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CO observations of massive star forming regions at different evolutionary phases

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Science china(Physics,Mechanics & Astronomy) 2006年第5期49卷 626-640页

作者： CHEN Xi1,2. XU Ye1,3, SHEN Zhiqiang1,3 & LI Jingjing1,2.1. shanghai Astronomical Observatory, chinese {2. of Sciences, shanghai 2.003., china 2. graduate school of the chinese {2. of Sciences, Beijing 100034, china 3. joint institute for {{12. and cosmology, shanghai Astronomical Observatory and the University of Science and Technology of china, shanghai 2.003., china shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai 200030 China graduate school of the {2. academy of Sciences Beijing 100034 China joint institute for {2. cosmology Shanghai Astronomical Observatory the University of Science Technology of china Shanghai 200030 China

The 12.O (J=1-0), 13CO (J=1-0) and C18O (J=1-0) emissions in 9 massive star forming regions, which are believed to be at different stages of massive star formation, were mapped with the 13.7 m millimeter wave telescope at Qinghai Station of Purple Mountain Observatory. Of the observed 9 sources, 13CO cores were detected in seven of them, and C18O cores in five of them. And only two sources associated with C18O cores and H2. masers showed the extended structures and strong outflows. This is the first detection of outflow associated with IRAS 2.566+582. in the observing field of S152.S153. The physical parameters of cores and outflows for these sources, derived from Local Thermal Equilibrium (LTE) analysis, are presented. These observing results suggest that the C18O cores will only appear when the gas density is high enough and the probability to have an outflow is very high when the clumps show the C18O and H2. maser simulta- neously.

关键词： star formation cloud core outflow H2. maser

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Multi-epoch X-ray observations of the narrow-line Seyfert 1 galaxy SDSS J160508.87+32.92..4 with XMM-Newton

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Science china(Physics,Mechanics & Astronomy) 2010年第S1期53卷 207-211页

作者： AI YanLi1,2.3,YUAN WeiMin1,2.ZHOU HongYan4,5 & WANG JianGuo1,2.3 1 National Astronomical Observatories/Yunnan Observatory,chinese academy of Sciences,Kunming 650011,{2. 2.Key Laboratory for the Structure and Evolution of Celestial Objects,chinese academy of Sciences,Kunming 650011,{2. 3.graduate University of the chinese academy of Sciences,Beijing 100049,{2. 4 Center for Astrophysics,University of Science and Technology of china,Hefei 2.002.,{2. 5 joint institute of Galaxies and cosmology,shao and USTC,shanghai 2.003.,{2. 1. National Astronomical Observatories/Yunnan Observatory Chinese Academy of Sciences Kunming 650011 China 2. Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China 3. graduate University of the chinese {2. of Sciences Beijing 100049 China 4. Center for Astrophysics University of Science and Technology of China Hefei 230026 China 5. joint institute of Galaxies and {2. SHAO and USTC Shanghai 200030 China

We present results of multi-epoch XMM-Newton observations separated by several years of the narrow-line Seyfert 1(NLS1) galaxy,SDSS J160508.87+*** NLS1 showed X-ray flux variations on timescales of years as well as low amplitude variations on timescales as short as hours,while the X-ray spectral shape remained essentially *** spectrum shows a significant soft X-ray *** model of reflection from an ionized disc,that is dominant in the whole XMM-Newton bandpass,provides the best description of the observed spectra for all the observations,though alternatives such as Compton scattering(T-0.2. keV) cannot be ruled out in a statistical *** the disc reflection model,the observed variations may originate either from the change in the reflection fraction,or from the variability of the intrinsic X-ray luminosity.

关键词： galaxies:active Seyfert X-rays individual

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HiFAST:An HIdata calibration and imaging pipeline for FAST

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Science china(Physics,Mechanics & Astronomy) 2024年第5期67卷 182-199页

作者： Yingjie Jing Jie Wang Chen Xu Ziming Liu Qingze Chen Tiantian Liang Jinlong Xu Yixian Cao Jing Wang Huijie Hu Chuan-Peng Zhang Qi Guo Liang Gao Mei Ai Hengqian Gan Xuyang Gao Jinlin Han Ligang Hou Zhipeng Hou Peng Jiang Xu Kong Fujia Li Zerui Liu Li shao Hengxing Pan Jun Pan Lei Qian Jinghai Sun Ningyu Tang Qingliang Yang Bo Zhang Zhiyu Zhang Ming Zhu National Astronomical Observatories Chinese Academy of SciencesBeijing 100012China institute for Frontiers in Astronomy and Astrophysics Beijing Normal UniversityBeijing 02206China school of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China Guizhou Radio Astronomical Observatory Guizhou UniversityGuiyang 55000China Max Planck institute for Extraterrestrial Physics Garching 85748Germany Kavli institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China institute of Computational cosmology Department of PhysicsUniversity of DurhamDurham DHI 3LEUK CAS Key Laboratory of FAST National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China Deep Space Exploration Laboratory/Department of Astronomy University of Science and Technology of ChinaHefei 230026China school of Astronomy and Space Science University of Science and Technology of ChinaHefei 230026China Astrophysics Department of PhysicsUniversity of OxfordOxford OX/3RHUK College of Earth Sciences Guilin University of TechnologyGuilin 541004China Department of Physics Anhui Normal UniversityWuhu 241002China school of Astronomy and Space Science Nanjing UniversityNanjing 210023China Key Laboratory of Modern Astronomy and Astrophysics Nanjing UniversityNanjing 20023China

The Five-hundred-meter Aperture Spherical radio Telescope(FAST)has the largest aperture and a 19-beam L-band receiver,making it powerful for investigating the neutral hydrogen atomic gas(HI)in the *** present HiFAST(https://***),a dedicated,modular,and self-contained calibration and imaging pipeline for processing the H?data of *** pipeline consists of frequency-dependent noise diode calibration,baseline fitting,standing wave removal using an FFT-based method,flux density calibration,stray radiation correction,and gridding to produce data *** modules can be combined as needed to process the data from most FAST observation modes:tracking,drift scanning,On-The-Fly mapping,and most of their *** HiFAST,the root-mean-square(RMS)noises of the calibrated spectra from all 19 beams were only slightly(~5%)higher than the theoretical *** results for the extended source M33 and the point sources are consistent with the results from *** moment maps(0,1 and 2.of M33 agree well with the results from the Arecibo galaxy Environment Survey(AGES)with a fractional difference of less than 10%.For a common sample of 2.1 sources with signal-to-noise ratio S/N>10 from the Arecibo Legacy Fast ALFA(ALFALFA)survey,the mean value of fractional difference in the integrated flux density,Sint,between the two datasets is approximately 0.005%,with a dispersion of 15.4%.Further checks on the integrated flux density of 2. sources with seven observations indicate that the variance in the flux density of the source with luminous objects(Sint>2.5 Jy km s-1)is less than 5%.Our tests suggest that the FAST telescope,with the efficient,precise,and user-friendly pipeline HiFAST,will yield numerous significant scientific findings in the investigation of the H?in the universe.

关键词： fractional luminous correction

HiFAST:An H?data calibration and imaging pipeline for FAST

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Science china(Physics,Mechanics & Astronomy) 2024年第5期Mechanics & Astronomy) .卷 186-203页

作者： Yingjie Jing Jie Wang Chen Xu Ziming Liu Qingze Chen Tiantian Liang Jinlong Xu Yixian Cao Jing Wang Huijie Hu Chuan-Peng Zhang Qi Guo Liang Gao Mei Ai Hengqian Gan Xuyang Gao Jinlin Han Ligang Hou Zhipeng Hou Peng Jiang Xu Kong Fujia Li Zerui Liu Li shao Hengxing Pan Jun Pan Lei Qian Jinghai Sun Ningyu Tang Qingliang Yang Bo Zhang Zhiyu Zhang Ming Zhu National Astronomical Observatories Chinese Academy of Sciences institute for Frontiers in Astronomy and Astrophysics Beijing Normal University school of Astronomy and Space Science University of Chinese Academy of Sciences Guizhou Radio Astronomical Observatory Guizhou University Max Planck institute for Extraterrestrial Physics Kavli institute for Astronomy and Astrophysics Peking University institute of Computational cosmology Department of PhysicsUniversity of Durham CAS Key Laboratory of FAST National Astronomical ObservatoriesChinese Academy of Sciences Deep Space Exploration Laboratory/Department of Astronomy University of Science and Technology of China school of Astronomy and Space Science University of Science and Technology of China Astrophysics Department of PhysicsUniversity of Oxford College of Earth Sciences Guilin University of Technology Department of Physics Anhui Normal University school of Astronomy and Space Science Nanjing University Key Laboratory of Modern Astronomy and Astrophysics Nanjing University

The Five-hundred-meter Aperture Spherical radio Telescope（FAST） has the largest aperture and a 19-beam L-band receiver,making it powerful for investigating the neutral hydrogen atomic gas（H?） in the *** present HiFAST（https://***）,a dedicated,modular,and self-contained calibration and imaging pipeline for processing the H?data of *** pipeline consists of frequency-dependent noise diode calibration,baseline fitting,standing wave removal using an FFT-based method,flux density calibration,stray radiation correction,and gridding to produce data *** modules can be combined as needed to process the data from most FAST observation modes:tracking,drift scanning,On-The-Fly mapping,and most of their *** HiFAST,the root-mean-square（RMS） noises of the calibrated spectra from all 19 beams were only slightly（～5%） higher than the theoretical *** results for the extended source M33 and the point sources are consistent with the results from *** moment maps（0,1 and 2. of M33 agree well with the results from the Arecibo galaxy Environment Survey（AGES） with a fractional difference of less than 10%.For a common sample of 2.1 sources with signal-to-noise ratio S/N>10 from the Arecibo Legacy Fast ALFA（ALFALFA） survey,the mean value of fractional difference in the integrated flux density,Sint,between the two datasets is approximately 0.005%,with a dispersion of 15.4%.Further checks on the integrated flux density of 2. sources with seven observations indicate that the variance in the flux density of the source with luminous objects(Sint>2.5 Jy km s-1) is less than 5%.Our tests suggest that the FAST telescope,with the efficient,precise,and user-friendly pipeline HiFAST,will yield numerous significant scientific findings in the investigation of the H? in the universe.

关键词：

Scientific objectives of the Hot Universe Baryon Surveyor(HUBS) mission

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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 134-178页

作者： Joel Bregman Renyue Cen Yang Chen Wei Cui Taotao Fang Fulai Guo Edmund Hodges-Kluck Rui Huang Luis C.Ho Li Ji Suoqing Ji Xi Kang Xiaoyu Lai Hui Li Jiangtao Li Miao Li Xiangdong Li Yuan Li Zhaosheng Li Guiyun Liang Helei Liu Wenhao Liu Fangjun Lu Junjie Mao Gabriele Ponti Zhijie Qu Chenxi Shan Lijing shao Fangzheng Shi Xinwen Shu Lei Sun Mouyuan Sun Hao Tong Junfeng Wang Junxian Wang Q.Daniel Wang Song Wang Tinggui Wang Weiyang Wang Zhongxiang Wang Dandan Xu Haiguang Xu Heng Xu Renxin Xu Xiaojie Xu Yongquan Xue Hang Yang Feng Yuan Shuinai Zhang Yuning Zhang Zhongli Zhang Yuanyuan Zhao Enping Zhou Ping Zhou Department of Astronomy University of MichiganAnn Arbor MI 48109-1107USA institute for Astronomy School of PhysicsZhejiang UniversityHangzhou 310027China school of Astronomy and Space Science Nanjing UniversityNanjing 210023China Key Laboratory of Modern Astronomy and Astrophysics Nanjing UniversityNanjing 210023China Department of Astronomy Tsinghua UniversityBeijing 100084China Department of Astronomy Xiamen UniversityXiamen 361005China Astrophysics Division Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory for Research in Galaxies and cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China NASA Goddard Space Flight Center Greenbelt MD 20771USA Kavli institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China Department of Astronomy School of PhysicsPeking UniversityBeijing 100871China Purple Mountain Observatory Chinese Academy of SciencesNanjing 210023China Department of Physics and Astronomy Hubei University of EducationWuhan 430205China Department of Physics University of North TexasDenton TX 76203USA Key Laboratory of Stars and Interstellar Medium Xiangtan UniversityXiangtan 411105China CAS Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China school of Physical Science and Technology Xinjiang UniversityUrumuqi 830046China Key Laboratory for Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China INAF-Osservatorio Astronomico di Brera Merate(LC)I-23807Italy Department of Astronomy&Astrophysics the University of ChicagoChicago IL 60637USA school of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Department of Physics Anhui Normal UniversityWuhu 241002China school of Physics and Materials Science Guangzhou UniversityGuangzhou 510006China Department of Astronomy University of Science and Technology of ChinaHefei 230026China Depart

The Hot Universe Baryon Surveyor(HUBS) is a proposed space-based X-ray telescope for detecting X-ray emissions from the hot gas content in our universe. With its unprecedented spatially-resolved high-resolution spectroscopy and large field of view,the HUBS mission will be uniquely qualified to measure the physical and chemical properties of the hot gas in the interstellar medium, the circumgalactic medium, the intergalactic medium, and the intracluster medium. These measurements will be valuable for two key scientific goals of HUBS, namely to unravel the AGN and stellar feedback physics that governs the formation and evolution of galaxies, and to probe the baryon budget and multi-phase states from galactic to cosmological scales. In addition to these two goals, the HUBS mission will also help us solve some problems in the fields of galaxy clusters, AGNs, difuse X-ray backgrounds, supernova remnants, and compact objects. This paper discusses the perspective of advancing these fields using the HUBS telescope.

关键词： X-ray telescopes Galactic halo X-ray sources

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