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Expansion of methanol maser rings

Published online by Cambridge University Press:  16 July 2018

Anna Bartkiewicz
Affiliation:
Centre for Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziadzka 5, 87-100 Torun, Poland email: annan@astro.umk.pl
Alberto Sanna
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121, Bonn, Germany email: asanna@mpifr-bonn.mpg.de
Marian Szymczak
Affiliation:
Centre for Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziadzka 5, 87-100 Torun, Poland email: annan@astro.umk.pl
Luca Moscadelli
Affiliation:
INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Firenze, Italy email: mosca@arcetri.astro.it
Huib van Langevelde
Affiliation:
Joint Institute for VLBI ERIC (JIVE), Postbus 2, 7990 AA Dwingeloo, The Netherlands email: langevelde@jive.eu Sterrewacht Leiden, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands
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Abstract

Ring−like sources of 6.7 GHz methanol maser emission were discovered a decade ago with the European VLBI Network. In the past years we have been incessantly working to understand the nature of these rings. In general, the methanol rings do not coincide with H II regions nor they show 22 GHz water maser emission. Here, we present a proper motion study over a time baseline up to 10.5 years for the first sub-sample of methanol maser rings. Our findings suggest that in three targets G23.207−00.377, G23.389+00.185, and G23.657−00.127, such rings form in outflows or even in winds close to the central sources, and the masers trace slow proper motions of a few km s−1 typically.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2018 

References

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