%0 Generic %1 ubler2019evolution %A Übler, Hannah D. N. %A Genzel, Reinhard %A Wisnioski, Emily %A Schreiber, Natascha M. Förster %A Shimizu, T. Taro %A Price, Sedona H. %A Tacconi, Linda J. %A Belli, Sirio %A Wilman, David J. %A Fossati, Matteo %A Mendel, J. Trevor %A Davies, Rebecca L. %A Beifiori, Alessandra %A Bender, Ralf %A Brammer, Gabriel B. %A Burkert, Andreas %A Chan, Jeffrey %A Davies, Richard I. %A Fabricius, Maximilian %A Galametz, Audrey %A Herrera-Camus, Rodrigo %A Lang, Philipp %A Lutz, Dieter %A Momcheva, Ivelina G. %A Naab, Thorsten %A Nelson, Erica J. %A Saglia, Roberto P. %A Tadaki, Ken-ichi %A van Dokkum, Pieter G. %A Wuyts, Stijn %D 2019 %K Tommre velocity-dispersion %T The Evolution and Origin of Ionized Gas Velocity Dispersion from $z\sim2.6$ to $z\sim0.6$ with KMOS$^3D$ %U http://arxiv.org/abs/1906.02737 %X 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 $\sigma_0\sim45$ km s$^-1$ at $z\sim2.3$ to $\sigma_0\sim30$ km s$^-1$ at $z\sim0.9$. There is substantial intrinsic scatter ($\sigma_\sigma_0, int\approx10$ km s$^-1$) around the best-fit $\sigma_0-z$-relation beyond what can be accounted for from the typical measurement uncertainties ($\delta\sigma_0\approx12$ 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 $\sim10-15$ 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.

@misc{ubler2019evolution, 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$^{\rm 3D}$ 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 $\sigma_0\sim45$ km s$^{-1}$ at $z\sim2.3$ to $\sigma_0\sim30$ km s$^{-1}$ at $z\sim0.9$. There is substantial intrinsic scatter ($\sigma_{\sigma_0, {\rm int}}\approx10$ km s$^{-1}$) around the best-fit $\sigma_0-z$-relation beyond what can be accounted for from the typical measurement uncertainties ($\delta\sigma_0\approx12$ 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 $\sim10-15$ 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.}, added-at = {2019-06-07T16:43:39.000+0200}, author = {Übler, Hannah D. N. and Genzel, Reinhard and Wisnioski, Emily and Schreiber, Natascha M. Förster and Shimizu, T. Taro and Price, Sedona H. and Tacconi, Linda J. and Belli, Sirio and Wilman, David J. and Fossati, Matteo and Mendel, J. Trevor and Davies, Rebecca L. and Beifiori, Alessandra and Bender, Ralf and Brammer, Gabriel B. and Burkert, Andreas and Chan, Jeffrey and Davies, Richard I. and Fabricius, Maximilian and Galametz, Audrey and Herrera-Camus, Rodrigo and Lang, Philipp and Lutz, Dieter and Momcheva, Ivelina G. and Naab, Thorsten and Nelson, Erica J. and Saglia, Roberto P. and Tadaki, Ken-ichi and van Dokkum, Pieter G. and Wuyts, Stijn}, biburl = {https://www.bibsonomy.org/bibtex/29d4c07a251f94bc9032c823c86461a61/heh15}, description = {The Evolution and Origin of Ionized Gas Velocity Dispersion from $z\sim2.6$ to $z\sim0.6$ with KMOS$^{\rm 3D}$}, interhash = {bed550a3ecd643fe81b6164fffc13179}, intrahash = {9d4c07a251f94bc9032c823c86461a61}, keywords = {Tommre velocity-dispersion}, note = {cite arxiv:1906.02737Comment: ~30 pages, 16 figures, 9 tables; accepted for publication in ApJ}, timestamp = {2019-06-07T16:43:39.000+0200}, title = {The Evolution and Origin of Ionized Gas Velocity Dispersion from $z\sim2.6$ to $z\sim0.6$ with KMOS$^{\rm 3D}$}, url = {http://arxiv.org/abs/1906.02737}, year = 2019 }