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Evidence for the non-destruction of the Most Massive Molecular Clouds even after they have given Birth to Massive Star Clusters

Published online by Cambridge University Press:  31 March 2017

J. Zaragoza-Cardiel ,
J. Beckman ,
J. Font ,
A. Camps-Fariña ,
B. García-Lorenzo  and
A. Serrano-Borlaff
J. Zaragoza-Cardiel
Affiliation:
Instituto de Astronomía, Universidad Nacional Autónoma de México, Mexico City, Mexico email: [email protected]
J. Beckman
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain Department of Astrophysics, University of La Laguna, E-38200 La Laguna, Tenerife, Spain CSIC, 28006 Madrid, Spain
J. Font
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain Department of Astrophysics, University of La Laguna, E-38200 La Laguna, Tenerife, Spain
A. Camps-Fariña
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain Department of Astrophysics, University of La Laguna, E-38200 La Laguna, Tenerife, Spain
B. García-Lorenzo
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain Department of Astrophysics, University of La Laguna, E-38200 La Laguna, Tenerife, Spain
A. Serrano-Borlaff
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain Department of Astrophysics, University of La Laguna, E-38200 La Laguna, Tenerife, Spain
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Abstract

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We have combined observations of the Antennae galaxies from the radio interferometer ALMA and from the optical interferometer GHαFaS (Galaxy Hα Fabry-Perot System). The two sets of observations have comparable angular and spectral resolutions, enabling us to identify 142 giant molecular clouds (GMCs) and 303 Hii regions. We have measured, and compared, their basic physical properties (radius, velocity dispersion, luminosity). We study the mass functions of Hii regions and GMCs, where a double population of Hii regions due to a double population of GMCs is found. Using the velocity dispersion measurements, we claim that the difference between the regimes is the nature of the dominant binding force. For the regions in the lower mass range, the dominant force is the external pressure, while in the higher mass range it is the internal gravity of the clouds. We have applied the same method to similar observations (GHαFaS & ALMA) of Arp 236 and NGC 1614 finding similar results.

Keywords

Interacting galaxiesstar formationHii regionsGMCs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S316: Formation, evolution, and survival of massive star clusters , August 2015 , pp. 135 - 136
Copyright
Copyright © International Astronomical Union 2017 

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