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The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS3D

MPG-Autoren

Übler,  H.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Genzel,  R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wisnioski,  E.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Förster Schreiber,  N. M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Shimizu,  T. T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Price,  S. H.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Tacconi,  L. J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Belli,  S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wilman,  D. J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Fossati,  M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Mendel,  J. T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Davies,  R. L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Beifiori,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bender,  R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Brammer,  G. B.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Burkert,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Chan,  J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Davies,  R. I.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Fabricius,  M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Galametz,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Herrera-Camus,  R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lang,  P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lutz,  D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Momcheva,  I. G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Naab,  T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Nelson,  E. J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Saglia,  R. P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Tadaki,  K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

van Dokkum,  P. G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wuyts,  S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Externe Ressourcen

https://ui.adsabs.harvard.edu/abs/2019ApJ...880...48U
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Zitation

Übler, H., Genzel, R., Wisnioski, E., Förster Schreiber, N. M., Shimizu, T. T., Price, S. H., et al. (2019). The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS3D. The Astrophysical Journal, 880.


Zitierlink: https://hdl.handle.net/21.11116/0000-0005-CF8E-3
Zusammenfassung
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 KMOS3D integral field spectroscopic survey. In a forward- modeling 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 σ 0. We find a reduction of the average intrinsic velocity dispersion of disk galaxies as a function of cosmic time, from σ 0 ∼ 45 km s−1 at z ∼ 2.3 to σ 0 ∼ 30 km s−1 at z ∼ 0.9. There is substantial intrinsic scatter ({σ }{σ 0,{int}}≈ 10 {km} {{{s}}}-1) around the best-fit σ 0─z relation beyond what can be accounted for from the typical measurement uncertainties (δσ 0 ≈ 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 ∼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. Based on observations collected at the Very Large Telescope (VLT) of the European Southern Observatory (ESO), Paranal, Chile, under ESO program IDs 092.A-0091, 093.A-0079, 094.A-0217, 095.A-0047, 096.A-0025, 097.A-0028, 098.A-0045, 099.A-0013, 0100.A-0039, and 0101.A-0022.