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The molecular environment of massive star forming cores associated with Class II methanol maser emission

Published online by Cambridge University Press:  01 March 2007

S. N. Longmore ,
M. G. Burton ,
P. J. Barnes ,
T. Wong ,
C. R. Purcell  and
J. Ott
S. N. Longmore
Affiliation:
School of Physics, University of New South Wales, Kensington, NSW 2052, Sydney, Australia Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia E-mail: snl@phys.unsw.edu.au
M. G. Burton
Affiliation:
School of Physics, University of New South Wales, Kensington, NSW 2052, Sydney, Australia
P. J. Barnes
Affiliation:
School of Physics A28, University of Sydney, NSW 2006, Australia
T. Wong
Affiliation:
School of Physics, University of New South Wales, Kensington, NSW 2052, Sydney, Australia Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia Department of Astronomy, University of Illinois, Urbana IL 61801, USA
C. R. Purcell
Affiliation:
School of Physics, University of New South Wales, Kensington, NSW 2052, Sydney, Australia University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL, UK
J. Ott
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
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Abstract

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Methanol maser emission has proven to be an excellent signpost of regions undergoing massive star formation (MSF). To investigate their role as an evolutionary tracer, we have recently completed a large observing program with the ATCA to derive the dynamical and physical properties of molecular/ionised gas towards a sample of MSF regions traced by 6.7GHz methanol maser emission. We find that the molecular gas in many of these regions breaks up into multiple sub-clumps which we separate into groups based on their association with/without methanol maser and cm continuum emission. The temperature and dynamic state of the molecular gas is markedly different between the groups. Based on these differences, we attempt to assess the evolutionary state of the cores in the groups and thus investigate the role of class II methanol masers as a tracer of MSF.

Keywords

stars: formationISM: evolutionISM: moleculesline: profilesmasersmolecular datastars: early-typeradio continuum: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 125 - 129
Copyright
Copyright © International Astronomical Union 2008

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