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题名: PLANCK COLD CLUMPS IN THE lambda ORIONIS COMPLEX. I. DISCOVERY OF AN EXTREMELY YOUNG CLASS 0 PROTOSTELLAR OBJECT AND A PROTO-BROWN DWARF CANDIDATE IN THE BRIGHT-RIMMED CLUMP PGCC G192.32-11.88
作者: Liu, Tie1; Zhang, Qizhou2; Kim, Kee-Tae1; Wu, Yuefang3; Lee, Chang Won1, 4; Lee, Jeong-Eun5; Tatematsu, Ken'ichi6; Choi, Minho1; Juvela, Mika7; Thompson, Mark8; Goldsmith, Paul F.9; Liu, Sheng-yuan10; Naomi, Hirano10; Koch, Patrick10; Henkel, Christian11, 12; Sanhueza, Patricio6; He, JinHua13; Rivera-Ingraham, Alana14; Wang, Ke15; Cunningham, Maria R.16; Tang, Ya-Wen10; Lai, Shih-Ping17, 18; Yuan, Jinghua19; Li, Di19, 20; Fuller, Gary21; Kang, Miju1; Luong, Quang Nguyen6; Liu, Hauyu Baobab10; Ristorcelli, Isabelle22; Yang Ji(杨戟)23; Xu Ye(徐烨)23; Hirota, Tomoya6; Mardones, Diego24; Qin, Sheng-Li25, 26; Chen, Huei-Ru10; Kwon, Woojin1; Meng, Fanyi27; Zhang, Huawei3; Kim, Mi-Ryang1; Yi, Hee-Weon5
刊名: ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
出版日期: 2016
卷号: 222, 期号:1
关键词: ISM: jets and outflows ; ISM: kinematics and dynamics ; stars: formation
文章类型: Article
英文摘要: We are performing a series of observations with ground-based telescopes toward Planck Galactic cold clumps (PGCCs) in the lambda Orionis complex in order to systematically investigate the effects of stellar feedback. In the particular case of PGCC G192.32-11.88, we discovered an extremely young Class 0 protostellar object (G192N) and a proto-brown dwarf candidate (G192S). G192N and G192S are located in a gravitationally bound brightrimmed clump. The velocity and temperature gradients seen in line emission of CO isotopologues indicate that PGCC G192.32-11.88 is externally heated and compressed. G192N probably has the lowest bolometric luminosity (similar to 0.8 L-circle dot) and accretion rate (6.3 x 10(-7) M-circle dot yr(-1)) when compared with other young Class 0 sources (e.g., PACS Bright Red Sources) in the Orion complex. It has slightly larger internal luminosity (0.21 +/- 0.01 L-circle dot) and outflow velocity (similar to 14 km s(-1)) than the predictions of first hydrostatic cores (FHSCs). G192N might be among the youngest Class 0 sources, which are slightly more evolved than an FHSC. Considering its low internal luminosity (0.08 +/- 0.01 L-circle dot) and accretion rate (2.8 x 10(-8) M-circle dot yr(-1)), G192S is an ideal proto-brown dwarf candidate. The star formation efficiency (similar to 0.3%-0.4%) and core formation efficiency (similar to 1%) in PGCC G192.32-11.88 are significantly smaller than in other giant molecular clouds or filaments, indicating that the star formation therein is greatly suppressed owing to stellar feedback.
WOS标题词: Science & Technology ; Physical Sciences
类目[WOS]: Astronomy & Astrophysics
研究领域[WOS]: Astronomy & Astrophysics
关键词[WOS]: MASSIVE-STAR-FORMATION ; SPECTRAL ENERGY-DISTRIBUTIONS ; RADIATION-DRIVEN IMPLOSION ; IRAS POINT SOURCES ; H-II REGIONS ; STELLAR OBJECTS ; MOLECULAR CLOUDS ; SUBMILLIMETER ARRAY ; FORMING REGION ; CORES
收录类别: SCI
项目资助者: KASI fellowship ; China Ministry of Science and Technology under State Key Development Program for Basic Research(2012CB821800) ; NSFC(11373009 ; ESO fellowship ; DFG Priority Program ("Physics of the Interstellar Medium")(1573 ; National Research Foundation of Korea (NRF) - Ministry of Education, Science, and Technology(NRF-2013R1A1A2A10005125) ; global research collaboration of the Korea Research Council of Fundamental Science & Technology (KRCF) ; National Research Foundation of Korea (NRF)(NRF-2015R1A2A2A01004769) ; Korea Astronomy and Space Science Institute under the RD program(2015-1-320-18) ; Ministry of Science and Technology of Taiwan(MoST 102-2119-M-007-004-MY3) ; 11433008) ; WA3628-1/1)
语种: 英语
WOS记录号: WOS:000368982300007
Citation statistics:
内容类型: 期刊论文
URI标识: http://libir.pmo.ac.cn/handle/332002/16118
Appears in Collections:紫金山天文台青海观测站_期刊论文

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作者单位: 1.Korea Astron & Space Sci Inst, Daejeon 34055, South Korea
2.Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
3.Peking Univ, Dept Astron, Beijing 100871, Peoples R China
4.Univ Sci & Technol, Daejeon 305333, South Korea
5.Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea
6.Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan
7.Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland
8.Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England
9.CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA
10.Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan
11.Max Planck Inst Radioastron, D-53121 Bonn, Germany
12.Abdulaziz Univ, Dept Astron, Jeddah 21589, Saudi Arabia
13.Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Yunnan Observ, Kunming 650011, Yunnan Province, Peoples R China
14.ESA ESAC, E-28691 Madrid, Spain
15.European So Observ, D-85748 Garching, Germany
16.Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia
17.Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan
18.Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan
19.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
20.Chinese Acad Sci, Key Lab Radio Astron, Beijing 100864, Peoples R China
21.Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England
22.Univ Toulouse 3, CNRS, IRAP, UMR5277, F-31028 Toulouse 4, France
23.Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China
24.Univ Chile, Dept Astron, Santiago, Chile
25.Yunnan Univ, Dept Astron, Kunming 650091, Peoples R China
26.Yunnan Univ, Key Lab Astroparticle Phys Yunnan Prov, Kunming 650091, Peoples R China
27.Univ Cologne, Inst Phys, D-50937 Cologne, Germany
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