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Variability of Methanol Masers

Published online by Cambridge University Press:  25 April 2016

J. L. Caswell ,
R. A. Vaile  and
S.P. Ellingsen
J. L. Caswell
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 2121, Australia jcaswell@rp.csiro.au
R. A. Vaile
Affiliation:
Department of Physics, Faculty of Business & Technology, University of Western Sydney, Macarthur, PO Box 555, Campbelltown, NSW 2560, Australia
S.P. Ellingsen
Affiliation:
Physics Department, University of Tasmania, GPO Box 252C, Hobart, Tas. 7001, Australia
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Abstract

Sites of recent star formation often radiate strong maser emission from methanol transitions near 6-6 and 12 GHz. We have studied many of these masers over several years and find that intensity variations are common on both transitions. We present observations which demonstrate marked variability in 48 sources. We explore the characteristics of the variability and find it to be typically quasi-periodic, on a timescale of between a month and several years. The amplitude of the variation is most commonly less than a factor of two, but can reach factors of ten. The variability of different features in a source is usually independent. Variability of features seen at both 6·6 and 12 GHz is sometimes correlated, with larger amplitudes usually seen at 12 GHz. A likely inference is that variations are occasionally due to a change in the pump rate throughout the masing region, but most are consistent with a change in the masing path length due to large-scale motions. In addition, it is likely that the majority of 6·6-GHz masers are saturated whereas the 12-GHz masers may be somewhat less saturated.

Keywords

masers — starsformation — ISMmoleculesradio linesISM
Type
Gallactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 12 , Issue 1 , April 1995 , pp. 37 - 53
Copyright
Copyright © Astronomical Society of Australia 1995

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References

Caswell, J. L., Gardner, F. F., Norris, R. P., Wellington, K.J., McCutcheon, W. H., & Peng, R.S. 1993, MNRAS, 260, 425 Google Scholar
Caswell, J. L., Vaile, R. A., Ellingsen, S. E., Whiteoak, J.B., & Norris, R. P. 1995a, MNRAS, 272, 96 Google Scholar
Caswell, J. L., Vaile, R. A., Ellingsen, S. E., & Norris, R.P. 1995b, MNRAS, in pressGoogle Scholar
Chapman, J. M., te Lintel Hekkert, P., Killeen, N. E.B., Caswell, J. L., & Harnett, J. I. 1993, in Astrophysical Masers, Springer Lecture Notes in Physics Vol. 412, ed. Clegg, A. & Nedoluha, G. (Berlin: Springer) 345 Google Scholar
Cragg, D. M., Johns, K. P., Godfrey, P. D., & Brown, R.D. 1992, MNRAS, 259, 203 Google Scholar
Gaines, L., Casleton, K. H., & Kukolich, S. G. 1974, ApJ, 191, L99 Google Scholar
Menten, K. M. 1991a, in Skylines: Proceedings of 3rd Haystack Observatory Meeting, ASP Conf. Ser., Vol. 16, ed. Haschick, A. D. & Ho, P. T. (San Francisco: ASP), 119 Google Scholar
Menten, K. M. 1991b, ApJ, 380, L75 Google Scholar
Norris, R. P., Whiteoak, J.B., Caswell, J. L., Wieringa, M.H., & Gough, R. G. 1993, ApJ, 412, 222 Google Scholar
Peng, R. S. 1989a, A&A, 216, 165 Google Scholar
Peng, R. S. 1989b, A&A, 216, 173 Google Scholar