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Class I Methanol Maser Emission in NGC 4945

Published online by Cambridge University Press:  16 July 2018

Tiege P. McCarthy
Affiliation:
School of Physical Sciences, University of Tasmania, Hobart, Tasmania 7001, Australia email: tiegem@utas.edu.au email: simon.ellingsen@utas.edu.au Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia
Simon P. Ellingsen
Affiliation:
School of Physical Sciences, University of Tasmania, Hobart, Tasmania 7001, Australia email: tiegem@utas.edu.au email: simon.ellingsen@utas.edu.au
Xi Chen
Affiliation:
Center for Astrophysics, GuangZhou University, Guangzhou 510006, China Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China email: chenxi@shao.ac.cn
Shari L. Breen
Affiliation:
Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, NSW 2006, Australia email: shari.breen@sydney.edu.au
Maxim A. Voronkov
Affiliation:
Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia
Hai-hua Qiao
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China email: chenxi@shao.ac.cn National Time Service Center, Chinese Academy of Sciences, Xi’An, Shaanxi 710600, China email: qiaohh@shao.ac.cn
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Abstract

We have detected maser emission from the 36.2 GHz (4−1 → 30E) methanol transition towards NGC 4945. This emission has been observed in two separate epochs and is approximately five orders of magnitude more luminous than typical emission from this transition within our Galaxy. NGC 4945 is only the fourth extragalactic source observed hosting class I methanol maser emission. Extragalactic class I methanol masers do not appear to be simply highly-luminous variants of their galactic counterparts and instead appear to trace large-scale regions where low-velocity shocks are present in molecular gas.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2018 

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Class I Methanol Maser Emission in NGC 4945
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