Observations of star formation and kinematics in early galaxies at high spatial and spectral resolution have shown that two-thirds are massive rotating disk galaxies1,2,3,4,5, with the remainder being less massive non-rotating objects2,4,6,7,8. The line-of-sight-averaged velocity dispersions are typically five times higher than in today’s disk galaxies. This suggests that gravitationally unstable, gas-rich disks in the early Universe are fuelled by cold, dense accreting gas flowing along cosmic filaments and penetrating hot galactic gas halos9,10. These accreting flows, however, have not been observed11, and cosmic accretion cannot power the observed level of turbulence12. Here we report observations of a sample of rare, high-velocity-dispersion disk galaxies in the nearby Universe where cold accretion is unlikely to drive their high star formation rates. We find that their velocity dispersions are correlated with their star formation rates, but not their masses or gas fractions, which suggests that star formation is the energetic driver of galaxy disk turbulence at all cosmic epochs.
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A.W.G. and K.G. acknowledge financial support from the Australian Research Council. A.W.G. acknowledges a special scholarship from the Chancellery of the Swinburne University of Technology. We wish to thank the staff of the Anglo-Australian Observatory and the staff of the ANU 2.3-m telescope for their support of these observations.
The authors declare no competing financial interests.
This file contains Supplementary Text comprising of an overview of comparison data presented, sample selection methods and σm errors and the effects of beam smearing and resolution. The file also contains Supplementary Figures 1-3 with legends and additional references. (PDF 415 kb)
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Green, A., Glazebrook, K., McGregor, P. et al. High star formation rates as the origin of turbulence in early and modern disk galaxies. Nature 467, 684–686 (2010). https://doi.org/10.1038/nature09452
Astrophysics and Space Science (2014)
Astrophysics and Space Science (2014)