High star formation rates as the origin of turbulence in early and modern disk galaxies

Andrew W. Green (), Karl Glazebrook, Peter J. McGregor, Roberto G. Abraham, Gregory B. Poole, Ivana Damjanov, Patrick J. McCarthy, Matthew Colless and Robert G. Sharp
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Andrew W. Green: Centre for Astrophysics and Supercomputing, Swinburne University, PO Box 218, Hawthorn, Victoria 3122, Australia
Karl Glazebrook: Centre for Astrophysics and Supercomputing, Swinburne University, PO Box 218, Hawthorn, Victoria 3122, Australia
Peter J. McGregor: Research School of Astronomy and Astrophysics, Australian National University
Roberto G. Abraham: University of Toronto, 50 St George Street, Toronto, Ontario M5S3H4, Canada
Gregory B. Poole: Centre for Astrophysics and Supercomputing, Swinburne University, PO Box 218, Hawthorn, Victoria 3122, Australia
Ivana Damjanov: University of Toronto, 50 St George Street, Toronto, Ontario M5S3H4, Canada
Patrick J. McCarthy: Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street
Matthew Colless: Australian Astronomical Observatory, PO Box 296
Robert G. Sharp: Australian Astronomical Observatory, PO Box 296

Nature, 2010, vol. 467, issue 7316, 684-686

Abstract: Galactic turbulence: disk galaxies ancient and modern We live in a disk galaxy, yet have a very poor understanding of how they form — not helped by the fact that disk galaxies in the early Universe seem rather different to our Milky Way. Many of the disk galaxies of the early Universe are surprisingly large and far more turbulent than the Milky Way and other modern spirals. Now the discovery of a new sample of similarly unusual disk galaxies persisting to the present day adds a significant new element to this debate. In these galaxies, resembling the 'turbulent disks' observed in the early Universe, velocity dispersions correlate with their star-formation rates, which suggests that star formation itself is the energetic driver of galaxy disk turbulence at all cosmic epochs.

Date: 2010
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DOI: 10.1038/nature09452

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