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New class I methanol masers

Published online by Cambridge University Press:  24 July 2012

M. A. Voronkov ,
J. L. Caswell ,
S. P. Ellingsen ,
S. L. Breen ,
T. R. Britton ,
J. A. Green ,
A. M. Sobolev  and
A. J. Walsh
M. A. Voronkov
Affiliation:
CSIRO Astronomy and Space Science, PO Box 76, Epping NSW 1710, Australia Astro Space Centre, Profsouznaya st. 84/32, 117997 Moscow, Russia
J. L. Caswell
Affiliation:
CSIRO Astronomy and Space Science, PO Box 76, Epping NSW 1710, Australia
S. P. Ellingsen
Affiliation:
School of Mathematics and Physics, University of Tasmania, GPO Box 252-37, Hobart, Tasmania 7000, Australia
S. L. Breen
Affiliation:
CSIRO Astronomy and Space Science, PO Box 76, Epping NSW 1710, Australia
T. R. Britton
Affiliation:
CSIRO Astronomy and Space Science, PO Box 76, Epping NSW 1710, Australia Macquarie University, Department of Physics and Engineering, NSW 2109, Australia
J. A. Green
Affiliation:
CSIRO Astronomy and Space Science, PO Box 76, Epping NSW 1710, Australia
A. M. Sobolev
Affiliation:
Ural State University, Lenin ave. 51, 620083 Ekaterinburg, Russia
A. J. Walsh
Affiliation:
Centre for Astronomy, School of Engineering and Physical Sciences, James Cook University, Townsville, QLD 4814, Australia
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Abstract

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We review properties of all known collisionally pumped (class I) methanol maser series based on observations with the Australia Telescope Compact Array (ATCA) and the Mopra radio telescope. Masers at 36, 84, 44 and 95 GHz are most widespread, while 9.9, 25, 23.4 and 104 GHz masers are much rarer, tracing the most energetic shocks. A survey of many southern masers at 36 and 44 GHz suggests that these two transitions are highly complementary. The 23.4 GHz maser is a new type of rare class I methanol maser, detected only in two high-mass star-forming regions, G357.97-0.16 and G343.12-0.06, and showing a behaviour similar to 9.9, 25 and 104 GHz masers. Interferometric positions suggest that shocks responsible for class I masers could arise from a range of phenomena, not merely an outflow scenario. For example, some masers might be caused by interaction of an expanding Hii region with its surrounding molecular cloud. This has implications for evolutionary sequences incorporating class I methanol masers if they appear more than once during the evolution of the star-forming region. We also make predictions for candidate maser transitions in the ALMA frequency range.

Keywords

masers – ISM: molecules – ISM: jets and outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S287: Cosmic Masers - from OH to H0 , January 2012 , pp. 433 - 440
Copyright
Copyright © International Astronomical Union 2012

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