The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS 3D

H. Übler, R. Genzel, E. Wisnioski, N. M. Förster Schreiber, T. T. Shimizu, S. H. Price, L. J. Tacconi, S. Belli, D. J. Wilman, M. Fossati, J. T. Mendel, A. Beifiori, R. Bender, G. B. Brammer, A. Burkert, J. Chan, M. Fabricius, A. Galametz, R. Herrera-camus, P. LangD. Lutz, I. G. Momcheva, T. Naab, E. J. Nelson, R. P. Saglia, K. Tadaki, P. G. Van Dokkum, S. Wuyts

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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 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 σ0,int ≈ 10km 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.

Original languageEnglish
Article number48
Pages (from-to)1-24
Number of pages24
JournalAstrophysical Journal
Volume880
Issue number1
DOIs
Publication statusPublished - 24 Jul 2019

Keywords

  • galaxies: ISM
  • galaxies: evolution
  • galaxies: high-redshift
  • galaxies: kinematics and dynamics

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Übler, H., Genzel, R., Wisnioski, E., Schreiber, N. M. F., Shimizu, T. T., Price, S. H., ... Wuyts, S. (2019). The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS 3D. Astrophysical Journal, 880(1), 1-24. [48]. https://doi.org/10.3847/1538-4357/ab27cc

The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS 3D. / Übler, H.; Genzel, R.; Wisnioski, E.; Schreiber, N. M. Förster; Shimizu, T. T.; Price, S. H.; Tacconi, L. J.; Belli, S.; Wilman, D. J.; Fossati, M.; Mendel, J. T.; Beifiori, A.; Bender, R.; Brammer, G. B.; Burkert, A.; Chan, J.; Fabricius, M.; Galametz, A.; Herrera-camus, R.; Lang, P.; Lutz, D.; Momcheva, I. G.; Naab, T.; Nelson, E. J.; Saglia, R. P.; Tadaki, K.; Dokkum, P. G. Van; Wuyts, S.

In: Astrophysical Journal, Vol. 880, No. 1, 48, 24.07.2019, p. 1-24.

Research output: Contribution to journalArticle

Übler, H, Genzel, R, Wisnioski, E, Schreiber, NMF, Shimizu, TT, Price, SH, Tacconi, LJ, Belli, S, Wilman, DJ, Fossati, M, Mendel, JT, Beifiori, A, Bender, R, Brammer, GB, Burkert, A, Chan, J, Fabricius, M, Galametz, A, Herrera-camus, R, Lang, P, Lutz, D, Momcheva, IG, Naab, T, Nelson, EJ, Saglia, RP, Tadaki, K, Dokkum, PGV & Wuyts, S 2019, 'The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS 3D', Astrophysical Journal, vol. 880, no. 1, 48, pp. 1-24. https://doi.org/10.3847/1538-4357/ab27cc
Übler H, Genzel R, Wisnioski E, Schreiber NMF, Shimizu TT, Price SH et al. The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS 3D. Astrophysical Journal. 2019 Jul 24;880(1):1-24. 48. https://doi.org/10.3847/1538-4357/ab27cc
Übler, H. ; Genzel, R. ; Wisnioski, E. ; Schreiber, N. M. Förster ; Shimizu, T. T. ; Price, S. H. ; Tacconi, L. J. ; Belli, S. ; Wilman, D. J. ; Fossati, M. ; Mendel, J. T. ; Beifiori, A. ; Bender, R. ; Brammer, G. B. ; Burkert, A. ; Chan, J. ; Fabricius, M. ; Galametz, A. ; Herrera-camus, R. ; Lang, P. ; Lutz, D. ; Momcheva, I. G. ; Naab, T. ; Nelson, E. J. ; Saglia, R. P. ; Tadaki, K. ; Dokkum, P. G. Van ; Wuyts, S. / The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS 3D. In: Astrophysical Journal. 2019 ; Vol. 880, No. 1. pp. 1-24.
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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 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 σ0,int ≈ 10km 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.",
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T1 - The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS 3D

AU - Übler, H.

AU - Genzel, R.

AU - Wisnioski, E.

AU - Schreiber, N. M. Förster

AU - Shimizu, T. T.

AU - Price, S. H.

AU - Tacconi, L. J.

AU - Belli, S.

AU - Wilman, D. J.

AU - Fossati, M.

AU - Mendel, J. T.

AU - Beifiori, A.

AU - Bender, R.

AU - Brammer, G. B.

AU - Burkert, A.

AU - Chan, J.

AU - Fabricius, M.

AU - Galametz, A.

AU - Herrera-camus, R.

AU - Lang, P.

AU - Lutz, D.

AU - Momcheva, I. G.

AU - Naab, T.

AU - Nelson, E. J.

AU - Saglia, R. P.

AU - Tadaki, K.

AU - Dokkum, P. G. Van

AU - Wuyts, S.

PY - 2019/7/24

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