Warm and Dense Molecular Gas in the N 159 Region: 12CO J = 4–3 and 13CO J = 3–2 Observations with NANTEN2 and ASTE

Publications of the Astronomical Society of Japan

Pineda, Jorge L.^6,8  Stutzki, Jürgen¹  Burton, Michael¹¹  Indebetouw, Remy¹²  Ezawa, Hajime^8,14  Meixner, Margaret²¹  Klein, Uli¹⁹  Wong, Tony^5,8  Kohno, Kotaro^9,20  Yamamoto, Hiroaki¹⁸  Koo, Bon-Chul^9,17  Mizuno, Norikazu¹⁶  Kawamura, Akiko¹⁸  Ott, Jürgen^4,8  Rubio, Monica^8,10  Minamidani, Tetsuhiro^8,15  Tatematsu, Ken’ichi^8,14  Hasegawa, Tetsuo^8,14  Ikeda, Masafumi^8,14  Hughes, Annie^3,8  Onishi, Toshikazu⁸  Hayakawa, Takahiro¹⁸  Bernard, Jean-Philippe^8,13  Fukui, Yasuo¹⁸  Mizuno, Akira^2,8  Bertoldi, Frank¹⁹  Whitney, Barbara⁹  Mizuno, Yoji¹⁸  Yamaguchi, Nobuyuki^8,14  Gordon, Karl D.²¹  Muller, Erik¹⁸  Benz, Arnold^7,8 

[1] KOSMA, I. Physikalisches Institut, Universität zu Köln, Zülpicher Straße 77, 50937 Köln, Germany.;Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601;CSIRO Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, AustraliaCenter for Supercomputing and Astrophysics, Swinburne University of Technology, Hawthorn, VIC 3122, Australia;National Radio Astronomy Observatory, PO Box O, Socorro, NM 87801-0387, USACalifornia Institute of Technology, 1200 E. California Blvd., Caltech Astronomy, 105-24 Pasadena, CA 91125-2400, USA;Department of Astronomy, University of Illinois, 1002 W. Green St., Urbana, IL 61801, USA;Jet Propulsion Laboratory, M/S 169-507, 4800 Oak Grove Drive, Pasadena, CA 91109, USA;Institute of Astronomy, ETH Zürich, 8093 Zürich, Switzerland.;Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602 y , Department of Physical Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai 599-8531;Space Science Institute, 4750 Walnut St., Suite 205, Boulder, CO 80301, USA;Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile;School of Physics, University of New South Wales, Sydney 2052, NSW, Australia;Department of Astronomy, University of Virginia, PO Box 400325, Charlottesville, VA 22903, USANational Radio Astronomy Observatory, 520 Edgemont Rd., Charlottesville, VA 22903, USA;CESR, 9 Avenue du Colonel Roche, BP 44346, 31028 Toulouse cedex 4, France;National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588;Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602 y , Department of Physics, Faculty of Science, Hokkaido University, Kita 10, Nishi 8, Kita-ku, Sapporo 060-0810;Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602 y , National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588;Seoul National University, Seoul 151-742, Korea.;Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602 y ,;Argelander-Institut für Astronomie, Auf dem Hügel 71, 53121 Bonn, Germany.;Institute of Astronomy, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015;Space Telescope Science Institute, 3700 San Martin Way, Baltimore, MD 21218, USA

关键词: "galaxies: Magellanic Clouds";    "ISM: clouds";    "ISM: molecules";    "stars: formation";    submillimeter;   

DOI  :  10.1093/pasj/62.1.51

学科分类：天文学(综合)

来源: Oxford University Press

【 摘 要 】

New$$^{12}$$CO$$J=$$4–3and$$^{13}$$CO$$J=$$3–2observationsoftheN159region,anactivesiteofmassivestarformationintheLargeMagellanicCloud,havebeenmadewiththeNANTEN2andASTEsubmillimetertelescopes,respectively.The$$^{12}$$CO$$J=$$4–3distributionisseparatedintothreeclumps,eachassociatedwithN159W,N159E,andN159S.Thesenewmeasurementstowardthethreeclumpsareusedincoupledcalculationsofmolecularrotationalexcitationandlineradiationtransfer,alongwithothertransitionsofthe$$^{12}$$CO$$J=$$1–0,$$J=$$2–1,$$J=$$3–2,and$$J=$$7–6aswellastheisotopetransitionsof$$^{13}$$CO$$J=$$1–0,$$J=$$2–1,$$J=$$3–2,and$$J=$$4–3.The$$^{13}$$CO$$J=$$3–2datawerenewlytakenforthepresentwork.Thetemperaturesanddensitieswerefoundtobe$$sim$$70amp;x2013;80Kand$$sim$$3$$imes$$10$$^{3}$$cm$$^{-3}$$inN159WandN159E,and$$sim$$30Kand$$sim$$1.6$$imes$$10$$^{3}$$cm$$^{-3}$$inN159S.Theseresultswerecomparedwiththestar-formationactivitybasedondataofyoungstellarclustersandHIIregionsaswellasmidinfraredemissionobtainedwiththeSpitzerMIPS.TheN159Eclumpisassociatedwithcluster(s)embedded,asobservedat24$$mu$$mbytheSpitzerMIPS,andthederivedhightemperature,80K,isinterpretedasbeingheatedbythesesources.TheN159EclumpislikelytoberesponsibleforadarklaneinalargeHIIregionbydustextinction.Ontheotherhand,theN159Wclumpisassociatedwithclustersembeddedmainlytowardtheeasternedgeoftheclumponly.Theseclustersshowoffsetsof20$${}^{primeprime}$$–40$${}^{primeprime}$$fromthe$$^{12}$$CO$$J=$$4–3peak,andareprobablyresponsibleforheatingindicatedbythederivedhightemperature,70K.TheN159Wclumpexhibitsnosignofstarformationtowardthe$$^{12}$$CO$$J=$$4–3peakpositionanditswesternregionthatshowsenhanced$$R_{4-3/1-0}$$and$$R_{3-2/1-0}$$ratios.WethereforesuggestthattheN159Wpeakrepresentsapre-star-clustercoreof$$sim$$10$$^{5}M_{odot}$$whichdeservesfurtherdetailedstudies.TheN159Sclumpshowslittlesignofstarformation,asisconsistentwiththelowertemperature,30K,andhasasomewhatlowerdensitythanN159WandN159E.TheN159Sclumpisalsoacandidateforfuturestarformation.

【 授权许可】

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