Hostname: page-component-78c5997874-t5tsf Total loading time: 0 Render date: 2024-11-14T06:35:46.934Z Has data issue: false hasContentIssue false
  • English
  • Français

Molecular cloud structure and star formation in the W43 complex

Published online by Cambridge University Press:  05 March 2015

P. Carlhoff ,
P. Schilke ,
F. Motte  and
Q. Nguyen Luong
P. Carlhoff
Affiliation:
1. Physikalisches Institut, Universität zu Köln, Germany email: carlhoff@ph1.uni-koeln.de
P. Schilke
Affiliation:
1. Physikalisches Institut, Universität zu Köln, Germany email: carlhoff@ph1.uni-koeln.de
F. Motte
Affiliation:
Laboratoire AIM, CEA/IRFU – CNRS/INSU – Université Paris Diderot, France
Q. Nguyen Luong
Affiliation:
Canadian Institute for Theoretical Astrophysics – CITA, University of Toronto, Canada
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The W43 region is one of the most massive star forming regions in our Galaxy. It is subject to a large IRAM 30m project that observes high spectral resolution maps of the complete complex in the 13CO (2–1) and C18O (2–1) lines. We find a variety of different sources of which we calculate excitation temperature, H2 column density and mass. We find the total mass of dense clouds in the complex to be 1.2×106 M⊙.

Keywords

ISM: moleculesISM: structureISM: kinematics and dynamicsmolecular data
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Highlights H16: Highlights of Astronomy , August 2012 , pp. 592
Copyright
Copyright © International Astronomical Union 2015 

References

Nguyen Luong, Q., Motte, F., Schuller, F., et al. 2011, A&A 529, A41Google Scholar
Schuller, F., Menten, K. M., Contreras, Y., et al. 2009, A&A 504, 415Google Scholar