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The Two Mini-lobes of the CSO OQ2.8——VLBI Observations at 5 GHz and 8.4 GHz

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Chinese Journal of Astronomy and Astrophysics 2003年第6期3卷 505-512页

作者： wei-hua Wang, {2.-{3. hong and tao anshanghai astronomical observatory, Chinese Academy of sciences, shanghai 2.003. National astronomical Observatories, Chinese Academy of sciences, Beijing 100012 shanghai astronomical {2. Chinese Academy of Sciences Shanghai 200030 []National Astronomical Observatories Chinese Academy of Sciences Beijing 100012

We present the results of VLBI observations at 5 GHz and 8.4 GHz of the compact symmetric object (CSO) OQ2.8. Images taken on four epochs at 5GHz and one at 8.4GHz show that the parsec radio structure of the source consists of two mini-lobes, both of them are resolved into two hot-spots. We note that the component D is stronger than the component C in the south-west region at 5 GHz, indicating that component D is less free-free absorbed than C at low frequency. On the basis of the separation of components A and D, a proper motion of 0.03.0}0.02.mas yrbetween the two mini-lobes is estimated. This value is about half the previous estimates based on the separation of components A and C with 8.4 GHz VLBI data. The reason for the decrease in the expansion velocity is discussed.

关键词： galaxies: individual (Mkn 668 OQ2.8) - galaxies: active

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-{3. An Ke Gong Jin-yuan Liao Yan-Qiu Zhang yue {3.ng 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-{3. Liang Ya-Qing Liu Da-Li Zhang Xi-Lei Sun Fan Zhang Gang Chen {3.n-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 {3.ng 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 S{3.ng-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 2.2. 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

Bending of Jets in the QSO NRAO 53.

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Chinese Journal of Astronomy and Astrophysics 2008年第2期8卷 179-194页

作者： xiao-yu {2. C{3.n-Hao Sun Jun-Hui Zhao Dong-Rong Jiang Zhi-Qiang Shen tao an wei-{3. Wang Jun Yang shanghai astronomical {2. Chinese Academy of Sciences Shanghai 200030 Graduate University of Chinese Academy of sciences Beijing 100049 Harvard-Smithsonlan Center for Astroplaysics 60 Garden street MS 72 Cambridge MA02138 Joint Institute for Galaxy and Cosmology

We present radio images of NRAO 53. on scales ranging from pc to kpc. The observations include the EVN at 5 GHz, the VLBA at 1.6, 8.6 and 15 GHz, the MERLIN at 1.6 and 5 GHz, and the VLA at 5, 8.4, 15, 2., and 43.GHz. The VLBI images show a core-jet structure with an oscillating trajectory on a scale of about 3. mas north of the strongest compact component （core）. Superluminal motions are detected in five of the jet components with apparent velocities in the range of 13.6 to 2..2.. A new component is detected at 15 GHz with the VLBA observations, which appears to be associated with the outburst in 2.02. Significant polarized emission is detected around the core with the VLBA observations at 15 GHz. Rapid variations of the polarization intensity and angle are found between the epochs in 2.02.and 2.04. On the kpc-scale, a distant component （labelled as WL） located 11 arcsec west （PA=-86°） of the core is detected beyond the core-jet structure which extended to several hundreds of mas in the north-west direction （-50°）. A significant emission between the core-jet structure and the WL is revealed. A clump of diffuse emission （labelled EL, 12.arcsec long） at PA 70° to the core, is also detected in the VLA observations, suggesting the presence of double lobes in the source. The core component shows a fiat spectrum, while the distant components WL and EL have steep spectra. The steep spectra of the distant components and the detection of the arched emission suggest that the distant components are lobes or hot-spots powered by the core of NRAO 53.. The morphologies from pc- to kpcscales and the bending of jets are investigated. The observed radio morphology from pc to kcp appears to favor the model in which precession or wobbling of the nuclear disk drives the helical motion of the radio plasma and produces the S-shaped structure on kpc scale.

关键词： galaxies: nuclei -- galaxies: jets -- quasars: individual: NRAO 53.

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 {3.e Wu Yan Cai Shu-{3.n Cao Zi-huang Cao Jeffrey L.Carlin Hai-{3.an 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 {3.an Liang Chien-Cheng Lin Chao Liu Gen-Rong Liu Guan-Qun Liu Zhi-Gang Liu Wen-Zhi Lu {3. 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 {23. {3.an 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 {3.e-Fei Wang You-Fen Wang Peng wei Ming-Zhi wei hong Wu Ke-Fei Wu Xue-Bing Wu {3.-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 {3. Hui {3.an Hai-Bo {3.an Hai-Long {3.an wei-Min {3.an 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 {2. 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 2.11 and ended in June 2.12. and the data have been released to the public as the LAMOST Pilot Data Release in August 2.12. The regular survey started in September 2.12. and completed its first year of operation in June 2.13. The LAMOST DR1 includes a total of 12.2.plates containing 2.955 3.6 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 2.2.4 696 spectra, of which 1 944 3.0} 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（12. 52. 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

Data processing and data products from 2.17 to 2.19 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 {3.an 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 {3. Liu Chong Pei Zhi-Xia Shen {3.n-Ying Jiang Jian-Feng Tian Xian-Qun Zeng Zhi-Gang Hou Xu Yang Jun-Bo Zhang Shi-Long Liao Dong-wei Fan {3.n-Fei Xu Jian-Ping Xiong Tai-Sheng Yan Xi Zhang Chang-hua Li Yi-Han tao Si-Cheng {3. Zhi-Song Cao hong-Shuai Wang National astronomical Observatories Chinese Academy of SciencesBeijing 100101China University of Chinese Academy of sciences Beijing 100049China shanghai astronomical {2. 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 2.17 March 10 to 2.19 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 {3.e 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 {3.an 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 {13. Liang-Ping Tu Da-Qing Wang Dan Wang Jian-Ping Wang Lei Wang Shou-Guan Wang Shu-Qing Wang Ya-Nan Wang You Wang {3.e-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 {3. Hui {3.an 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 {2. 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 3.9 000 spectra and a catalog of these objects.

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

Feasibility and physics potential of detecting ^(8)B solar neutrinos at JUNO

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Chinese Physics C 2021年第2期45卷 93-110页

作者： Angel Abusleme Thomas Adam Shakeel Ahmad Sebastiano Aiello Muhammad Akram Nawab Ali Fengpeng An Guangpeng An Qi An Giuseppe Andronico Nikolay Anfimov Vito Antonelli Tatiana Antoshkina Burin Asavapibhop João Pedro Athayde Marcondes de André Didier Auguste Andrej Babic Wander Baldini Andrea Barresi Eric Baussan Marco Bellato Antonio Bergnoli Enrico Bernieri David Biare Thilo Birkenfeld Sylvie Blin David Blum Simon Blyth Anastasia Bolshakova Mathieu Bongrand Clément Bordereau Dominique Breton Augusto Brigatti Riccardo Brugnera Riccardo Bruno Antonio Budano Max Buesken Mario Buscemi Jose Busto Ilya Butorov Anatael Cabrera Hao Cai xiao Cai Yanke Cai Zhiyan Cai Antonio Cammi Agustin Campeny Chuanya Cao Guofu Cao Jun Cao Rossella Caruso Cédric Cerna Jinfan Chang {2.n Chang Pingping Chen Po-An Chen Shaomin Chen Shenjian Chen Xurong Chen Yi-Wen Chen Yixue Chen {2. Chen Zhang Chen Jie Cheng Yaping Cheng Alexander Chepurnov Davide Chiesa Pietro Chimenti Artem Chukanov Anna Chuvashova Gérard Claverie Catia Clementi Barbara Clerbaux Selma Conforti Di Lorenzo Daniele Corti Salvatore Costa Flavio Dal Corso Christophe De La Taille Jiawei Deng Zhi Deng Ziyan Deng Wilfried Depnering Marco Diaz Xuefeng Ding Ya{2.n Ding Ba{2. Dirgantara Sergey Dmitrievsky Tadeas Dohnal Georgy Donchenko Jianmeng Dong Damien Dornic Evgeny Doroshkevich Marcos Dracos Frédéric Druillole Shuxian Du Stefano Dusini Martin Dvorak Timo Enqvist Heike Enzmann Andrea Fabbri Lukas Fajt Donghua Fan Lei Fan Can Fang Jian Fang Marco Fargetta Anna Fatkina Dmitry Fedoseev Vladko Fekete Li-Cheng Feng Qichun Feng Richard Ford Andrey Formozov Amélie Fournier Haonan Gan Feng Gao Alberto Garfagnini Alexandre Göttel Christoph Genster Marco Giammarchi Agnese Giaz Nunzio Giudice Franco Giuliani Maxim Gonchar Guanghua Gong Hui Gong Oleg Gorchakov {2.ri Gornushkin Marco Grassi Christian Grewing Maxim Gromov Vasily Gromov Minghao Gu xiaofei Gu {2. Gu Meng{2.n Guan Nunzio Guardone Maria Gul Cong Guo Jing{2.an Guo Wanlei Guo Xinheng Guo {2.hang Guo Paul Hackspacher Caren Hagner Ran Han Yan Yerevan Physics Institute YerevanArmenia UniversitéLibre de Bruxelles BrusselsBelgium Universidade Estadual de Londrina LondrinaBrazil Pontificia Universidade Catolica do Rio de Janeiro RioBrazil Pontificia Universidad Católica de Chile SantiagoChile Universidad Tecnica Federico Santa Maria ValparaisoChile Beijing Institute of Spacecraft Environment Engineering BeijingChina Beijing Normal University BeijingChina China Institute of Atomic Energy BeijingChina Institute of High Energy Physics BeijingChina North China Electric Power University BeijingChina School of Physics Peking UniversityBeijingChina Tsinghua University BeijingChina University of Chinese Academy of sciences BeijingChina Jilin University ChangchunChina College of Electronic Science and Engineering National University of Defense TechnologyChangshaChina Chongqing University ChongqingChina Dongguan University of Technology DongguanChina Jinan University GuangzhouChina Sun Yat-Sen University GuangzhouChina Harbin Institute of Technology HarbinChina University of Science and Technology of China HefeiChina The Radiochemistry and Nuclear Chemistry Group in University of South China HengyangChina Wuyi University JiangmenChina Shandong University JinanChina Institute of Modern Physics Chinese Academy of SciencesLanzhouChina Nanjing University NanjingChina Guangxi University NanningChina East China University of Science and Technology ShanghaiChina School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghaiChina Tsung-Dao Lee Institute Shanghai Jiao Tong UniversityShanghaiChina Institute of Hydrogeology and Environmental Geology Chinese Academy of Geological SciencesShijiazhuangChina Nankai University TianjinChina Wuhan University WuhanChina Xi’an Jiaotong University Xi’anChina Xiamen University XiamenChina School of Physics and Microelectronics Zhengzhou UniversityZhengzhouChina Institute of Physics National Chiao-Tung University Hsinchu National United University Miao-Li Department of Physics National T

The Jiangmen Underground Neutrino observatory(JUNO)features a 2. kt multi-purpose underground liquid scintillator sphere as its main *** of JUNO's features make it an excellent location for^8B solar neutrino measurements,such as its low-energy threshold,high energy resolution compared with water Cherenkov detectors,and much larger target mass compared with previous liquid scintillator *** this paper,we present a comprehensive assessment of JUNO's potential for detecting^8B solar neutrinos via the neutrino-electron elastic scattering process.A reduced 2.MeV threshold for the recoil electron energy is found to be achievable,assuming that the intrinsic radioactive background^(2.8)U and^(2.2.Th in the liquid scintillator can be controlled to 10^(-17)g/*** ten years of data acquisition,approximately 60,000 signal and 3.,000 background events are *** large sample will enable an examination of the distortion of the recoil electron spectrum that is dominated by the neutrino flavor transformation in the dense solar matter,which will shed new light on the inconsistency between the measured electron spectra and the predictions of the standard three-flavor neutrino oscillation *** m^(2._(2.)=4.8times10^(-5);(7.5times10^(-5))eV^(2.,JUNO can provide evidence of neutrino oscillation in the Earth at approximately the 3.igma(2.igma)level by measuring the non-zero signal rate variation with respect to the solar zenith ***,JUNO can simultaneously measureDelta m^2.(2.)using^8B solar neutrinos to a precision of 2.% or better,depending on the central value,and to sub-percent precision using reactor antineutrinos.A comparison of these two measurements from the same detector will help understand the current mild inconsistency between the value of Delta m^2.(2.)reported by solar neutrino experiments and the KamLAND experiment.

关键词： neutrino oscillation solar neutrino JUNO

国家重点研发计划“SKA前期数据处理系统建设和相关科学预研”简介

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天文学进展 2018年第3期36卷 348-352页

作者：洪晓瑜武向平安涛叶叔华毛羽丰黄滟伍筱聪吕唯佳李亭李惠华吴芳中国科学院上海天文台上海200030 中国科学院国家天文台北京100101 中国科学院前沿科学与教育局北京100864

在继承平方公里阵列(Square Kilometre Array,SKA)望远镜的中国低频探路者——"宇宙第一缕曙光"探测项目2.CMA在十年间所积累的经验和广泛国际合作的基础上,计划小规模改造现有设备,迅速掌握数字多波束合成、高动态大视场成像、前景去除... 详细信息

在继承平方公里阵列(Square Kilometre Array,SKA)望远镜的中国低频探路者——"宇宙第一缕曙光"探测项目2.CMA在十年间所积累的经验和广泛国际合作的基础上,计划小规模改造现有设备,迅速掌握数字多波束合成、高动态大视场成像、前景去除等SKA低频成像的关键核心技术。同时,与SKA低频阵(SKA-low)先导设备MWA(Murchison Widefield Array)开展深层次合作,预选未来用于SKA1-low宇宙再电离深度成像的观测候选区域,为最终利用SKA第一阶段(SKA1)低频阵列,对选定观测候选区域进行深度定点观测做好充分准备,最终实现SKA1既定的首要科学目标。该项目还将建设中国SKA区域中心数据处理原型样机,并以2.CMA和MWA实测数据为基础,完成低频射电干涉成像的数据处理流程,为建设中国SKA区域数据中心打下基础。

关键词：平方公里阵列数字多波束合成高动态大视场成像低频成像