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Profiling young massive stars

Published online by Cambridge University Press:  01 March 2007

Tracey Hill ,
M. G. Burton ,
M. R. Cunningham  and
V. Minier
Tracey Hill
Affiliation:
Leiden Observatory, Leiden University, PO BOX 9513, 2300RA, Leiden, the Netherlands. email: thill@strw.leidenuniv.nl School of Physics, University of New South Wales, Kensington, NSW 2052, Australia Present address: Leiden Observatory, Leiden University, PO BOX 9513, 2300RA Leiden, the Netherlands.
M. G. Burton
Affiliation:
School of Physics, University of New South Wales, Kensington, NSW 2052, Australia
M. R. Cunningham
Affiliation:
School of Physics, University of New South Wales, Kensington, NSW 2052, Australia
V. Minier
Affiliation:
Service d'Astrophysique, DAPNIA/DSM/CEA Saclay, 91191 Gif-sur-Yvette, France.
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Abstract

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We present the results of spectral energy distribution analysis for 162 of the 405 sources reported in the SIMBA survey of Hill et al. (2005). The fits reveal source specific parameters including: the luminosity, mass, temperature, H2 number density, the surface density and the luminosity-to-mass ratio. Each of these parameters are examined with respect to the four classes of source present in the sample. Obvious luminosity and temperature distinctions exist between the mm-only cores and those cores with methanol maser and/or radio continuum emission, with the former cooler and less luminous than the latter. The evidence suggests that the mm-only cores are a precursor to the methanol maser in the formation of massive stars. The mm-only cores comprise two distinct populations distinguished by temperature. Analysis and conclusions about the nature of the cool-mm and warm-mm cores comprising the mm-only population are drawn.

Keywords

masersstars: formationstars: fundamental parametersstars: early-typeradio continuum: starsmethods: data analysis
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 120 - 124
Copyright
Copyright © International Astronomical Union 2008

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