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Confirmation of the exclusive association between 6.7-GHz methanol masers and high-mass star formation regions


Breen, SL and Ellingsen, SP and Contreras, Y and Green, JA and Caswell, JL and Stevens, JB and Dawson, JR and Voronkov, MA, Confirmation of the exclusive association between 6.7-GHz methanol masers and high-mass star formation regions, Monthly Notices of the Royal Astronomical Society, 435, (1) pp. 524-530. ISSN 0035-8711 (2013) [Refereed Article]

Copyright Statement

Copyright 2013 The Authors

DOI: doi:10.1093/mnras/stt1315


Recently, a comparison between the locations of 6.7-GHz methanol masers and dust continuum emission has renewed speculation that these masers can be associated with evolved stars. The implication of such a scenario would be profound, especially for the interpretation of large surveys for 6.7-GHz masers, individual studies where high-mass star formation has been inferred from the presence of 6.7-GHz methanol masers and for the pumping mechanisms of these masers. We have investigated the two instances where 6.7-GHz methanol masers have been explicitly suggested to be associated with evolved stars, and we find the first to be associated with a standard high-mass star formation region, and the second to be a spurious detection.We also find no evidence to suggest that the methanol maser action can be supported in the environments of evolved stars.We thereby confirm their exclusive association with high-mass star formation regions.

Item Details

Item Type:Refereed Article
Keywords:masers - stars: formation - ISM: molecules
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Cosmology and extragalactic astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Ellingsen, SP (Professor Simon Ellingsen)
UTAS Author:Dawson, JR (Dr Joanne Dawson)
ID Code:87011
Year Published:2013
Web of Science® Times Cited:92
Deposited By:Mathematics and Physics
Deposited On:2013-11-05
Last Modified:2017-11-03

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