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Title:
The Influence of Far-Ultraviolet Radiation on the Properties of Molecular Clouds in the 30 Dor Region of the Large Magellanic Cloud
Authors:
Pineda, Jorge L.; Ott, Jürgen; Klein, Ulrich; Wong, Tony; Muller, Erik; Hughes, Annie
Affiliation:
AA(Argelander Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany ; Current address: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109-8099, USA. ; ), AB(National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801, USA ; Also at California Institute of Technology, 1200 E. California Blvd., Caltech Astronomy, 105-24 Pasadena, CA 91125-2400, USA. ; Jansky Fellow of the National Radio Astronomy Observatory. ), AC(Argelander Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany ), AD(School of Physics, University of New South Wales, Sydney, NSW 2052, Australia ; Also at CSIRO Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia. ; Current address: Department of Astronomy, University of Illinois, Urbana, IL 61801, USA. ), AE(Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan ; Also at CSIRO Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia. ; JSPS Fellow.), AF(Centre for Supercomputing and Astrophysics, Swinburne University of Technology, Hawthorn, VIC 3122, Australia ; Also at CSIRO Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia. )
Publication:
The Astrophysical Journal, Volume 703, Issue 1, pp. 736-751 (2009). (ApJ Homepage)
Publication Date:
09/2009
Origin:
IOP
ApJ Keywords:
galaxies: ISM, ISM: molecules, ISM: structure, Magellanic Clouds
DOI:
10.1088/0004-637X/703/1/736
Bibliographic Code:
2009ApJ...703..736P

Abstract

We present a complete 12CO J = 1 → 0 map of the prominent molecular ridge in the Large Magellanic Cloud (LMC) obtained with the 22 m ATNF Mopra Telescope. The region stretches southward by ~2° (or 1.7 kpc) from 30 Doradus, the most vigorous star-forming region in the Local Group. The location of this molecular ridge is unique insofar as it allows us to study the properties of molecular gas as a function of the ambient radiation field in a low-metallicity environment. We find that the physical properties of CO-emitting clumps within the molecular ridge do not vary with the strength of the far-ultraviolet radiation field. Since the peak CO brightness of the clumps shows no correlation with the radiation field strength, the observed constant value for CO-to-H2 conversion factor along the ridge seems to require an increase in the kinetic temperature of the molecular gas that is offset by a decrease in the angular filling factor of the CO emission. We find that the difference between the CO-to-H2 conversion factor in the molecular ridge and the outer Milky Way is smaller than has been reported by previous studies of the CO emission: applying the same cloud identification and analysis methods to our CO observations of the LMC molecular ridge and CO data from the outer Galaxy survey by Dame et al., we find that the average CO-to-H2 conversion factor in the molecular ridge is X CO sime (3.9 ± 2.5) × 1020 cm-2 (K km s-1)-1, approximately twice the value that we determine for the outer Galaxy clouds. The mass spectrum and the scaling relations between the properties of the CO clumps in the molecular ridge are similar, but not identical, to those that have been established for Galactic molecular clouds.
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