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A search for OH 6 GHz maser emission towards southern supernova remnants

Published online by Cambridge University Press:  01 March 2007

Korinne E. McDonnell ,
Alan E. Vaughan  and
Mark Wardle
Korinne E. McDonnell
Affiliation:
Department of Physics, Macquarie University, Sydney, NSW 2109, Australia email: korinnem@physics.mq.edu.au, alanv@physics.mq.edu.au, wardle@physics.mq.edu.au
Alan E. Vaughan
Affiliation:
Department of Physics, Macquarie University, Sydney, NSW 2109, Australia email: korinnem@physics.mq.edu.au, alanv@physics.mq.edu.au, wardle@physics.mq.edu.au
Mark Wardle
Affiliation:
Department of Physics, Macquarie University, Sydney, NSW 2109, Australia email: korinnem@physics.mq.edu.au, alanv@physics.mq.edu.au, wardle@physics.mq.edu.au
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Abstract

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OH masers at 1720 MHz have proven to be excellent indicators of interactions between supernova remnants and molecular clouds. Recent calculations suggest that the 6049 MHz OH maser line is excited at higher column densities than for the 1720 MHz line. It is therefore a potentially valuable indicator of remnant-cloud interaction.

We present preliminary results of a survey using the Parkes Methanol Multibeam receiver for 6049 MHz and 6035/6030 MHz OH masers towards 36 supernova remnants and four fields in the Large and Small Magellanic Clouds. While no 6049 MHz masers have been found, three new sites of 6035 and 6030 MHz OH maser emission have been discovered in star-forming regions.

Keywords

supernova remnantsmasersstars: formationradio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 232 - 233
Copyright
Copyright © International Astronomical Union 2008

References

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