EDP Sciences
Free Access
Volume 434, Number 2, May I 2005
Page(s) 613 - 621
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361:20042437
Published online 11 April 2005

A&A 434, 613-621 (2005)
DOI: 10.1051/0004-6361:20042437

Masers as signposts of high-mass protostars

A water maser survey of methanol maser sources
M. Szymczak1, T. Pillai2 and K. M. Menten2

1  Torun Centre for Astronomy, Nicolaus Copernicus University, Gagarina 11, 87100 Torun, Poland
    e-mail: msz@astro.uni.torun.pl
2  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

(Received 26 November 2004 / Accepted 31 December 2004 )

The 22 GHz H2O maser line was observed towards 79 candidate high-mass protostellar objects from a flux-limited sample of 6.7 GHz methanol sources. The emission was detected in 41 sources, towards 28 of these for the first time. The detection rate of 52% was similar to rates reported for other samples of high-mass protostars selected mainly with far-infrared (FIR) colour criteria. The median value of H2O maser luminosity of $10^{-5.5}~L_{\odot}$ is equal to that of the CH3OH maser luminosity, whereas the median OH maser luminosity was found to be ~1.5 orders of magnitude lower. Comparison of the velocity ranges showing maser emission implies that for the majority of sources the H2O and CH3OH maser lines originate from different regions. The percentage of sources with emission in two or three of the maser species, their association with radio continuum and IR emission and the maser and IR luminosities are consistent with the view that evolutionary phases with H2O and CH3OH masers largely overlap and precede the OH maser phase, while at a later stage OH and CH3OH masers may coexist. Strong correlations of OH and CH3OH maser luminosities with IR luminosity and only a marginal correlation of H2O and IR luminosity confirm current pumping schemes of all three maser lines.

Key words: masers - stars: formation - ISM: molecules - radio lines: ISM - HII regions

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© ESO 2005

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