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Astrochemical Properties of Planck Cold Clumps
Tatematsu, Ken'ichi1,2; Liu, Tie3; Ohashi, Satoshi4; Sanhueza, Patricio1; Quang Nguyen Luong1,3; Hirota, Tomoya1,2; Liu, Sheng-Yuan5; Hirano, Naomi5; Choi, Minho3; Kang, Miju3; Thompson, Mark A.6; Fuller, Gary7; Wu, Yuefang8; Li, Di9; Di Francesco, James10,11; Kim, Kee-Tae3; Wang, Ke12; Ristorcelli, Isabelle13; Juvela, Mika14; Shinnaga, Hiroko15; Cunningham, Maria16; Saito, Masao17; Lee, Jeong-Eun18; Toth, L. Viktor19; He, Jinhua20,21,22; Sakai, Takeshi23; Kim, Jungha18; JCMT Large Program SCOPE Collabora; TRAO Key Science Program TOP Colla
2017-02-01
Source PublicationASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
Volume228Issue:2
AbstractWe observed 13 Planck cold clumps with the James Clerk Maxwell Telescope/SCUBA-2 and with the Nobeyama 45 m radio telescope. The N2H+ distribution obtained with the Nobeyama telescope is quite similar to SCUBA-2 dust distribution. The 82 GHz HC3N, 82 GHz CCS, and 94 GHz CCS emission are often distributed differently with respect to the N2H+ emission. The CCS emission, which is known to be abundant in starless molecular cloud cores, is often very clumpy in the observed targets. We made deep single-pointing observations in DNC, (HNC)-C-13, N2D+, and cyclic-C3H2 toward nine clumps. The detection rate of N2D+ is 50%. Furthermore, we observed the NH3 emission toward 15 Planck cold clumps to estimate the kinetic temperature, and confirmed that most targets are cold (less than or similar to 20 K). In two of the starless clumps we observed, the CCS emission is distributed as it surrounds the N2H+ core (chemically evolved gas), which resembles the case of L1544, a prestellar core showing collapse. In addition, we detected both DNC and N2D+. These two clumps are most likely on the verge of star formation. We introduce the chemical evolution factor (CEF) for starless cores to describe the chemical evolutionary stage, and analyze the observed Planck cold clumps.
SubtypeArticle
KeywordIsm: Clouds Ism: Molecules Ism: Structure Stars: Formation
WOS HeadingsScience & Technology ; Physical Sciences
Funding OrganizationNational Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning(NRF-2015R1C1A1A01052160) ; National Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning(NRF-2015R1C1A1A01052160) ; Academy of Finland(285769) ; Academy of Finland(285769) ; German Research Foundation (DFG)(WA3628-1/1) ; German Research Foundation (DFG)(WA3628-1/1) ; Chinese Academy of Sciences(XDB09000000) ; Chinese Academy of Sciences(XDB09000000) ; Science and Technology Facilities Council of the United Kingdom ; Science and Technology Facilities Council of the United Kingdom ; National Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning(NRF-2015R1C1A1A01052160) ; National Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning(NRF-2015R1C1A1A01052160) ; Academy of Finland(285769) ; Academy of Finland(285769) ; German Research Foundation (DFG)(WA3628-1/1) ; German Research Foundation (DFG)(WA3628-1/1) ; Chinese Academy of Sciences(XDB09000000) ; Chinese Academy of Sciences(XDB09000000) ; Science and Technology Facilities Council of the United Kingdom ; Science and Technology Facilities Council of the United Kingdom
DOI10.3847/1538-4365/228/2/12
WOS KeywordMOLECULAR CLOUD CORES ; STAR-FORMING REGIONS ; INFRARED DARK CLOUDS ; 45-M RADIO TELESCOPE ; DENSE CORES ; DEUTERIUM FRACTIONATION ; CHEMICAL VARIATION ; MAPPING OBSERVATIONS ; PHYSICAL CONDITIONS ; ANGULAR-MOMENTUM
Indexed BySCI
Language英语
Funding OrganizationNational Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning(NRF-2015R1C1A1A01052160) ; National Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning(NRF-2015R1C1A1A01052160) ; Academy of Finland(285769) ; Academy of Finland(285769) ; German Research Foundation (DFG)(WA3628-1/1) ; German Research Foundation (DFG)(WA3628-1/1) ; Chinese Academy of Sciences(XDB09000000) ; Chinese Academy of Sciences(XDB09000000) ; Science and Technology Facilities Council of the United Kingdom ; Science and Technology Facilities Council of the United Kingdom ; National Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning(NRF-2015R1C1A1A01052160) ; National Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning(NRF-2015R1C1A1A01052160) ; Academy of Finland(285769) ; Academy of Finland(285769) ; German Research Foundation (DFG)(WA3628-1/1) ; German Research Foundation (DFG)(WA3628-1/1) ; Chinese Academy of Sciences(XDB09000000) ; Chinese Academy of Sciences(XDB09000000) ; Science and Technology Facilities Council of the United Kingdom ; Science and Technology Facilities Council of the United Kingdom
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000397312100002
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/8245
Collection射电天文研究部
Affiliation1.Natl Astron Observ Japan, Natl Inst Nat Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
2.SOKENDAI Grad Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
3.Korea Astron & Space Sci Inst, Daedeokdaero 776, Daejeon, South Korea
4.Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan
5.Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sect 4,Roosvelt Rd, Taipei 10617, Taiwan
6.Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England
7.Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Oxford Rd, Manchester M13 9PL, Lancs, England
8.Peking Univ, Dept Astron, Beijing 100871, Peoples R China
9.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
10.NRC, Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada
11.Univ Victoria, Dept Phys & Astron, Victoria, BC V8P IA1, Canada
12.European Southern Observ, Garching, Germany
13.Univ Toulouse 3, CNRS, IRAP, UMR5277, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France
14.Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland
15.Kagoshima Univ, Dept Phys, 1-21-35 Korimoto, Kagoshima 8900065, Japan
16.Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia
17.Natl Astron Observ Japan, Natl Inst Nat Sci, Nobeyama Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan
18.Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea
19.Eotvos Lorand Univ, Dept Astron, Pazmany Peter Setny 1, H-1117 Budapest, Hungary
20.Chinese Acad Sci, Yunnan Observ, Key Lab Struct & Evolut Celestial Objects, POB 110, Kunming 650011, Yunnan, Peoples R China
21.Chinese Acad Sci, South Amer Ctr Astrophys, Camino El Observ 1515, Santiago, Chile
22.Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile
23.Univ Electrocommun, Grad Sch Informat & Engn, Chofu, Tokyo 1828585, Japan
Recommended Citation
GB/T 7714
Tatematsu, Ken'ichi,Liu, Tie,Ohashi, Satoshi,et al. Astrochemical Properties of Planck Cold Clumps[J]. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,2017,228(2).
APA Tatematsu, Ken'ichi.,Liu, Tie.,Ohashi, Satoshi.,Sanhueza, Patricio.,Quang Nguyen Luong.,...&TRAO Key Science Program TOP Colla.(2017).Astrochemical Properties of Planck Cold Clumps.ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,228(2).
MLA Tatematsu, Ken'ichi,et al."Astrochemical Properties of Planck Cold Clumps".ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 228.2(2017).
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