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DYNAMO Survey: An Upclose View of Clumpy Galaxies

Published online by Cambridge University Press:  09 February 2015

David Fisher  and
the DYNAMO Team
David Fisher
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P. O. Box 218, Hawthorn, VIC 3122, Australia email: dfisher@swin.edu.au
the DYNAMO Team
Affiliation:
http://adsabs.harvard.edu/abs/2014MNRAS.437.1070G
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Abstract

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We highlight recent results on the DYNAMO survey of turbulent, clumpy disks galaxies found at z=0.1. Bright star forming DYNAMO galaxies are found to be very similar in properties to star forming galaxies in the high redshift Universe. Typical star formation rates of turbulent DYNAMO galaxies range 10-80 M⊙ yr−1. Roughly 2/3 of DYNAMO galaxies have Hα kinematics that are consistent with rotation. The typical gas velocity dispersion of DYNAMO galaxies is σHα ~ 20 - 60 km s−1. We show that, when convolved to the same resolution, maps of Hα emission in DYNAMO galaxies have essentially identical morphology as that of z ~ 1 - 3 galaxies. Finally, DYNAMO galaxies have high molecular gas fractions fmol ~ 20 - 35%. We note that DYNAMO galaxies are not dwarfs, typical masses are Mstar ~ 0.8 - 8 × 1010 M⊙. These data are all consistent with a scenario in which despite being at relatively low redshift the DYNAMO galaxies are forming stars similarly to that observed in the high-redshift Universe, that is to say star formation is occurring in very massive (Mclump ~ 109 M⊙), very large (rclump ~ 300 pc) clumps of gas.

Keywords

galaxies: elliptical and lenticularcD - galaxies: evolution - galaxies: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S309: Galaxies in 3D across the Universe , July 2014 , pp. 129 - 132
Copyright
Copyright © International Astronomical Union 2015 

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