YNAO OpenIR  > 大样本恒星演化研究组
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 JH(何金华)20,21,22; Sakai, Takeshi23; Kim, Jungha18; JCMT Large Program SCOPE Collabora; TRAO Key Science Program TOP Colla
Source PublicationASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
2017-02-01
Volume228Issue:2
DOI10.3847/1538-4365/228/2/12
Contribution Rank第20完成单位
Indexed BySCI
KeywordIsm: Clouds Ism: Molecules Ism: Structure Stars: Formation
Abstract

We 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.

Funding ProjectNational Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning[NRF-2015R1C1A1A01052160] ; Academy of Finland[285769] ; German Research Foundation (DFG)[WA3628-1/1] ; Chinese Academy of Sciences[XDB09000000] ; Science and Technology Facilities Council of the United Kingdom
Funding OrganizationNational Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning[NRF-2015R1C1A1A01052160] ; Academy of Finland[285769] ; German Research Foundation (DFG)[WA3628-1/1] ; Chinese Academy of Sciences[XDB09000000] ; Science and Technology Facilities Council of the United Kingdom
Language英语
Subject Area天文学 ; 恒星与银河系
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0067-0049
URL查看原文
WOS IDWOS:000397312100002
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
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
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/9988
Collection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
Corresponding AuthorTatematsu, Ken'ichi
Affiliation1.National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
2.Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
3.Korea Astronomy and Space Science Institute, Daedeokdaero 776, Yuseong, Daejeon 305-348, Korea
4.Department of Astronomy, The University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
5.Academia Sinica Institute of Astronomy and Astrophysics, 11F of Astronomy-Mathematics Building, AS/NTU. No.1, Section 4, Roosevelt Rd, Taipei 10617, Taiwan, R.O.C.
6.Centre for Astrophysics Research, Science & Technology Research Institute, University of Hertfordshire, Hatfield, AL10 9AB, UK
7.Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester, M13 9PL, UK
8.Department of Astronomy, Peking University, 100871, Beijing, China
9.National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China
10.NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
11.Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 1A1, Canada
12.European Southern Observatory, Germany
13.IRAP, CNRS (UMR5277), Universite Paul Sabatier, 9 avenue du Colonel Roche, BP 44346, F-31028, Toulouse Cedex 4, France
14.Department of physics, University of Helsinki, FI-00014, Helsinki, Finland
15.Department of Physics, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, Japan
16.School of Physics, University of New South Wales, Sydney, NSW 2052, Australia
17.Nobeyama Radio Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Nobeyama, Minamimaki, Minamisaku, Nagano 384-1305, Japan
18.School of Space Research, Kyung Hee University, Seocheon-Dong, Giheung-Gu, Yongin-Si, Gyeonggi-Do, 446-701, Korea
19.Department of Astronomy, Eötvös Loránd Unviersity, Pázmany Péter sétny 1, 1117 Budapest, Hungary
20.Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, Kunming, 650011, Yunnan Province, China
21.Chinese Academy of Sciences, South America Center for Astrophysics (CASSACA), Camino El Observatorio 1515, Las Condes, Santiago, Chile
22.Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
23.Graduate School of Informatics and Engineering, The University of Electro-Communications, Chofu, Tokyo 182-8585, 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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