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The Giant Radio Array for Neutrino Detection(GRAND):Science and design

Science China(Physics,Mechanics & Astronomy) 2020年第1期Mechanics & Astronomy) .卷 5-47页

作者： Jaime álvarez-Mu?iz Rafael Alves Batista Aswathi Balagopal V. Julien Bolmont Mauricio Bustamante Washington Carvalho Jr. Didier Charrier Isma?l Cognard Valentin Decoene Peter B.Denton Sijbrand De Jong Krijn D.De Vries Ralph Engel Ke Fang Chad Finley Stefano Gabici Quan Bu Gou Jun Hua Gu Claire Guépin Hong Bo Hu Yan Huang Kumiko Kotera Sandra Le Coz Jean-Philippe Lenain Guo Liang Léü Olivier Martineau-Huynh Miguel Mostafá Fabrice Mottez Kohta Murase Valentin Niess Foteini Oikonomou Tanguy Pierog Xiang Li Qian Bo Qin Duan Ran Nicolas Renault-Tinacci Markus Roth Frank G.Schr ?der Fabian Schüssler Cyril Tasse Charles Timmerman Matías Tueros Xiang Ping Wu Philippe Zarka Andreas Zech B.Theodore Zhang Jian Li Zhang Yi Zhang Qian Zheng Anne Zilles Departamento de Física de Partículas & Instituto Galego de Física de Altas Enerxías Universidad de Santiago de Compostela Instituto de Astronomia Geofísica e Ciências Atmosféricas Universidade de S?o Paulo Department of Physics—Astrophysics University of Oxford DWB Institute of Experimental Particle Physics (ETP) Karlsruhe Institute of Technology (KIT) Laboratoire de Physique Nucléeaire et de Hautes Energies (LPNHE) Sorbonne Université Université Paris Diderot Sorbonne Paris Cité Niels Bohr International Academy and DARK Niels Bohr Institute Discovery Center Niels Bohr Institute Center for Cosmology and Astro Particle Physics (CCAPP) & Department of Physics Ohio State University Universidade de Santiago de Compostela SUBATECH Institut Mines-Telecom Atlantique – CNRS/IN2P3 – Université de Nantes Laboratoire de Physique et Chimie de l’Environnement et de l’Espace LPC2E CNRS-Université d’Orléans Station de Radioastronomie de Nan?cay Observatoire de Paris Sorbonne Université UMR 7095 Institut d’Astrophysique de Paris Institute for Mathematics Astrophysics and Particle Physics (IMAPP) Radboud Universiteit Nationaal Instituut voor Kernfysica en Hoge Energie Fysica (NIKHEF) IIHE/ELEM Vrije Universiteit Brussel Institute for Nuclear Physics (IKP) Karlsruhe Institute of Technology (KIT) Einstein Fellow Stanford University Department of Astronomy University of Maryland Joint Space-Science Institute Oskar Klein Centre Stockholm University Department of Physics Stockholm University Astro Particule et Cosmologie (APC) Université Paris Diderot CNRS/IN2P3 CEA/Irfu Observatoire de Paris Institute of High Energy Physics Chinese Academy of Sciences national astronomical observatories Chinese Academy of Sciences School of Physical Science and Technology Xinjiang University Center for Particle and Gravitational Astrophysics Pennsylvania State University Department of Physics Pennsylvania State University Department of Astronomy & Astrophysics Pennsylvania State University LUTH Observatoire de Paris

The Giant Radio Array for Neutrino Detection（GRAND） is a planned large-scale observatory of ultra-high-energy（UHE） cosmic particles, with energies exceeding 10～8 Ge V. Its goal is to solve the long-standing mystery of the origin of UHE cosmic rays. To do this, GRAND will detect an unprecedented number of UHE cosmic rays and search for the undiscovered UHE neutrinos and gamma rays associated to them with unmatched sensitivity. GRAND will use large arrays of antennas to detect the radio emission coming from extensive air showers initiated by UHE particles in the atmosphere. Its design is modular: 20 separate, independent sub-arrays, each of 10000 radio antennas deployed over 10000 km2. A staged construction plan will validate key detection techniques while achieving important science goals early. Here we present the science goals, detection strategy, preliminary design, performance goals, and construction plans for GRAND.

关键词： radio telescopes neutrinos in astronomical observations cosmic rays in astronomical observations radiowave radiation: sources galactic and extragalactic cosmic rays

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Negative Parity States in ^(39)Cl Configured by Crossing Major Shell Orbits

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Chinese Physics Letters 2019年第6期36卷 17-20页

作者： Long-Chun Tao Cen-Xi Yuan Jian-Ling Lou Xiao-Fei Yan Yan-Lin Ye School of Physics and State Key Laboratory of Nuclear Physics and Technology Peking University RIKEN Nishina Center Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Department of Physics University of Tsukuba Department of Physics Kyungpook National University Department of Physics Osaka University Department of Physics Tokyo Institute of Technology Department of Advanced Sciences Hosei University Department of Physics Meiji University

Traditional "magic numbers" were once regarded as immutable throughout the nuclear chart. However, unexpected changes were found for unstable nuclei around N = 20. With both proton and neutron numbers around the magic number of 20, the neutron-rich ^(39)Cl isotope provides a good test case for the study of the quantumstate evolution across the major shell. In the present work, the negative parity states in ^(39)Cl are investigated through the β decay spectroscopy of 39 S. Newly observed γ transitions together with a new state are assigned into the level scheme of ^(39)Cl. The spin parity of 5/2^- for the lowest negative parity state in ^(39)Cl is reconfirmed using the combined γ transition information. These systematic observations of the negative parity states in ^(39)Cl allow a comprehensive comparison with the theoretical descriptions. The lowest 5/2^- state in ^(39)Cl remains exotic in terms of comparisons with existing theoretical calculations and with the neighboring isotopes having similar single-particle configurations. Further experimental and theoretical investigations are suggested.

关键词： Negative Parity States Crossing Major Shell Orbits immutable throughout

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The Giant Radio Array for Neutrino Detection(GRAND):Science and design

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Science China(Physics,Mechanics & Astronomy) 2020年第1期63卷 1-43页

作者： Jaime Alvarez-Muniz Rafael Alves Batista Aswathi Balagopal V. Julien Bolmont Mauricio Bustamante Washington Carvalho Jr. Didier Charrier Ismael Cognard Valentin Decoene Peter B.Denton Sijbrand De Jong Krijn D.De Vries Ralph Engel Ke Fang Chad Finley Stefano Gabici Quan Bu Gou Jun Hua Gu Claire Guépin Hong Bo Hu Yan Huang Kumiko Kotera Sandra Le Coz Jean-Philippe Lenain Guo Liang Léü Olivier Martineau-Huynh Miguel Mostafá Fabrice Mottez Kohta Murase Valentin Niess Foteini Oikonomou Tanguy Pierog Xiang Li Qian Bo Qin Duan Ran Nicolas Renault-Tinacci Markus Roth Frank G.Schroder Fabian Schüssler Cyril Tasse Charles Timmerman Matías Tueros Xiang Ping Wu Philippe Zarka Andreas Zech B.Theodore Zhang Jian Li Zhang Yi Zhang Qian Zheng Anne Zilles Departamento de Fisica de Particulas&lnstituto Galego de Fisica de Altas Enerxias Universidad de Santiago de CompostelaSantiago de Compostela 15782Spain Instituto de Astronomia Geofisica e Ciencias AtmosfericasUniversidade de Sao PauloSao Paulo-SP 05508-090Brazil Department of Physics-Astrophysics University of OxfordDWBOxford 0X13RHUK Institute of Experimental Particle Physics(ETP) Karlsruhe Institute of Technology(KIT)Karlsru he D-76021Germany Laboratoire de Physique Nucleeaire et de Hautes Energies(LPNHE) Sorbonne UniversiteUniversite Paris DiderotSorbonne Paris CiteCNRS place Jussieu F-75252Paris Cedex 5France Niels Bohr International Academy and DARK Niels Bohr InstituteCopenhagen 2100Denmark Discovery Center Niels Bohr InstituteCopenhagen 2100Denmark Center for Cosmology and AstroParticle Physics(CCA.PP)&Department of Physics Ohio State UniversityColumbus OH 43210USA Universidade de Santiago de Compostela Santiago de Compostela 15782Spain 0SUBATECH Institut Mines-Telecom Atlantique-CNRS/IN2P3-Universite de NantesNantes 44300France Laboratoire de Physique et Chimie de KEnvironnement et de VEspace LPC2E CNRS-Universite d'Orleans Orleans F-45071France Station de Radioastronomie de Nancay Observatoire de ParisCNRS/INSU F-18330 NangayFrance Sorbonne Universite UMR 7095Institut d'Astrophysique de Paris98 bis bd AragoParis 75014France Institute for Mathematics Astrophysics and Particle Physics(IMAPP)Radboud UniversiteitNijmegen 6500Netherlands Nationaal Instituut voor Kemfysica en Hoge Energie Fysica(NIKHEF) Amsterdam NL-1009Netherlands IIHE/ELEM Vrije Universiteit BrusselPleinlaan 2Brussels 1050Belgium Institute for Nuclear Physics(IKP) Karlsruhe Institute of Technology(KIT)Karlsruhe D-76021Germany Einstein Fellow Stanford UniversityStanford CA 94305USA Department of Astronomy University of MarylandCollege Park MD 20742-2421USA Joint Space-Science Institute College Park MD 20742-2421USA Oskar Klein Centre Stockholm UniversityStockholm SE-10691Sweden Department of Phy

The Giant Radio Array for Neutrino Detection(GRAND)is a planned large-scale observatory of ultra-high-energy(UHE)cosmic particles,with energies exceeding 10~8 Ge *** goal is to solve the long-standing mystery of the origin of UHE cosmic *** do this,GRAND will detect an unprecedented number of UHE cosmic rays and search for the undiscovered UHE neutrinos and gamma rays associated to them with unmatched *** will use large arrays of antennas to detect the radio emission coming from extensive air showers initiated by UHE particles in the *** design is modular:20 separate,independent sub-arrays,each of 10000 radio antennas deployed over 10000 km^2.A staged construction plan will validate key detection techniques while achieving important science goals *** we present the science goals,detection strategy,preliminary design,performance goals,and construction plans for GRAND.

关键词： radio telescopes neutrinos in astronomical observations cosmic rays in astronomical observations radiowave radiation:sources galactic and extragalactic cosmic rays:galactic and extragalactic

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Forecast of Observing Time Delay of Strongly Lensed Quasars with the Muztagh-Ata 1.93m Telescope

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Research in Astronomy and Astrophysics 2023年第3期23卷 1-15页

作者： Shanhao Zhu Yiping Shu Haibo Yuan Jian-Ning Fu Jian Gao Jianghua Wu Xiangtao He Kai Liao Guoliang Li Xinzhong Er Bin Hu Institute for Frontier in Astronomy and Astrophysics Beijing Normal UniversityBejing 102206China Department of Astronomy Beijing Normal UniversityBeijing 100875China Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str.1D-85748 GarchingGermany Ruhr University Bochum Faculty of Physics and AstronomyAstronomical Institute(AIRUB)German Centre for Cosmological LensingD-44780 Bochum German School of Physics and Technology Wuhan UniversityWuhan 430072China Purple Mountain Observatory Chinese Academy of SciencesNanjing 210023.China South-Western Institute for Astronomy Research Yunnan UniversityKunming 650500China

As a completely independent method,the measurement of time delay of strongly lensed quasars(TDSL)are crucial to resolve the Hubble *** monitoring is required but so far limited to a small sample of strongly lensed *** with several partner institutes,Beijing Normal University is constructing a 1.93 m reflector telescope at the Muztagh-Ata site in west China,which has the world class observing conditions with median seeing of 082 and median sky brightness of 21.74 mag arcsec-2 in V-band during the dark *** telescope will be equipped with both a three-channel imager/photometer which covers 3500–11,000?wavelength band,and a low-medium resolution(λ/δλ=500/2000/7500)*** this paper,we investigate the capability of the Muztagh-Ata 1.93 m telescope in measuring time delays of strongly lensed *** generate mock strongly lensed quasar systems and light curves with microlensing effects based on five known strongly lensed quasars,i.e.,RX J1131-1231,HE 0435-1223,PG 1115+080,WFI 2033-4723 and SDSS 1206+*** particular,RX J1131-1231 is generated based on the lens modeling results of Suyu et *** to the lack of enough information,the other four systems are calculated by a simple analytical *** to simulations,for RX J1131-like systems(wide variation in time delay between images)the TDSL measurement can be achieved with the precision aboutΔt=0.5 day with four seasons campaign length and 1 day *** accuracy is comparable to the up-coming TDCOSMO *** it would be better when the campaign length keeps longer and with high *** a result,the capability of the Muztagh-Ata 1.93 m telescope allows it to join the network of TDSL *** will enrich the database for strongly lensed quasar observations and make more precise measurements of time delays,especially considering the unique coordinate of the site.

关键词： equipped Together precise

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A giant central red disk galaxy at redshift z=0.76:Challenge to theories of galaxy formation

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Science China(Physics,Mechanics & Astronomy) 2021年第7期64卷 137-141页

作者： Kun Xu ChengZe Liu YiPeng Jing Marcin Sawicki Stephen Gwyn Department of Astronomy School of Physics and AstronomyShanghai Jiao Tong UniversityShanghai200240China Tsung-Dao Lee Institute Shanghai Key Laboratory for Particle Physics and CosmologyShanghai Jiao Tong UniversityShanghai200240China Canada Research Chair Department of Astronomy&Physics and the Institute for Computational AstrophysicsSaint Mary’s UniversityHalifaxB3H 3C3Canada NRC-Herzberg Astronomy and Astrophysics National Research Council of CanadaVictoriaV9E 2E7Canada

We report a giant red central disk galaxy in the XMM-LSS north region. The region is covered with a rich variety of multi-band photometric and spectroscopic observations. Using the photometric data of the Canada-France-Hawaii Telescope Legacy Survey(CFHTLS) and spectroscopic observation of the baryon oscillation spectroscopic survey(BOSS), we find that the galaxy has a stellar mass of ~1011.6 M⊙. The galaxy has a red color and has an old stellar population, and thus its star formation has *** the photometric image data of the Hyper Suprime-Cam(HSC) Subaru Strategic Program, we demonstrate that its luminosity profile is perfectly described by a Sérsic form with n=1.22 consistent with that of a disk. We also analyze its environment based on the VIMOS Public Extragalactic Redshift Survey(VIPERS) photometric catalog, and find that its close neighbors are all less massive, indicating that our observed galaxy is sitting at the center of its dark matter host halo. Existence of such a giant red central disk galaxy seriously challenges the current standard paradigm of galaxy formation, as there is no known physical mechanism to explain the quenching of its star formation. This conclusion is supported by state-of-the-art hydrodynamical simulations of galaxy formation.

关键词： disk galaxies galaxy quenching massive galaxies

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Erratum to:Forecasts on CMB lensing observations with AliCPT-1

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中国科学:物理学、力学、天文学英文版 2023年第9期66卷 200-200页

作者： Jinyi Liu Zeyang Sun Jiakang Han Julien Carron Jacques Delabrouille Siyu Li Yang Liu Jing Jin Shamik Ghosh Bin Yue Pengjie Zhang Chang Feng Zhi-Qi Huang Hao Liu Yi-Wen Wu Le Zhang Zi-Rui Zhang Wen Zhao Bin Hu Hong Li Xinmin Zhang Department of Astronomy Beijing Normal UniversityBeijing 100875China Department of Astronomy School of Physics and AstronomyShanghai Jiao Tong UniversityShanghai200240China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240China Division of Astronomy and Astrophysics Tsung-Dao Lee InstituteShanghai Jiao Tong UniversityShanghai200240China D´epartement de Physique Th´eorique et CAP Universit´e de Gen`eveGen`eve CH-1211Switzerland CNRS-UCB International Research Laboratory Centre Pierre Bin´etruyCPB-IN2P3Berkeley IRL2007USA Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China CAS Key Laboratory for Researches in Galaxies and Cosmology Department of AstronomyUniversity of Science and Technology of ChinaChinese Academy of SciencesHefei 230026China School of Astronomy and Space Science University of Science and Technology of ChinaHefei 230026China national astronomical observatories Chinese Academy of SciencesBeijing100101China School of Physics and optoelectronics engineering Anhui UniversityHefei 230039China School of Physics and Astronomy Sun Yat-sen UniversityZhuhai519082China CSST Science Center for the Guangdong-Hong Kong-Macao Greater Bay Area Zhuhai 519082China Peng Cheng Laboratory Shenzhen 518000China Theoretical devision Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China

One of the authors regrets that there was an omission of affiliation in this published article[1].The affiliation information of author Yi-WenWu only included the institution name for the author,and it is advised to a... 详细信息

关键词： observations CPT CMB

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ROSAT巡天X射线选活动星系核的光学证认

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天文学进展 2012年第1期30卷 106-124页

作者：孙艳春白宇何香涛陈阳吴江华李庆康 Green Richard F. Voges Wolfgang 北京师范大学天文系北京100875 中国科学院国家天文台北京100012 NOAO Kitt Peak national Observatory USA Tucson AZ85726-6732 Max-Planck-Institute fur Extrater-restrische Physik Germany D85740Garching

获得完备的样本一直是类星体统计分析工作中至关重要的第一步。类星体巡天选择候选体的方法主要有射电波段筛选、色指数筛选、无缝光谱筛选、X射线波段筛选、对红外源或变源进行筛选和零自行的方法。单独运用任一方法都有选择效应,采用... 详细信息

获得完备的样本一直是类星体统计分析工作中至关重要的第一步。类星体巡天选择候选体的方法主要有射电波段筛选、色指数筛选、无缝光谱筛选、X射线波段筛选、对红外源或变源进行筛选和零自行的方法。单独运用任一方法都有选择效应,采用多波段方法可以极大地提高样本的完备性。阐述了使用多波段方法选择活动星系核样本的研究现状,提出多波段类星体巡天方法和选源判据,给出ROSAT巡天中F.1002,***,F.836和*** 4个天区以及空源的15年来X射线选活动星系核的选源和光学新证认的AGN结果,表明多波段类星体巡天方法能有效地提高观测效率。

关键词：活动星系核 X射线光学证认

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FAST 19波束脉冲星漂移扫描巡天模拟

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天文学进展 2018年第2期36卷 173-188页

作者：刘鹏王培李菂张洁张蕾张承民朱炜炜岳友岭代实西华师范大学物理与空间科学学院南充637009 中国科学院国家天文台北京100012 中国科学院FAST重点实验室北京100012 CSIRO Astronomy and Space Science Australia Telescope National FacilityBox 76 Epping NSW 1710Australia

脉冲星搜索是500 m口径球面射电望远镜(Five-hundred-meter Aperture Spherical Radio Telescope,FAST)的主要科学目标之一。针对FAST设备性能,模拟FAST脉冲星巡天,优化巡天方案,对即将开展的FAST脉冲星巡天项目具有重要的实用价值。基... 详细信息

脉冲星搜索是500 m口径球面射电望远镜(Five-hundred-meter Aperture Spherical Radio Telescope,FAST)的主要科学目标之一。针对FAST设备性能,模拟FAST脉冲星巡天,优化巡天方案,对即将开展的FAST脉冲星巡天项目具有重要的实用价值。基于Parkes多波束巡天、Parkes中纬度巡天和Parkes高纬度巡天的结果,利用脉冲星分布模拟软件包PsrPopPy,模拟得到了银河系中正常脉冲星和毫秒脉冲星的空间分布样本,并根据FAST设备参数进行了虚拟观测。结果表明,使用FAST 19波束接收机漂移扫描观测模式,在中心频率为1250MHz,带宽为400 MHz,每波束扫描时间为13.5 s,有效积分时间为6.0 s的情况下,在赤纬为-14~?12′～65~?48′天区内,可发现1600颗正常脉冲星和238颗毫秒脉冲星。为获得银河系中脉冲星自旋演化的样本,使用evolve代码进行了再次模拟。设置相同的观测参数的情况下,在全天范围内模拟探测到孤立正常脉冲星1749颗,并得到其在P-P图上的分布。

关键词： FAST 脉冲星脉冲星模拟脉冲星巡天模拟

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相干消色散脉冲星观测系统的研究

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天文研究与技术 2015年第4期12卷 480-486页

作者：徐永华李纪云张颖倩罗近涛李志玄郝龙飞汪敏中国科学院云南天文台云南昆明650011 中国科学院天体结构与演化重点实验室云南昆明650011 中国科学院上海天文台上海200030 national Radio Astronomy Observatory

云南天文台射电天文研究团组利用从美国伯克利大学CASPER天文信号与电子学研究中心购买的现场可编程门阵列(Field-Programmable Gate Array,FPGA)接收机平台ROACH2,实现了512 MHz输入带宽,512 MHz带宽分为128通道输出(每个通道4 M带宽),... 详细信息

云南天文台射电天文研究团组利用从美国伯克利大学CASPER天文信号与电子学研究中心购买的现场可编程门阵列(Field-Programmable Gate Array,FPGA)接收机平台ROACH2,实现了512 MHz输入带宽,512 MHz带宽分为128通道输出(每个通道4 M带宽),8比特采样和双极化输入(1 024 MHz)的基带数据采集终端。海量数据传输方式通过SFP+万兆网口实现,利用编写的脚本文件调用DSPSR程序包实现数据的解码、相干消色散、偏振计算和折叠等处理。数据处理结果以PSRFITS格式存储。构建以ROACH2为基带数据采集终端和DSPSR为数据处理核心的脉冲星观测系统,相比于以VLBI观测终端为基础构建的观测系统,在观测模式、数据处理方法、运算效率和观测数据的通用性等方面具有更好的优越性。

关键词：射电天文脉冲星PSR J0835-4510 脉冲星PSR J0332+5434 40m射电望远镜 ROACH2 DSPSR 相干消色散

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