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Research in Astronomy and Astrophysics 2024年第10期24卷 130-140页

作者： Long-Fei Chen Chao-Wei Tsai Jian-Yang li Bin Yang Di li Yan Duan Chih-Hao Hsia Zhichen Pan Lei Qian Donghui Quan Xue-Jian Jiang Xiaohu li Ruining Zhao Pei Zuo School of Physics and Electronic Science Guizhou Normal UniversityGuiyang 550025China Guizhou Provincial key Laboratory of Radio Astronomy and Data Processing Guiyang 550025China Research Center for astronomical Computing Zhejiang LaboratoryHangzhou 311100China national astronomical {2. Chinese Academy of SciencesBeijing 100101China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal UniversityBeijing 102206China key Laboratory of Radio Astronomy and Technology Chinese Academy of SciencesBeijing 100101China School of Atmospheric sciences Sun Yat-sen UniversityZhuhai 519082China Núcleo de Astronomía Facultad de Ingenieríay CienciasUniversidad Diego PortalesChile Department of Astronomy College of Physics and Electronic EngineeringQilu Normal UniversityJinan 250200China Department of Electronic and Optical Engineering Space Engineering UniversityBeijing 101416China Laboratory for Space Research Faculty of ScienceThe University of Hong KongHong Kong(SAR)China Xinjiang astronomical observatory Chinese Academy of SciencesUrumqi 830011China CAS key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China School of Astronomy and Space sciences University of Chinese Academy of SciencesBeijing 100049China

We used the Five-hundred-meter Aperture Spherical radio Telescope(FAST)to search for the molecular emissions in the L-band between 1.0 and 1.5 GHz toward four comets,C/2.2. F3(NEOWISE),C/2.2. R4(ATLAS),C/2.2. A1(Leonard),and 67P/Churyumov-Gerasimenko during or after their perihelion *** of molecular transition lines fall in this low-frequency range,many attributed to complex organic or prebiotic *** conducted a blind search for the possible molecular lines in this frequency range in those comets and could not identify clear signals of molecular emissions in the *** several molecules have been detected at high frequencies of greater than100 GHz in comets,our results confirm that it is challenging to detect molecular transitions in the L-band frequency *** non-detection of L-band molecular lines in the cometary environment could rule out the possibility of unusually strong lines,which could be caused by the masers or non-LTE *** the line strengths are predicted to be weak,for FAST,using the ultra-wide bandwidth receiver and improving the radio frequency interference environments would enhance the detectability of those molecular transitions at low frequencies in the future.

关键词： astrochemistry ISM:molecules comets:general line:identification

A discovery of two slow pulsars with FAST:“Ronin”from the globular cluster M15

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Science china(Physics,Mechanics & Astronomy) 2024年第6期67卷 166-180页

作者： Dengke Zhou Pei Wang Di li Jianhua Fang Chenchen Miao Paulo CCFreire Lei Zhang Dandan Zhang Huaxi Chen Yi Feng Yifan Xiao Jintao Xie Xu Zhang Chenwu Jin Han Wang Yinan ke Xuerong Guo Rushuang Zhao Chenhui Niu Weiwei Zhu Mengyao Xue Yabiao Wang Jiafu Wu Zhenye Gan Zhongyi Sun Chengjie Wang Jie Zhang junshuo Zhang Jinhuang Cao Wanjin Lu Research Center for astronomical Computing Zhejiang LaboratoryHangzhou 311121China national astronomical {2. Chinese Academy of SciencesBeijing 100101China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal UniversityBeijing 102206China University of chinese Academy of sciences Beijing 100049China New Cornerstone Science Laboratory Shenzhen 518054China Max Planck Institut f¨ur Radioastronomie Bonn 53121Germany Centre for Astrophysics and Supercomputing Swinburne University of TechnologyHawthorn 3122Australia School of Mathematical sciences School of Physics and Electronic SciencesGuizhou Normal UniversityGuiyang 550001China Guizhou Provincial key Laboratory of Radio Astronomy and Data Processing Guiyang 550001China School of Physics and Electronic Engineering Qilu Normal UniversityJinan 250200China School of Physics and Electronic Science Guizhou Normal UniversityGuiyang 550001China College of Physical Science and Technology Central China Normal UniversityWuhan 430079China Tencent Youtu Lab Shanghai 201103China

Globular clusters harbor numerous millisecond pulsars,but long-period pulsars(P 100 ms)are rarely *** this study,we employed a fast folding algorithm to analyze observational data from multiple globular clusters obtained by the Five-hundredmeter Aperture Spherical radio Telescope(FAST),aiming to detect the existence of long-period *** estimated the impact of the median filtering algorithm in eliminating red noise on the minimum detectable flux density(S_(min))of ***,we successfully discovered two isolated long-period pulsars in M15 with periods approximately equal to 1.92.451 and3.960716 s,*** the P-˙P diagram,both pulsars are positioned below the spin-up line,suggesting a possible history of partial recycling in X-ray binary systems disrupted by dynamical encounters later *** to timing results,these two pulsars exhibit remarkably strong magnetic *** the magnetic fields were weakened during the accretion process,then a short duration of accretion might explain the strong magnetic fields of these pulsars.

关键词： pulsar globular cluster FAST

A versatile framework for analyzing galaxy image data by incorporating Human-in-the-loop in a large vision model

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chinese Physics C 2024年第9期48卷 176-187页

作者： Ming-Xiang Fu Yu Song Jia-Meng Lv liang Cao Peng Jia Nan li Xiang-Ru li Ji-Feng liu A-li Luo Bo Qiu Shi-Yin Shen liang-Ping Tu li-li Wang Shou-lin Wei Hai-Feng Yang Zhen-Ping Yi Zhi-Qiang Zou national astronomical {2. Chinese Academy of SciencesBeijing 100101China College of Electronic Information and Optical Engineering Taiyuan University of TechnologyTaiyuan 030024China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 101408China key lab of Space Astronomy and Technology National Astronomical ObservatoriesBeijing 100101China School of Computer Science South China Normal UniversityGuangzhou 510631China CAS key Laboratory of Optical Astronomy National Astronomical ObservatoriesBeijing 100101China University of chinese Academy of sciences NanjingNanjing 211135China University of Science and Technology Beijing Beijing 100083China Shanghai astronomical observatory Chinese Academy of SciencesShanghai 200030China School of Computer and Information Dezhou UniversityDezhou 253023China Faculty of Information Engineering and Automation Kunming University of Science and TechnologyKunming 650500China School of Computer Science and Technology Taiyuan University of Science and TechnologyTaiyuan 30024China School of Mechanical Electrical and Information EngineeringShandong UniversityWeihai 264209China Nanjing University of Posts&Telecommunications Nanjing 210023China School of Science University of Science and Technology LiaoningAnshan 114051China

The exponential growth of astronomical datasets provides an unprecedented opportunity for humans to gain insight into the ***,effectively analyzing this vast amount of data poses a significant *** response,astronomers are turning to deep learning techniques,but these methods are limited by their specific training sets,leading to considerable duplicate *** overcome this issue,we built a framework for the general analysis of galaxy images based on a large vision model(LVM)plus downstream tasks(DST),including galaxy morphological classification,image restoration object detection,parameter extraction,and *** the low signal-to-noise ratios of galaxy images and the imbalanced distribution of galaxy categories,we designed our LVM to incorporate a Human-in-the-loop(HITL)module,which leverages human knowledge to enhance the reliability and interpretability of processing galaxy images *** proposed framework exhibits notable fewshot learning capabilities and versatile adaptability for all the abovementioned tasks on galaxy images in the DESI Legacy Imaging *** particular,for the object detection task,which was trained using 1000 data points,our DST in the LVM achieved an accuracy of 96.7%,while ResNet50 plus Mask R-CNN reached an accuracy of 93.1%.For morphological classification,to obtain an area under the curve(AUC)of~0.9,LVM plus DST and HITL only requested 1/50 of the training sets that ResNet18 *** addition,multimodal data can be integrated,which creates possibilities for conducting joint analyses with datasets spanning diverse domains in the era of multi-messenger astronomy.

关键词： artificial intelligence large vision model human-in-the-loop astronomy galaxies

Application of multi-pulse optical imaging to measure evolution of laser-produced counter-streaming flows

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chinese Physics B 2017年第5期26卷 165-169页

作者：袁大伟李玉同朱保君李彦霏仲佳勇魏会冈刘畅原晓霞张喆梁贵云王菲鹿李芳赵家瑞华能朱宝强朱健强江少恩杜凯丁永坤赵刚张杰 key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences national Laboratory for Condensed Matter Physics Institute of Physics Chinese Academy of Sciences School of Physical sciences University of Chinese Academy of Sciences Collaborative Innovation Center of IFSA(CICIFSA) Shanghai Jiaotong University Department of Astronomy Beijing Normal University national Laboratory on High Power Lasers and Physics Research Center for Laser Fusion China Academy of Engineering Physics key Laboratory for Laser Plasmas(Ministry of Education)and Department of Physics and Astronomy Shanghai Jiao Tong University

A counter-streaming flow system is a test-bed to investigate the astrophysical collisionless shock（CS） formation in the laboratory. Electrostatic/electromagnetic instabilities, competitively growing in the system and exciting the CS formation, are sensitive to the flows parameters. One of the most important parameters is the velocity, determining what kind of instability contributes to the shock formation. Here we successfully measure the evolution of the counter-streaming flows within one shot using a multi-pulses imaging diagnostic technique. With the technique, the average velocity of the high-density-part（ne ≥ 8–9 × 10^19cm^-3） of the flow is directly measured to be of ～ 10^6cm/s between 7 ns and 17 ***, the average velocity of the low-density-part（ne ≤ 2.× 10^19cm^-3） can be estimated as ～ 10^7cm/s. The experimental results show that a collisionless shock is formed during the low-density-part of the flow interacting with each other.

关键词： streaming counter interacting exciting instability determining diagnostic colors distinguish gamma

Estimating the Size and Timing of the Maximum Amplitude of Solar Cycle 2.

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chinese Journal of Astronomy and Astrophysics 2005年第5期5卷 539-545页

作者： ke-jun {2. Peng-Xin Gao Tong.Wei Su national astronomical {2. Yunnan Observatory Chinese Academy of SciencesKunming 650011 Graduate University of chinese Academy of sciences Beijing 100049

A simple statistical method is used to estimate the size and timing of maximum amplitude of the next solar cycle （cycle 2.）. Presuming cycle 2. to be a short cycle （as is more li{2.ly）, the minimum of cycle 2. should occur about December 2.06 （±2.months） and the maximum, around March 2.11 （±9 months）, and the amplitude is 189.9 ± 15.5, if it is a fast riser, or about 136, if it is a slow riser. If we presume cycle 2. to be a long cycle （as is less li{2.ly）, the minimum of cycle 2. should occur about june 2.08 （±2.months） and the maximum, about February 2.13 （±8 months） and the maximum will be about 137 or 80, according as the cycle is a fast riser or a slow riser.

关键词： Sun: activity - Sun: sunspot - Sun: prediction

The ALMA-QUARKS Survey.Ⅰ.Survey Description and Data Reduction

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Research in Astronomy and Astrophysics 2024年第2期24卷 104-124页

作者：刘训川 Tie liu Lei Zhu Guido Garay Hong-li liu Paul Goldsmith Neal Evans kee-Tae Kim Sheng-Yuan liu Fengwei Xu Xing Lu Anandmayee Tej Xiaofeng Mai Leonardo Bronfman Shanghuo li Diego Mardones Amelia Stutz ken'ichi Tatematsu ke Wang Qizhou Zhang Sheng-li Qin Jianwen Zhou Qiuyi Luo Siju Zhang Yu Cheng Jinhua He Qilao Gu Ziyang li Zhenying Zhang Suinan Zhang Anindya Saha Lokesh Dewangan Patricio Sanhueza Zhiqiang Shen Shanghai astronomical observatory Chinese Academy of SciencesShanghai 200030China chinese Academy of sciences South America Center for Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China Departamento de Astronomía Universidad de ChileLas Condes7591245 SantiagoChile School of Physics and Astronomy Yunnan UniversityKunming 650091China Jet Propulsion Laboratory California Institute of Technology4800 Oak Grove DrivePasadena CA 91109USA Department of Astronomy The University of Texas at AustinTX 78712-1205USA Korea Astronomy and Space Science Institute 776 Daedeokdae-roYuseong-guDaejeon 34055Republic of Korea Institute of Astronomy and Astrophysics Academia SinicaRoosevelt RoadTaipei 10617China Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China Department of Astronomy School of PhysicsPeking UniversityBeijing 100871China Indian Institute of Space Science and Technology Thiruvananthapuram 695547KeralaIndia Max Planck Institute for Astronomy Königstuhl 17D-69117 HeidelbergGermany Departamento de Astronomía Universidad de ConcepciónCasilla 160-CConcepciónChile Nobeyama Radio observatory National Astronomical Observatory of JapanNational Institutes of Natural Sciences462-2 NobeyamaMinamimakiMinamisakuNagano 384-1305Japan Center for Astrophysics∣Harvard&Smithsonian 60 Garden StreetCambridgeMA 02138USA Max-Planck-Institut für Radioastronomie Auf dem Hügel 69D-53125 BonnGermany School of Astronomy and Space sciences University of Chinese Academy of SciencesBeijing 100049China national astronomical {2. of Japan 2-21-1 OsawaMitakaTokyo181-8588Japan yunnan observatories Chinese Academy of SciencesKunming 650216China Physical Research Laboratory NavrangpuraAhmedabad-380009India astronomical Science Program The Graduate University for Advanced StudiesSOKENDAI2-21-1 OsawaMitakaTokyo 181-8588Japan University of Science and Technology Korea(UST)217 Gajeong-roYuseong-guDaejeon 34113Republic o

This paper presents an overview of the QUARKS survey,which stands for Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures."The QUARKS survey is observing139 massive clumps covered by 156 pointings at Atacama Large Millimeter/submillimeter Array(ALMA)Band 6(λ~1.3 mm).In con{2.ction with data obtained from the ALMA-ATOMS survey at Band 3(λ~3 mm),QUARKS aims to carry out an unbiased statistical investigation of massive star formation process within protoclusters down to a scale of 1000 *** overview paper describes the observations and data reduction of the QUARKS survey,and gives a first look at an exemplar source,the mini-starburst Sgr B2.M).The wide-b and width(7.5 GHz)and high-angular-resolution(~0."3)observations of the QUARKS survey allow for the resolution of much more compact cores than those could be done by the ATOMS survey,and to detect previously unrevealed fainter filamentary *** spectral windows cover transitions of species including CO,SO,N_(2.D^(+),SiO,H_(30)α,H_(2.CO,CH_(3)CN,and many other complex organic molecules,tracing gas components with different temperatures and spatial *** aims to deepen our understanding of several scientific topics of massive star formation,such as the mass transport within protoclusters by(hub-)filamentary structures,the existence of massive starless cores,the physical and chemical properties of dense cores within protoclusters,and the feedback from already formed high-mass young protostars.

关键词： stars formation-stars kinematics and dynamics-ISM clouds-ISM molecules

On the Performances of Estimating Stellar Atmospheric Parameters from CSST Broad-band Photometry

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Research in Astronomy and Astrophysics 2024年第4期24卷 161-173页

作者： Rui-Feng Shi Yang Huang Xin-Yi li Hua-Wei Zhang School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China South-Western Institute for Astronomy Research Yunnan UniversityKunming 650500China CAS key Lab of Optical Astronomy Key Laboratory of Space Astronomy and TechnologyNational Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China College of Physics and Electronic Engineering Qilu Normal UniversityJinan 250200China Department of Astronomy School of PhysicsPeking UniversityBeijing 100871China Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China

Deriving atmospheric parameters of a large sample of stars is of vital importance to understand the formation and evolution of the Milky *** surveys,especially those with near-ultraviolet filters,can offer accurate measurements of stellar parameters,with the precision comparable to that from low/medium resolution *** this study,we explore the capability of measuring stellar atmospheric parameters from chinese Space Station Telescope(CSST)broad-band photometry(particularly in the near-ultraviolet bands),based on synthetic colors derived from model *** find that colors from the optical and near-ultraviolet filter systems adopted by CSST show significant sensitivities to the stellar atmospheric parameters,especially the *** to our mock data tests,the precision of the photometric metallicity is quite high,with typical values of0.17 and 0.2. dex for dwarf and giant stars,*** precision of the effective temperature estimated from broad-band colors are within 50 K.

关键词： methods:data analysis stars:abundances surveys

Preliminary results of FeO mapping using Imaging Interferometer data from Chang'E-1

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Science Bulletin 2011年第Z1期 376-379页

作者： liNG ZongCheng1,2.ZHANG Jiang1,2.liU JianZhong1,ZHANG WenXi3,BIAN Wei1, REN Xin1,MU lingli1,liU Jianjun1 & li ChunLai1 1 national astronomical observatories,chinese Academy of sciences,Beijing 100012.{12. 2.School of Space Science and Physics & Shandong Provincial key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Shandong University at Weihai,Weihai 2.42.9,{12. 3 Academy of Opto-Electronics,chinese Academy of sciences,Beijing 100080,{12.

Information about the variability,and spatial distribution of iron abundance is important to understand lunar geological history and for future resource utilization. In this paper we present a preliminary model to produce an iron abundance map using images taken by an Imaging Interferometer on board the satellite Chang'E-1. Compared with the Clementine UVVIS images,the images from the Chang'E-1 satellite also allowed for the extraction of FeO abundance distributions on the Moon. However,the prelimi-nary model results suggest an underestimation of ～2.wt.% for the FeO content of the mare region and an overestimation of ～3 wt.% for the highland region.

关键词： Chang’E-1 Imaging Interferometer FeO mapping Clementine UVVIS

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强迫振动及实时振中控制的气浮台仿真技术

系统仿真学报 2003年第5期15卷 667-669页

作者：李怀锋韩建国李彦琴金声震中国科学院国家天文台空间实验室北京100012 北京化工大学信息科学与技术学院111信箱北京100029

通过分析该控制系统中的力矩及干扰因素,提出一种高频振动下的气浮台仿真方法。在仿真过程中对气浮台进行电磁强迫振动而又对其实时振动中心进行反馈虑波PID控制。推导出其关键参数的测算方法并分析了相应的实验结果。这种技术可广泛应... 详细信息

通过分析该控制系统中的力矩及干扰因素,提出一种高频振动下的气浮台仿真方法。在仿真过程中对气浮台进行电磁强迫振动而又对其实时振动中心进行反馈虑波PID控制。推导出其关键参数的测算方法并分析了相应的实验结果。这种技术可广泛应用于与一维角位移振动仿真的有关领域。

关键词：气浮平台一维角位移振动振动中心反馈滤波PID控制