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Ultra-precise monitoring of a class I methanol maser

Published online by Cambridge University Press:  07 February 2024

M. A. Voronkov Open the ORCID record for M. A. Voronkov [Opens in a new window] ,
S. L. Breen ,
S. P. Ellingsen Open the ORCID record for S. P. Ellingsen [Opens in a new window] ,
J. A. Green ,
A. M. Sobolev ,
S. Yu. Parfenov  and
D. J. van der Walt
M. A. Voronkov*
Affiliation:
CSIRO Space & Astronomy, PO Box 76, Epping, NSW 1710, Australia.
S. L. Breen
Affiliation:
SKAO, Jodrell Bank, Lower Withington, Macclesfield, Cheshire SK11 9FT, UK
S. P. Ellingsen
Affiliation:
School of Natural Sciences, University of Tasmania, Private Bag 37, Hobart, Tasmania 7001, Australia
J. A. Green
Affiliation:
SKAO, SKA-LOW Science Operations Centre, ARRC Building, 26 Dick Perry Avenue, Technology Park, Kensington WA 6151 Australia
A. M. Sobolev
Affiliation:
Ural Federal University, 19 Mira street, 620002 Ekaterinburg, Russia
S. Yu. Parfenov
Affiliation:
Ural Federal University, 19 Mira street, 620002 Ekaterinburg, Russia
D. J. van der Walt
Affiliation:
Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
*
email: Maxim.Voronkov@csiro.au
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Abstract

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We report the results of a 7-year monitoring program using the Australia Telescope Compact Array (ATCA) for the 9.9 GHz class I methanol maser in G331.13-0.24 where a periodic class II methanol maser is present. The great deal of the project was to control systematics at an unprecedented level. Although no periodic flux variation was found, the maser shows a very stable decline of 166±7 μJy/day. The radial velocity of the maser is stable down to 1 m/s level. We also report a marginal periodic signal in radial velocity (comparable to the level of systematics) of about 20±7 cm/s with the period of 475±22 days, close to that of the 6.7-GHz maser in the source. No hyperfine split was detected which suggests preferential excitation of a single hyperfine transition.

Keywords

masersstars: formationHii regions
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S380: Cosmic Masers: Proper Motion toward the Next-Generation Large Projects , December 2022 , pp. 255 - 257
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution and reproduction, provided the original article is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Belov, S. P., Golubiatnikov, G. Yu., Lapinov, A. V. et al. 2016, J. Chem. Phys., 145, 024307CrossRefGoogle Scholar
Goedhart, S., Maswanganye, J. P., Gaylard, M. J., van der Walt, D. J. 2014, MNRAS, 437, 1808 CrossRefGoogle Scholar
Parfenov, S., Yu., Sobolev, A. M. 2014, MNRAS, 444, 620CrossRefGoogle Scholar
Voronkov, M. A., Caswell, J. L., Ellingsen, S. P., et al. 2014, MNRAS, 439, 2584 CrossRefGoogle Scholar
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