qiang Jiang lin jin Wen-jing li Xiu-Fang li Ye lin Ming liu yong-hao liu Ya-Juan liu Ming Lv Qing-Ru Mi lian-Hua Ouyang Wei-Guo Shi Hang Shu Qi-Sheng Tang Kun Wang Zhi-Shan Wang Jun Wu Xiao-Bing Wu Jia-Qiang Xu Wen-Zhen Xu Chong-Xian Yin cheng Yu Ren-Xian Yuan Qi-Bing Yuan Hai-Qun zhang Miao zhang Wen-Zhi zhang li-Ying zhao Wei-Min zhou Shou-Xian Fang Xi-Dong Sun Zhen-Tang zhao Shanghai Institute of Applied Physics Chinese Academy of SciencesShanghai 201800China Shanghai Advanced Research Institute Chinese Academy of SciencesShanghai 201204China APACTRON Particle Equipment Co. Ltd.Shanghai 201815China The Institute of High Energy Physics Chinese Academy of SciencesBeijing 100049China

Because of its excellent dose distribution,proton therapy is becoming increasingly popular in the medical application of cancer treatment.A synchrotron-based proton therapy facility was designed and constructed in *** synchrotron,beam delivery system,and other technical systems were commissioned and reached their expected *** a clinical trial of 47 patients was finished,the proton therapy facility obtained a registration certificate from the National Medical Products *** characteristics of the accelerator and treatment systems are described in this article.

关键词： Proton therapy Synchrotron Slow extraction Gantry Beam delivery system

The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST)

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Research in Astronomy and Astrophysics 2012年第9期12卷 1197-1242页

作者： Xiang-Qun Cui yong-Heng zhao Yao-Quan chu Guo-Ping li Qi li li-Ping zhang Hong-Jun Su Zheng-Qiu Yao Ya-Nan Wang Xiao-Zheng Xing Xin-Nan li yong-Tian Zhu Gang Wang Bo-Zhong Gu A-li Luo Xin-Qi Xu Zhen-Chao zhang Gen-Rong liu hao-Tong zhang De-Hua Yang Shu-Yun Cao Hai-Yuan Chen Jian-Jun Chen Kun-Xin Chen Ying Chen Jia-Ru chu Lei Feng Xue-Fei Gong yong-Hui Hou Hong-Zhuan Hu Ning-Sheng Hu Zhong-Wen Hu Lei Jia Fang-Hua Jiang Xiang Jiang Zi-Bo Jiang Ge jin Ai-Hua li Yan li Ye-Ping li Guan-Qunliu Zhi-Gang liu Huo-Ming Shi Zheng-Hong Tang Qing-Sheng Tao Xiang-Yan Yuan Chao Zhai jing zhang Yan-Xia zhang yong zhang Ming zhao Fang zhou Guo-Hua zhou Jie Zhu Si-cheng Zou National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China yzhao @ *** Nanjing Institute of Astronomical Optics and Technology National Astronomical ObservatoriesChinese Academy of Sciences Nanjing 210042 China University of Science and Tecfinologyof China Hefei 230026 China Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai 200030 China Institute of Architecture Design and Research Chinese Academy of Sciences Beijing 100190China

The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, also called the Guo Shou jing Telescope) is a special reflecting Schmidt telescope. LAMOST’s special design allows both a large aperture (effective aperture of 3.6 m–4.9 m) and a wide field of view (FOV) (5°). It has an innovative active reflecting Schmidt configuration which continuously changes the mirror’s surface that adjusts during the observation process and combines thin deformable mirror active optics with segmented active optics. Its primary mirror (6.67m×6.05 m) and active Schmidt mirror (5.74m×4.40 m) are both segmented, and composed of 37 and 24 hexagonal sub-mirrors respectively. By using a parallel controllable fiber positioning technique, the focal surface of 1.75 m in diameter can accommodate 4000 optical fibers. Also, LAMOST has 16 spectrographs with 32 CCD cameras. LAMOST will be the telescope with the highest rate of spectral acquisition. As a national large scientific project, the LAMOST project was formally proposed in 1996, and approved by the Chinese government in 1997. The construction started in 2001, was completed in 2008 and passed the official acceptance in June 2009. The LAMOST pilot survey was started in October 2011 and the spectroscopic survey will launch in September 2012. Up to now, LAMOST has released more than 480 000 spectra of objects. LAMOST will make an important contribution to the study of the large-scale structure of the Universe, structure and evolution of the Galaxy, and cross-identification of multiwaveband properties in celestial objects.

关键词： techniques: wide field telescope - active optics - multi fiber - spectroscopy survey - data reduction

Data processing and data products from 2017 to 2019 campaign of astronomical site testing at Ali,Daocheng and Muztagh-ata

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Research in Astronomy and Astrophysics 2020年第6期20卷 109-130页

作者： Zi-Huang Cao jin-Xin hao Lu Feng Hugh RAJones Jian li jing Xu li-yong liu Teng-Fei Song Jian-Feng Wang Hua-lin Chen Yan-Jie Xue Huang Shen yong-Heng zhao zhao-Xiang Qi Jian-Rong Shi Yuan Tian Zheng Wang Xia Wang jin-liang Hou jin-Ming Bai Ji Yang Xu zhou yong-Qiang Yao Jia Yin Ali Esamdin Guang-Xin Pu Peng Wei chun-Hai Bai Guo-Jie Feng Lu Ma Xuan zhang Yu liu Chong Pei Zhi-Xia Shen Yun-Ying Jiang Jian-Feng Tian Xian-Qun Zeng Zhi-Gang Hou Xu Yang Jun-Bo zhang Shi-long liao Dong-Wei Fan Yun-Fei Xu Jian-Ping Xiong Tai-Sheng Yan Xi zhang Chang-Hua li Yi-Han Tao Si-cheng Yu Zhi-Song Cao Hong-Shuai Wang National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China University of Chinese Academy of Sciences Beijing 100049China Shanghai Astronomical Observatory Chinese Academy of SciencesShanghai 200030China Centre for Astrophysics University of HertfordshireHatfieldUK School of Journalism Communication University of ChinaBeijing 100024China Nanjing Institute of Astronomical Optics&Technology Chinese Academy of SciencesNanjing 210042China Xinjiang Astronomical Observatory Chinese Academy of SciencesUrumqi 830011China Yunnan Observatories Chinese Academy of SciencesKunming 650216China Purple Mountain Observatory Chinese Academy of SciencesNanjing 210033China Beijing Kaiyang Space Technology Co. LtdBeijing 100085China

Based on previous site testing and satellite cloud data,Ali,Daocheng and Muztagh-ata have been selected as candidate sites for the Large Optical/Infrared Telescope(LOT) in *** present the data collection,processing,management and quality analysis for our site testing based on using similar *** analyze meteorological data,seeing,background light,cloud and precipitable water vapor data from 2017 March 10 to 2019 March *** also investigated the relative usefulness of our all-sky camera data in comparison to that from the meteorological TERRA satellite data based on a night-by-night comparison of the correlation and consistency between *** find a 6% discrepancy arising from a wide range of factors.

关键词： LOT Site-selection-data processing

Data release of the LAMOST pilot survey

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Research in Astronomy and Astrophysics 2012年第9期12卷 1243-1246页

作者： A-li Luo hao-Tong zhang yong-Heng zhao Gang zhao Xiang-Qun Cui Guo-Ping li Yao-Quan chu Jian-Rong Shi Gang Wang Jian-Nan zhang Zhong-Rui Bai Xiao-Yan Chen Feng-Fei Wang Yan-Xin Guo Jian-Jun Chen Bing Du Xiao Kong Ya-Juan Lei Yin-Bi li Yi-Han Song Yue Wu Yan-Xia zhang Xin-lin zhou Fang Zuo Peng Du lin He Wen Hou Yi-Qiao Dong Jian li Guang-Wei li Shuang li jing Song Yuan Tian Meng-Xin Wang yong-Hui Hou Zhi-Ying Huo Hong-Zhuan Hu Ning-Sheng Hu Zhong-Wen Hu Lei Jia Fang-Hua Jiang Xiang Jiang Zi-Bo Jiang Ge jin Ai-Hua li Qi li Yin-Dun Mao Zheng-Hong Tang Qing-Sheng Tao liang-Ping Tu Da-Qing Wang Dan Wang Jian-Ping Wang Lei Wang Shou-Guan Wang Shu-Qing Wang Ya-Nan Wang You Wang Yue-Fei Wang Ming-Zhi Wei Xiang-Xiang Xue Xiao-Zheng Xing ling-Zhe Xu Xin-Qi Xu Yan Xu De-Hua Yang Shi-Hai Yang Zheng-Qiu Yao yong Yu Hui Yuan Chao Zhai En-Peng zhang jing zhang li-Ping zhang Weizhang yong zhang Zhen-Chao zhang Ming zhao Fang zhou yong-Tian Zhu Jie Zhu Si-cheng Zou National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China lal @ lamost o rg Nanjing Institute of Astronomical Optics and Technology National Astronomical ObservatoriesChinese Academy of Sciences Nanjing 210042 China University of Science and Technologyof China Hefei 230026 China Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai 200030 China Institute of Architecture Design and Research Chinese Academy of Sciences Beijing 100190China

This paper describes the data release of the LAMOST pilot survey, which includes data reduction, calibration, spectral analysis, data products and data access. The accuracy of the released data and the information about the FITS headers of spectra are also introduced. The released data set includes 319 000 spectra and a catalog of these objects.

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

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

Panda X-III： Searching for neutrinoless double beta decay with high pressure ^(136)Xe gas time projection chambers

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Science China(Physics,Mechanics & Astronomy) 2017年第6期60卷 8-47页

作者： Xun Chen Chang Bo fu Javier Galan Karl Giboni Franco Giuliani ling Hui Gu Ke Han Xiang Dong Ji Heng lin Jiang Lai liu Kai Xiang Ni Hiroki Kusano Xiang Xiang Ren Shao Bo Wang yong Yang Dan zhang Tao zhang li zhao Xiang Ming Sun Shou Yang Hu Si Yu Jian Xing long li Xiao Mei li hao liang Huan Qiao zhang Ming Rui zhao jing zhou Ya Jun Mao hao Qiao Si Guang Wang Ying Yuan Meng Wang Amir N.Khan Neill Raper Jian Tang Wei Wang Jia Ning Dong Chang Qing Feng cheng li Jian Bei liu Shu Bin liu Xiao lian Wang Dan Yang Zhu Juan F.Castel Susana Cebri'an Theopisti Dafni Javier G.Garza Igor G.Irastorza Francisco J.Iguaz Gloria Luz ′on Hector Mirallas Stephan Aune Eric Berthoumieux Yann Bedfer Denis Calvet Nicole d'Hose Alain Delbart Maria Diakaki Esther Ferrer-Ribas Andrea Ferrero Fabienne Kunne Damien Neyret Thomas Papaevangelou Franck Sabatie Maxence Vanderbroucke AnDi Tan Wick Haxton Yuan Mei Chinorat Kobdaj Yu-Peng Yan NPAC and Department of Physics and Astronomy Shanghai Jiao Tong University Shanghai Laboratory for Particle Physics and Cosmology Shanghai 200240 China College of Physical Science and Technology Central China Normal University Wuhan 430079 China China Institute of Atomic Energy Beijing 102413 China School of Physics Peking University Beijing 100871 China School of Physics and Key Laboratory of Particle Physics and Particle Irradiation (MOE) Shandong University Jinan 250100 China School of Physics and Engineering Sun Yat-Sen University Guangzhou 510275 China Department of Modern Physics University of Science and Technology of China Hefei 230026 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei 230026 China University ofZaragoza C/P Cerbuna 12 50009 Zaragoza Spain IRfu CEA Universite Paris-Saclay F-91191 Gif-sur-Yvette France Department of Physics University of Maryland College Park MD 20742 USA Nuclear Science Division Lawrence Berkeley National Laboratory Berkeley CA 94720 USA Center for Excellence in High Energy Physics and Astrophysics Suranaree University of Technology Nakhon Ratchasima 30000 Thailand

Searching for the neutrinoless double beta decay(NLDBD)is now regarded as the topmost promising technique to explore the nature of neutrinos after the discovery of neutrino masses in oscillation *** X-III(particle and astrophysical xenon experiment III)will search for the NLDBD of136Xe at the China jin Ping Underground Laboratory(CJPL).In the first phase of the experiment,a high pressure gas Time Projection Chamber(TPC)will contain 200 kg,90%136Xe enriched gas operated at10 *** pitch micro-pattern gas detector(Microbulk Micromegas)will be used at both ends of the TPC for the charge readout with a cathode in the *** signals can be used to reconstruct the electron tracks of the NLDBD events and provide good energy and spatial *** detector will be immersed in a large water tank to ensure～5 m of water shielding in all *** second phase,a ton-scale experiment,will consist of five TPCs in the same water tank,with improved energy resolution and better control over backgrounds.

关键词： neutrinoless double beta decay lepton number violation underground experiment TPC Micromegas

Quantum computational advantage via 60-qubit 24-cycle random circuit sampling

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Science Bulletin 2022年第3期67卷 240-245页

作者： Qingling Zhua Sirui Cao fusheng Chen Ming-cheng Chen Xiawei Chen Tung-Hsun chung Hui Deng Yajie Du Daojin Fan Ming Gong cheng Guo chu Guo Shaojun Guo lianchen Han linyin Hong He-liang Huang yong-Heng Huo liping li Na li Shaowei li Yuan li futian liang chun lin jin lin haoran Qian Dan Qiao hao Rong Hong Su lihua Sun liangyuan Wang Shiyu Wang Dachao Wu Yulin Wu Yu Xu Kai Yan Weifeng Yang Yang Yang Yangsen Ye Jianghan Yin Chong Ying Jiale Yu Chen Zha Cha zhang Haibin zhang Kaili zhang Yiming zhang Han zhao Youwei zhao liang zhou Chao-Yang Lu cheng-Zhi Peng Xiaobo Zhu Jian-Wei Pan Hefei National Laboratory for Physical Sciences at the Microscale and Department of Modern Physics University of Science and Technology of ChinaHefei 230026China Shanghai Branch CAS Center for Excellence in Quantum Information and Quantum PhysicsUniversity of Science and Technology of ChinaShanghai 201315China Shanghai Research Center for Quantum Sciences Shanghai 201315China QuantumCTek Co. Ltd.Hefei 230026China Henan Key Laboratory of Quantum Information and Cryptography Zhengzhou 450000China Shanghai Institute of Technical Physics Chinese Academy of SciencesShanghai 200083China

To ensure a long-term quantum computational advantage,the quantum hardware should be upgraded to withstand the competition of continuously improved classical algorithms and ***,we demonstrate a superconducting quantum computing systems Zuchongzhi 2.1,which has 66 qubits in a two-dimensional array in a tunable coupler *** readout fidelity of Zuchongzhi 2.1 is considerably improved to an average of 97.74%.The more powerful quantum processor enables us to achieve larger-scale random quantum circuit sampling,with a system scale of up to 60 qubits and 24 cycles,and fidelity of FXEB=(3·66±0·345)×10^(-4).The achieved sampling task is about 6 orders of magnitude more difficult than that of Sycamore[Nature 574,505(2019)]in the classic simulation,and 3 orders of magnitude more difficult than the sampling task on Zuchongzhi 2.0[arXiv:2106.14734(2021)].The time consumption of classically simulating random circuit sampling experiment using state-of-the-art classical algorithm and supercomputer is extended to tens of thousands of years(about 4·8×104years),while Zuchongzhi 2.1 only takes about 4.2 h,thereby significantly enhancing the quantum computational advantage.

关键词： Quantum physics Quantum computation Quantum information Superconducting quantum computing Superconducting qubit