The Evolution and Origin of Ionized Gas Velocity Dispersion from $z\sim 2.6$ to $z\sim 0.6$ with KMOS${}^{3D}$

Abstract

We present the $0.6<z<2.6$ evolution of the ionized gas velocity dispersion in 175 star-forming disk galaxies based on data from the full KMOS${}^{3D}$ integral field spectroscopic survey. In a forward-modelling Bayesian framework including instrumental effects and beam-smearing, we fit simultaneously the observed galaxy velocity and velocity dispersion along the kinematic major axis to derive the intrinsic velocity dispersion ${\sigma }_0$. We find a reduction of the average intrinsic velocity dispersion of disk galaxies as a function of cosmic time, from ${\sigma }_0\sim 45$ km s${}^{-1}$ at $z\sim 2.3$ to ${\sigma }_0\sim 30$ km s${}^{-1}$ at $z\sim 0.9$. There is substantial intrinsic scatter (${\sigma }_{{\sigma }_0,\mathrm{int}}\approx 10$ km s${}^{-1}$) around the best-fit ${\sigma }_0-z$-relation beyond what can be accounted for from the typical measurement uncertainties ($\delta {\sigma }_0\approx 12$ km s${}^{-1}$), independent of other identifiable galaxy parameters. This potentially suggests a dynamic mechanism such as minor mergers or variation in accretion being responsible for the scatter. Putting our data into the broader literature context, we find that ionized and atomic+molecular velocity dispersions evolve similarly with redshift, with the ionized gas dispersion being $\sim 10-15$ km s${}^{-1}$ higher on average. We investigate the physical driver of the on average elevated velocity dispersions at higher redshift, and find that our galaxies are at most marginally Toomre-stable, suggesting that their turbulent velocities are powered by gravitational instabilities, while stellar feedback as a driver alone is insufficient. This picture is supported through comparison with a state-of-the-art analytical model of galaxy evolution.

arXiv comment~30 pages, 16 figures, 9 tables; accepted for publication in ApJ

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