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Sequential star formation in the filamentary structures of the Planck Galactic cold clump G181.84+0.31

文献类型：期刊论文

作者Yuan, Lixia1,2,3; Zhu, Ming1,3; Liu, Tie4,5; Yuan, Jinghua1; Wu, Yuefang6; Kim, Kee-Tae4; Wang, Ke7,8; Zhou, Chenlin1,2,3; Tatematsu, Ken'ichi9; Kuno, Nario10,11
刊名MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
出版日期2019-07-01
卷号487期号:1页码:1315-1334
关键词stars: formation stars: protostars ISM: clouds ISM: kinematics and dynamics ISM: structure
ISSN号0035-8711
DOI10.1093/mnras/stz1266
英文摘要We present a multiwavelength study of the Planck Galactic cold clump G181.84+0.31, which is located at the northern end of the extended filamentary structure S242. We have extracted nine compact dense cores from the SCUBA-2 850-mu m map, and we have identified 18 young stellar objects (YSOs; four Class I and 14 Class II) based on their Spitzer, Wide-field Infrared Survey Explorer (WISE) and Two-Micron All-Sky Survey (2MASS) near-and mid-infrared colours. The dense cores and YSOs are mainly distributed along the filamentary structures of G181.84 and are well traced by HCO+(1-0) and N2H+(1-0) spectral-line emission. We find signatures of sequential star formation activities in G181.84: dense cores and YSOs located in the northern and southern substructures are younger than those in the central region. We also detect global velocity gradients of about 0.8 +/- 0.05 and 1.0 +/- 0.05 km s(-1) pc(-1) along the northern and southern substructures, respectively, and local velocity gradients of 1.2 +/- 0.1 km s(-1) pc(-1) in the central substructure. These results might be due to the fact that the global collapse of the extended filamentary structure S242 is driven by an edge effect, for which the filament edges collapse first and then further trigger star formation activities inward. We identify three substructures in G181.84 and estimate their critical masses per unit length, which are similar to 101 +/- 15, 56 +/- 8 and 28 +/- 4 M-circle dot pc(-1), respectively. These values are all lower than the observed values (similar to 200 M-circle dot pc(-1)), suggesting that these substructures are gravitationally unstable.
WOS关键词DARK CLOUDS ; DENSE CORES ; MAIN-SEQUENCE ; IDENTIFICATION ; N2H+ ; EXCITATION ; EMISSION ; CLUSTERS ; MAPS
资助项目National Key R&D Program of China[2017YFA0402600] ; NSFC[U1531246] ; NSFC[11503035] ; NSFC[11573036] ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; National Key Research and Development Program of China[2017YFA0402702] ; National Science Foundation of China[11721303] ; Kavli Institute for Astronomy and Astrophysics, Peking University[7101502016] ; Science and Technology Facilities Council of the United Kingdom ; National Science Foundation[ACI-1440620] ; NASA's Earth Science Technology Office, Computation Technologies Project[NCC5626] ; Ministry of Finance (MOF) of China
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:000474907100101
出版者OXFORD UNIV PRESS
资助机构National Key R&D Program of China ; National Key R&D Program of China ; NSFC ; NSFC ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Science and Technology Facilities Council of the United Kingdom ; Science and Technology Facilities Council of the United Kingdom ; National Science Foundation ; National Science Foundation ; NASA's Earth Science Technology Office, Computation Technologies Project ; NASA's Earth Science Technology Office, Computation Technologies Project ; Ministry of Finance (MOF) of China ; Ministry of Finance (MOF) of China ; National Key R&D Program of China ; National Key R&D Program of China ; NSFC ; NSFC ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Science and Technology Facilities Council of the United Kingdom ; Science and Technology Facilities Council of the United Kingdom ; National Science Foundation ; National Science Foundation ; NASA's Earth Science Technology Office, Computation Technologies Project ; NASA's Earth Science Technology Office, Computation Technologies Project ; Ministry of Finance (MOF) of China ; Ministry of Finance (MOF) of China ; National Key R&D Program of China ; National Key R&D Program of China ; NSFC ; NSFC ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Science and Technology Facilities Council of the United Kingdom ; Science and Technology Facilities Council of the United Kingdom ; National Science Foundation ; National Science Foundation ; NASA's Earth Science Technology Office, Computation Technologies Project ; NASA's Earth Science Technology Office, Computation Technologies Project ; Ministry of Finance (MOF) of China ; Ministry of Finance (MOF) of China ; National Key R&D Program of China ; National Key R&D Program of China ; NSFC ; NSFC ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Science and Technology Facilities Council of the United Kingdom ; Science and Technology Facilities Council of the United Kingdom ; National Science Foundation ; National Science Foundation ; NASA's Earth Science Technology Office, Computation Technologies Project ; NASA's Earth Science Technology Office, Computation Technologies Project ; Ministry of Finance (MOF) of China ; Ministry of Finance (MOF) of China
源URL[http://ir.bao.ac.cn/handle/114a11/26915]  
专题中国科学院国家天文台
通讯作者Yuan, Lixia; Zhu, Ming
作者单位1.Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100101, Peoples R China
2.Univ Chinese Acad Sci, Beijing 100049, Peoples R China
3.Chinese Acad Sci, Key Lab FAST, NAOC, Beijing 100012, Peoples R China
4.Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea
5.East Asian Observ, 660 N Aohoku Pl, Hilo, HI 96720 USA
6.Peking Univ, Dept Astron, Beijing 100871, Peoples R China
7.Peking Univ, Kavli Inst Astron & Astrophys, 5 Yiheyuan Rd, Beijing 100871, Peoples R China
8.ESO Headquarters, Karl Schwarzschild Str 2, D-85748 Garching, Germany
9.Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
10.Univ Tsukuba, Tomonaga Ctr Hist Universe, 1-1-1 Tennodai, Tsukuba, Ibaraki 3058571, Japan
推荐引用方式
GB/T 7714		 Yuan, Lixia,Zhu, Ming,Liu, Tie,et al. Sequential star formation in the filamentary structures of the Planck Galactic cold clump G181.84+0.31[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2019,487(1):1315-1334.
APA Yuan, Lixia.,Zhu, Ming.,Liu, Tie.,Yuan, Jinghua.,Wu, Yuefang.,...&Kuno, Nario.(2019).Sequential star formation in the filamentary structures of the Planck Galactic cold clump G181.84+0.31.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,487(1),1315-1334.
MLA Yuan, Lixia,et al."Sequential star formation in the filamentary structures of the Planck Galactic cold clump G181.84+0.31".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 487.1(2019):1315-1334.

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