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Different Evolutionary Stages in the Massive Star-forming Complex W3 Main

Published online by Cambridge University Press:  21 March 2013

Yuan Wang
Affiliation:
Purple Mountain Observatory, 2 West Beijing Road, Nanjing 210008, China email: ywang@pmo.ac.cn MPIA
Henrik Beuther
Affiliation:
MPIA
Qizhou Zhang
Affiliation:
Harvard-Smithsonian CfA
Arjan Bik
Affiliation:
MPIA
Javier A. Rodón
Affiliation:
ESO, Chile
Zhibo Jiang
Affiliation:
Purple Mountain Observatory, 2 West Beijing Road, Nanjing 210008, China email: ywang@pmo.ac.cn
Cassandra Fallscheer
Affiliation:
University of Victoria
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Abstract

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We observed with the Submillimeter Array and IRAM 30 m telescope three high-mass star-forming regions in different evolutionary stages in the W3 high-mass star formation complex. These regions, i.e. W3 SMS1 (W3 IRS5), SMS2 (W3 IRS4) and SMS3, are located within the same large-scale environment, which allows us to study rotation and outflows as well as chemical properties in an evolutionary sense. While we find multiple mm continuum sources toward all regions, these three subregions exhibit different dynamical and chemical properties, which indicates that they are in different evolutionary stages. Even within each sub-region, massive cores of different ages are found, e.g. in SMS2, sub-sources from the most evolved UCHii region to potential starless cores exist within 30 000 AU (left panel, Fig. 1). Outflows and rotational structures are found in SMS1 and SMS2. Evidence for interactions between the molecular cloud and the HII regions is found in the 13CO channel maps (right panel, Fig. 1), which may indicate triggered star formation.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013

References

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