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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
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 JH(何金华)13; Rivera-Ingraham, Alana14; Wang, Ke15; Cunningham, Maria R.16; Tang, Ya-Wen10; Lai, Shih-Ping17; Yuan, Jinghua18; Li, Di18,19; Fuller, Gary20; Kang, Miju1; Luong, Quang Nguyen6; Liu, Hauyu Baobab10; Ristorcelli, Isabelle21; Yang, Ji22; Xu, Ye22; Hirota, Tomoya6; Mardones, Diego23; Qin, Sheng-Li24; Chen, Huei-Ru10,16; Kwon, Woojin1; Meng, Fanyi25; Zhang, Huawei3; Kim, Mi-Ryang1; Yi, Hee-Weon5
发表期刊ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
2016
卷号222期号:1
DOI10.3847/0067-0049/222/1/7
产权排序第13完成单位
收录类别SCI
关键词Ism: Jets And Outflows Ism: Kinematics And Dynamics Stars: Formation
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.
项目资助者KASI fellowship ; China Ministry of Science and Technology under State Key Development Program for Basic Research(2012CB821800) ; NSFC (11373009, 11433008) ; ESO fellowship ; DFG Priority Program ("Physics of the Interstellar Medium") (1573, WA3628-1/1) ; 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)
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0067-0049
URL查看原文
WOS记录号WOS:000368982300007
WOS研究方向Astronomy & Astrophysics
WOS类目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
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/9323
专题大样本恒星演化研究组
中国科学院天体结构与演化重点实验室
作者单位1.Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Korea
2.Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
3.Department of Astronomy, Peking University, 100871, Beijing, China
4.University of Science & Technology, 217 Gajungro, Yuseong-gu, 305-333 Daejeon, Korea
5.School of Space Research, Kyung Hee University, Yongin-Si, Gyeonggi-Do 446-701, Korea
6.National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
7.Department of Physics, University of Helsinki, FI-00014 Helsinki, Finland
8.Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK
9.Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
10.Academia Sinica, Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 106, Taiwan
11.Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121, Bonn, Germany
12.Astronomy Department, Abdulaziz University, P.O. Box 80203, 21589, Jeddah, Saudi Arabia
13.Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, Kunming, 650011, Yunnan Province, Pr China
14.ESA/ESAC, E-28691 Villanueva de la Cañada, Madrid, Spain
15.European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München, Germany
16.School of Physics, University of New South Wales, Sydney, NSW 2052, Australia
17.Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, Taiwan
18.National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China
19.Key Lab of Radio Astronomy, Chinese Academy of Sciences, China
20.Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK
21.IRAP, CNRS (UMR5277), Université Paul Sabatier, 9 avenue du Colonel Roche, BP 44346, F-31028, Toulouse Cedex 4, France
22.Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China
23.Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
24.Department of Astronomy, Yunnan University, and Key Laboratory of Astroparticle Physics of Yunnan Province, Kunming, 650091, China
25.Physikalisches Institut, Universität zu Köln, Zülpicher Strasse 77, D-50937 Köln, Germany
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Liu, Tie,Zhang, Qizhou,Kim, Kee-Tae,et al. 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[J]. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,2016,222(1).
APA Liu, Tie.,Zhang, Qizhou.,Kim, Kee-Tae.,Wu, Yuefang.,Lee, Chang Won.,...&Yi, Hee-Weon.(2016).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.ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,222(1).
MLA Liu, Tie,et al."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".ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 222.1(2016).
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