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Water masers within the G 333.2–0.6 giant molecular cloud

Published online by Cambridge University Press:  01 March 2007

S. L. Breen ,
S. P. Ellingsen ,
M. Johnston-Hollitt ,
S. Wotherspoon ,
I. Bains ,
M. G. Burton ,
M. Cunningham ,
N. Lo ,
C. E. Senkbeil  and
T. Wong
S. L. Breen
Affiliation:
School of Mathematics and Physics, University of Tasmania, Private Bag 37, Hobart, Tasmania 7001, Australia
S. P. Ellingsen
Affiliation:
School of Mathematics and Physics, University of Tasmania, Private Bag 37, Hobart, Tasmania 7001, Australia
M. Johnston-Hollitt
Affiliation:
School of Mathematics and Physics, University of Tasmania, Private Bag 37, Hobart, Tasmania 7001, Australia
S. Wotherspoon
Affiliation:
School of Mathematics and Physics, University of Tasmania, Private Bag 37, Hobart, Tasmania 7001, Australia
I. Bains
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia
M. G. Burton
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia
M. Cunningham
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia
N. Lo
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia
C. E. Senkbeil
Affiliation:
School of Mathematics and Physics, University of Tasmania, Private Bag 37, Hobart, Tasmania 7001, Australia
T. Wong
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia Australia telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia
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Abstract

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We report the results of a blind search for 22 GHz water masers in two regions, covering approximately half a square degree, within the G 333.2–0.6 giant molecular cloud. The complete search of the two regions was carried out with the 26 m Mount Pleasant radio telescope and resulted in the detection of nine water masers, five of which are new detections. Australia Telescope Compact Array (ATCA) observations of these detections have allowed us to obtain positions with arcsecond accuracy, allowing meaningful comparison with infrared and molecular data for the region. We find that for the regions surveyed there are more water masers than either 6.7 GHz methanol, or main-line OH masers. The water masers are concentrated towards the central axis of the star formation region, in contrast to the 6.7 GHz methanol masers which tend to be located near the periphery. The colours of the GLIMPSE point sources associated with the water masers are slightly less red than those associated with methanol masers. Statistical investigation of the properties of the 13CO and 1.2 mm dust clumps with and without associated water masers shows that the water masers are associated with the more massive, denser and brighter 13CO and 1.2 mm dust clumps. We present statistical models that can predict those 13CO and 1.2 mm dust clumps likely to have associated water masers.

Keywords

MasersISM: moleculesradio lines: generalstars: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 144 - 145
Copyright
Copyright © International Astronomical Union 2008

References

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