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Investigating high-mass star formation through maser surveys

Published online by Cambridge University Press:  01 March 2007

S. P. Ellingsen ,
M. A. Voronkov ,
D. M. Cragg ,
A. M. Sobolev ,
S. L. Breen  and
P. D. Godfrey
S. P. Ellingsen
Affiliation:
School of Mathematics and Physics, University of Tasmania, Private Bag 21, Hobart 7001, TAS, Australia email: [email protected]
M. A. Voronkov
Affiliation:
Australia Telescope National Facility CSIRO, PO Box 76, Epping 1710, NSW, Australia
D. M. Cragg
Affiliation:
School of Chemistry, Building 23, Monash University, Victoria 3800, Australia
A. M. Sobolev
Affiliation:
Ural State University, Lenin ave. 51, 620083 Ekaterinburg, Russia
S. L. Breen
Affiliation:
School of Mathematics and Physics, University of Tasmania, Private Bag 21, Hobart 7001, TAS, Australia email: [email protected]
P. D. Godfrey
Affiliation:
School of Chemistry, Building 23, Monash University, Victoria 3800, Australia
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Abstract

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Interstellar masers are unique probes of the environments in which they arise. In studies of high-mass star formation their primary function has been as signposts of these regions and they have been used as probes of the kinematics and physical conditions in only a few sources. With a few notable exceptions, we know relatively little about the evolutionary phase the different maser species trace, nor their location with respect to other star formation tracers. While detailed studies of a small number of maser regions can reveal much about them, other information can only be obtained through large, systematic searches. In particular, such surveys are vital in efforts to determine an evolutionary sequence for the common maser species, and there is growing evidence that methanol masers may trace an earlier phase than the other common maser species of OH and water.

Keywords

stars: formationMasersSurveys
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 213 - 217
Copyright
Copyright © International Astronomical Union 2008

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