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Journal Article

Atomic and molecular gas in IllustrisTNG galaxies at low redshift

MPS-Authors

Diemer,  Benedikt
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Stevens,  Adam R. H.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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

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

Tacchella,  Sandro
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hernquist,  Lars
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Marinacci,  Federico
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Nelson,  Dylan
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pillepich,  Annalisa
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Rodriguez-Gomez,  Vicente
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Villaescusa-Navarro,  Francisco
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Vogelsberger,  Mark
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.1529D
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Citation

Diemer, B., Stevens, A. R. H., Lagos, C. d. P., Calette, A. R., Tacchella, S., Hernquist, L., et al. (2019). Atomic and molecular gas in IllustrisTNG galaxies at low redshift. Monthly Notices of the Royal Astronomical Society, 487, 1529-1550.


Cite as: https://hdl.handle.net/21.11116/0000-0005-D160-2
Abstract
We have recently developed a post-processing framework to estimate the abundance of atomic and molecular hydrogen (H I and H2, respectively) in galaxies in large-volume cosmological simulations. Here we compare the H I and H2 content of IllustrisTNG galaxies to observations. We mostly restrict this comparison to z ≈ 0 and consider six observational metrics: the overall abundance of H I and H2, their mass functions, gas fractions as a function of stellar mass, the correlation between H2 and star formation rate, the spatial distribution of gas, and the correlation between gas content and morphology. We find generally good agreement between simulations and observations, particularly for the gas fractions and the H I mass-size relation. The H2 mass correlates with star formation rate as expected, revealing an almost constant depletion time that evolves up to z = 2 as observed. However, we also discover a number of tensions with varying degrees of significance, including an overestimate of the total neutral gas abundance at z = 0 by about a factor of 2 and a possible excess of satellites with no or very little neutral gas. These conclusions are robust to the modelling of the H I/H2 transition. In terms of their neutral gas properties, the IllustrisTNG simulations represent an enormous improvement over the original Illustris run. All data used in this paper are publicly available as part of the IllustrisTNG data release.