Dynamic Equilibrium Sets of the Atomic Content of Galaxies across Cosmic Time

Wang, Liang; Obreschkow, Danail; Lagos, Claudia D. P.; Sweet, Sarah M.; Fisher, Deanne B.; Glazebrook, Karl; Macciò, Andrea V.; Dutton, Aaron A.; Kang, Xi

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Dynamic Equilibrium Sets of the Atomic Content of Galaxies across Cosmic Time

MPS-Authors

Wang, Liang
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Obreschkow, Danail
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lagos, Claudia D. P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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

Fisher, Deanne B.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Glazebrook, Karl
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Macciò, Andrea V.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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

Kang, Xi
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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https://ui.adsabs.harvard.edu/abs/2018ApJ...868...93W
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Citation

Wang, L., Obreschkow, D., Lagos, C. D. P., Sweet, S. M., Fisher, D. B., Glazebrook, K., et al. (2018). Dynamic Equilibrium Sets of the Atomic Content of Galaxies across Cosmic Time. The Astrophysical Journal, 868.

Cite as: https://hdl.handle.net/21.11116/0000-0005-CA5C-1

Abstract

We analyze 88 independent, high-resolution, cosmological zoomed-in simulations of disk galaxies in the NIHAO simulations suite to explore the connection between the atomic gas fraction and angular momentum (AM) of baryons throughout cosmic time. The study is motivated by the analytical model of Obreschkow et al., which predicts a relation between the atomic gas fraction f _atm and the integrated atomic stability parameter q\equiv jσ /({GM}), where M and j are the mass and specific AM of the galaxy (stars+cold gas) and σ is the velocity dispersion of the atomic gas. We show that the simulated galaxies follow this relation from their formation (z ≃ 4) to the present within ̃0.5 dex. To explain this behavior, we explore the evolution of the local Toomre stability and find that 90%-100% of the atomic gas in all simulated galaxies is stable at any time. In other words, throughout the entire epoch of peak star formation until today, the timescale for accretion is longer than the timescale to reach equilibrium, thus resulting in a quasi-static equilibrium of atomic gas at any time. Hence, the evolution of f _atm depends on the complex hierarchical growth history primarily via the evolution of q. An exception is galaxies subject to strong environmental effects.