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作 者:江治波 张少博 陈志维 杨旸 于书岭 冯浩然 杨戟 the MWISP Group Zhibo Jiang;Shaobo Zhang;Zhiwei Chen;Yang Yang;Shuling Yu;Haoran Feng;Ji Yang;the MWISP Group(Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210023,China;University of Science and Technology of China,Hefei 230026,China;Center for Astronomy and Space Sciences,Three Gorges University,Yichang 443002,China)
机构地区:[1]Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210023,China [2]University of Science and Technology of China,Hefei 230026,China [3]Center for Astronomy and Space Sciences,Three Gorges University,Yichang 443002,China
出 处:《Research in Astronomy and Astrophysics》2023年第7期1-14,共14页天文和天体物理学研究(英文版)
基 金:supported by the National Key R&D Program of China(Grant No.2017YFA0402702);the National Natural Science Foundation of China(NSFC,Grant Nos.,11873093,U2031202,and 11903083);sponsored by the National Key R&D Program of China with Grant 2017YFA0402701;CAS Key Research Program of Frontier Sciences with grant QYZDJ-SSW-SLH047。
摘 要:We have started a systematic survey of molecular clumps with infall motions to study the very early phase of star formation.Our first step is to utilize the data products by MWISP to make an unbiased survey for blue asymmetric line profiles of CO isotopical molecules.Within a total area of~2400 square degrees nearby the Galactic plane,we have found 3533 candidates showing blue-profiles,in which 3329 are selected from the^(12)CO&^(13)CO pair and 204 are from the^(13)CO&C^(18)O pair.Exploration of the parametric spaces suggests our samples are in the cold phase with relatively high column densities ready for star formation.Analysis of the spatial distribution of our samples suggests that they exist virtually in all major components of the galaxy.The vertical distribution suggest that the sources are located mainly in the thick disk of~85 pc,but still a small part are located far beyond Galactic midplane.Our follow-up observation indicates that these candidates are a good sample to start a search for infall motions,and to study the condition of very early phase of star formation.
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