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Title:
Submillimeter Observations of Giant Molecular Clouds in the Large Magellanic Cloud: Temperature and Density as Determined from J=3-2 and J=1-0 Transitions of CO
Authors:
Minamidani, Tetsuhiro; Mizuno, Norikazu; Mizuno, Yoji; Kawamura, Akiko; Onishi, Toshikazu; Hasegawa, Tetsuo; Tatematsu, Ken'ichi; Ikeda, Masafumi; Moriguchi, Yoshiaki; Yamaguchi, Nobuyuki; Ott, Jürgen; Wong, Tony; Muller, Erik; Pineda, Jorge L.; Hughes, Annie; Staveley-Smith, Lister; Klein, Ulrich; Mizuno, Akira; Nikolić, Silvana; Booth, Roy S.; Heikkilä, Arto; Nyman, Lars-Åke; Lerner, Mikael; Garay, Guido; Kim, Sungeun; Fujishita, Motosuji; Kawase, Tokuichi; Rubio, Monicá; Fukui, Yasuo
Affiliation:
AA(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan.; Current address: Department of Physics, Faculty of Science, Hokkaido University, N10W8, Kita-ku, Sapporo 060-0810, Japan.), AB(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan.), AC(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan.), AD(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan.), AE(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan.), AF(National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan.), AG(National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan.), AH(Research Center for the Early Universe and Department of Physics, University of Tokyo, Tokyo 113-0033, Japan.), AI(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan.), AJ(National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan.), AK(National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475.; Jansky Fellow of the National Radio Astronomy Observatory.), AL(CSIRO Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia.; Current address: Department of Astronomy, MC 221, University of Illinois, Urbana, IL 61801.), AM(CSIRO Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia.), AN(Radioastronomisches Institut der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany.), AO(CSIRO Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia.; Center for Supercomputing and Astrophysics, Swinburne University of Technology, Hawthorn, VIC 3122, Australia.), AP(School of Physics, M013, University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia.), AQ(Radioastronomisches Institut der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany.), AR(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan.; Current address: Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan.), AS(Onsala Space Observatory, 439-92 Onsala, Sweden.; Current address: Departament de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile.), AT(Onsala Space Observatory, 439-92 Onsala, Sweden.; Current address: Hartebeesthoek Radio Astronomy Observatory, P.O. Box 443, Krugersdorp 1740, South Africa.), AU(Onsala Space Observatory, 439-92 Onsala, Sweden.), AV(European Southern Observatory, Casilla 19001, Santiago 19, Chile.), AW(European Southern Observatory, Casilla 19001, Santiago 19, Chile.), AX(Departament de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile.), AY(Astronomy and Space Science Department, Sejong University, 98 Kwangjin-gu, Kunja-dong, Seoul 143-747, Korea.), AZ(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan.), BA(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan.), BB(Departament de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile.), BC(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan.)
Publication:
The Astrophysical Journal Supplement Series, Volume 175, Issue 2, pp. 485-508. (ApJS Homepage)
Publication Date:
04/2008
Origin:
UCP
ApJ Keywords:
galaxies: individual (LMC), ISM: Clouds, ISM: Molecules, Galaxies: Magellanic Clouds, Radio Lines: ISM, Submillimeter
DOI:
10.1086/524038
Bibliographic Code:
2008ApJS..175..485M

Abstract

We have carried out submillimeter 12CO(J=3-2) observations of six giant molecular clouds (GMCs) in the Large Magellanic Cloud (LMC) with the ASTE 10 m submillimeter telescope at a spatial resolution of 5 pc and very high sensitivity. We have identified 32 molecular clumps in the GMCs and revealed significant details of the warm and dense molecular gas with n(H2)~103-105 cm-3 and Tkin~60 K. These data are combined with 12CO(J=1-0) and 13CO(J=1-0) results and compared with LVG calculations. The results indicate that clumps that we detected are distributed continuously from cool (~10-30 K) to warm (>~30-200 K), and warm clumps are distributed from less dense (~103 cm-3) to dense (~103.5-105 cm-3). We found that the ratio of 12CO(J=3-2) to 12CO(J=1-0) emission is sensitive to and is well correlated with the local Hα flux. We infer that differences of clump properties represent an evolutionary sequence of GMCs in terms of density increase leading to star formation. Type I and II GMCs (starless GMCs and GMCs with H II regions only, respectively) are at the young phase of star formation where density does not yet become high enough to show active star formation, and Type III GMCs (GMCs with H II regions and young star clusters) represent the later phase where the average density is increased and the GMCs are forming massive stars. The high kinetic temperature correlated with Hα flux suggests that FUV heating is dominant in the molecular gas of the LMC.
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