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Anatomy of the S255–S257 complex – triggered high-mass star formation

Published online by Cambridge University Press:  01 August 2006

V. Minier ,
N. Peretto ,
S. N. Longmore ,
M. G. Burton ,
R. Cesaroni ,
C. Goddi ,
M. R. Pestalozzi  and
Ph. André
V. Minier
Affiliation:
SAp/DAPNIA/DSM & UMR AIM, CEA Saclay, 91191 Gif-sur-Yvette, France email: vincent.minier@cea.fr
N. Peretto
Affiliation:
Department of Physics & Astronomy, University of Manchester, Manchester, UK
S. N. Longmore
Affiliation:
School of Physics, University of New South Wales, Sydney, Australia
M. G. Burton
Affiliation:
School of Physics, University of New South Wales, Sydney, Australia
R. Cesaroni
Affiliation:
INAF, Osservatorio Astrofisico di Arcetri, Firenze, Italy
C. Goddi
Affiliation:
INAF, Osservatorio Astrofisico di Arcetri, Firenze, Italy
M. R. Pestalozzi
Affiliation:
School of Physics, Astronomy & Maths, University of Hertfordshire, Hatfield, UK
Ph. André
Affiliation:
SAp/DAPNIA/DSM & UMR AIM, CEA Saclay, 91191 Gif-sur-Yvette, France email: vincent.minier@cea.fr
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Abstract

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We present a multi-wavelength (NIR to radio) and multi-scale (1 AU to 10 pc) study of the S255–S257 complex of young high-mass (proto)stars. The complex consists of two evolved HII regions and a molecular gas filament in which new generations of high mass stars form. Four distinct regions are identified within this dusty filament: a young NIR/optical source cluster, a massive protostar binary, a (sub)millimetre continuum and molecular clump in global collapse and a reservoir of cold gas. Interestingly, the massive binary protostellar system is detected through methanol maser and mid-IR emission at the interface between the NIR cluster and the cold gas filament. The collapsing clump is located to the north of the NIR cluster and hosts a young high-mass star associated with an outflow that is observed in mid-IR, methanol maser and radio emission. We interpret this anatomy as the possible result of triggered star formation, starting with the formation of two HII regions, followed by the compression of a molecular gas filament in which a first generation of high-mass stars forms (the NIR cluster), which then triggers the formation of high mass protostars in its near environment (the massive protostellar binary). The global collapse of the northern clump might be due to both the expansion of the HII regions that squashes the filament. In conclusion, we witness the formation of four generations of clusters of high-mass stars in S255–S257.

Keywords

stars: formationISM: cloudsHII regionsmethods: data analysis
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 160 - 164
Copyright
Copyright © International Astronomical Union 2007

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