EDP Sciences
Free access
Volume 429, Number 3, January III 2005
Page(s) 945 - 960
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20041137

A&A 429, 945-960 (2005)
DOI: 10.1051/0004-6361:20041137

Star-forming protoclusters associated with methanol masers

V. Minier1, 2, M. G. Burton2, T. Hill2, M. R. Pestalozzi3, C. R. Purcell2, G. Garay4, A. J. Walsh5 and S. Longmore2

1  Service d'Astrophysique, DAPNIA/DSM/CEA CE de Saclay, 91191 Gif-sur-Yvette, France
    e-mail: Vincent.Minier@cea.fr
2  School of Physics, University of New South Wales, Sydney 2052, NSW, Australia
3  Onsala Space Observatory, 439 92 Onsala, Sweden
4  Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
5  Center for Astrophysics, 60 Garden Street, Cambridge, MA, 02138, USA

(Received 21 April 2004 / Accepted 16 September 2004 )

We present a multiwavelength study of five methanol maser sites which are not directly associated with a strong ( >100 mJy) radio continuum source: G 31.28+0.06, G 59.78+0.06, G 173.49+2.42 (S231, S233IR), G 188.95+0.89 (S252, AFGL5180) and G 192.60-0.05 (S255IR). These radio-quiet methanol maser sites are often interpreted as precursors of ultra-compact $\ion{H}{ii}$ regions or massive protostar sites. In this work, the environment of methanol masers is probed from mid-IR to millimetre wavelengths at angular resolutions of 8''-34''. Spectral energy distribution (SED) diagrams for each site are presented, together with mass and luminosity estimates. Each radio-quiet maser site is always associated with a massive ( >50  $M_{\odot}$), deeply embedded ( $A_{\rm v}>40$ mag) and very luminous ( > 104  $L_{\odot}$) molecular clump, with $L_{\rm total}\propto M_{\rm gas}^{0.75}$. These physical properties characterise massive star-forming clumps in earlier evolutionary phases than $\ion{H}{ii}$ regions. In addition, colder gas clumps seen only at mm-wavelengths are also found near the methanol maser sites. These colder clumps may represent an even earlier phase of massive star formation. These results suggest an evolutionary sequence for massive star formation from a cold clump, seen only at mm wavelengths, evolving to a hot molecular core with a two-component SED with peaks at far-IR and mid-IR wavelengths, to an (ultra-compact) $\ion{H}{ii}$ region. Alternatively, the cold clumps might be clusters of low-mass YSOs, in formation near the massive star-forming clusters. Finally, the values of the dust grain emissivity index ( $\beta$) range between 1.6 and 1.9.

Key words: masers -- stars: formation -- ISM: dust, extinction

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© ESO 2005

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