Atomic hydrogen in IllustrisTNG galaxies: the impact of environment parallelled with local 21-cm surveys

Stevens, Adam; Diemer, Benedikt; Lagos, Claudia del P.; Nelson, Dylan; Pillepich, Annalisa; Brown, Toby; Catinella, Barbara; Hernquist, Lars; Weinberger, Rainer; Vogelsberger, Mark; Marinacci, Federico

doi:10.1093/mnras/sty3451

Cited by 110 publications

(131 citation statements)

References 149 publications

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“…A direct comparison of the slope in the ∆ f q -∆ M * between different models is not straight forward. For instance Figure 8 of Stevens et al (2019) shows that ∆ M * and ∆ f q covary, but a direct comparison to our study is complicated by different analysis techniques. A comparison of the ∆ f q -∆ M * between models and observations could offer an interesting avenue for future research, which might benefit from the use of ∆ f q as a uniform definition of H i deficiencies.…”

Section: Discussion Of Quenching Process Of Eagle Cluster Galaxiesmentioning

confidence: 64%

“…A simple way of defining a H i deficiency, often used for simulations (e.g. Crain et al 2017;Stevens et al 2019), is to measure the offset of a galaxy from the mean stellar mass-H i mass relation, or, equivalently the baryon mass-H i fraction relation, M-f atm . Formally, this definition of the H i deficiency can be written as ∆ f M = log 10 0.5 M 10 9 M −0.37 − log 10 ( f atm ) ,…”

Section: H I Deficiency Relative To Stellar Massmentioning

confidence: 99%

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Angular momentum-related probe of cold gas deficiencies

Jie

Obreschkow

Lagos

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Recent studies of neutral atomic hydrogen (H i) in nearby galaxies found that all field disk galaxies are H i saturated, in that they carry roughly as much H i as permitted before this gas becomes gravitationally unstable. By taking this H i saturation for granted, the atomic gas fraction f atm of galactic disks can be predicted as a function of the stability parameter q = jσ/(GM), where M and j are the baryonic mass and specific angular momentum of the disk and σ is the H i velocity dispersion (Obreschkow et al. 2016). The log-ratio ∆ f q between this predictor and the observed atomic fraction can be seen as a physically motivated 'H i deficiency'. While field disk galaxies have ∆ f q ≈ 0, objects subject to environmental removal of H i are expected to have ∆ f q > 0. Within this framework, we revisit the H i deficiencies of satellite galaxies in the Virgo cluster and in clusters of the EAGLE simulation. We find that observed and simulated cluster galaxies are H i deficient and that ∆ f q slightly increases when getting closer to the cluster centres. The ∆ f q values are similar to traditional H i deficiency estimators, but ∆ f q is more directly comparable between observations and simulations than morphology-based deficiency estimators. By tracking the simulated H i deficient cluster galaxies back in time, we confirm that ∆ f q ≈ 0 until the galaxies first enter a halo with M halo > 10 13 M , at which moment they quickly lose H i by environmental effects. Finally, we use the simulation to investigate the links between ∆ f q and quenching of star formation.

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Section: Discussion Of Quenching Process Of Eagle Cluster Galaxiesmentioning

confidence: 64%

Section: H I Deficiency Relative To Stellar Massmentioning

confidence: 99%

Angular momentum-related probe of cold gas deficiencies

Jie

Obreschkow

Lagos

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The observational data points correspond to weighted medians and the errors take into account statistical uncertainties associated with the IRAM calibration and aperture corrections and the sampling error determined from bootstrapping. It should be noted that while model results are presented for individual galaxies, observational mass estimates are derived using a beam size of 3.5 arcmin (corresponding to ∼ 25kpc at z=0.015) and might include contributions from multiple objects (see Stevens et al 2019 for an extensive discussion on the topic). The distribution of HI mass fractions in our new model closely match those observed showing a strong decline with increasing stellar mass.…”

Section: H 2 Contentmentioning

confidence: 99%

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

Henriques

Yates

et al. 2019

Monthly Notices of the Royal Astronomical Society

112

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We have updated the Munich galaxy formation model, L-galaxies, to follow the radial distributions of stars and atomic and molecular gas in galaxy discs. We include an H 2 -based star-formation law, as well as a detailed chemical-enrichment model with explicit mass-dependent delay times for SN-II, SN-Ia and AGB stars. Information about the star formation, feedback and chemical-enrichment histories of discs is stored in 12 concentric rings. The new model retains the success of its predecessor in reproducing the observed evolution of the galaxy population, in particular, stellar mass functions and passive fractions over the redshift range 0 z 3 and mass range 8 log(M * / M ) 12, the black hole-bulge mass relation at z = 0, galaxy morphology as a function of stellar mass and the mass-metallicity relations of both stellar and gas components. In addition, its detailed modelling of the radial structure of discs allows qualitatively new comparisons with observation, most notably with the relative sizes and masses of the stellar, atomic and molecular components in discs. Good agreement is found with recent data. Comparison of results obtained for simulations differing in mass resolution by more than two orders of magnitude shows that all important distributions are numerically well converged even for this more detailed model. An examination of metallicity and surface-density gradients in the stars and gas indicates that our new model, with star formation, chemical enrichment and feedback calculated self-consistently on local disc scales, reproduces some but not all of the trends seen in recent many-galaxy IFU surveys.

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“…Gas cells in the simulation are post-processed to calculate their mass fractions in the form of atomic and molecular hydrogen (Diemer et al 2018;Stevens et al 2019). We present results from three methods, based on the works by Gnedin & Kravtsov (2011), Krumholz (2013), and Gnedin & Draine (2014).…”

Section: Illustristngmentioning

confidence: 99%

Origin of the galaxy H i size–mass relation

Stevens

Diemer

Lagos

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We analytically derive the observed size-mass relation of galaxies' atomic hydrogen (H i), including limits on its scatter, based on simple assumptions about the structure of H i discs. We trial three generic profiles for H i surface density as a function of radius. Firstly, we assert that H i surface densities saturate at a variable threshold, and otherwise fall off exponentially with radius or, secondly, radius squared. Our third model assumes the total gas surface density is exponential, with the H i fraction at each radius depending on local pressure. These are tested against a compilation of 110 galaxies from the THINGS, LITTLE THINGS, LVHIS, and Bluedisk surveys, whose H i surface density profiles are well resolved. All models fit the observations well and predict consistent size-mass relations. Using an analytical argument, we explain why processes that cause gas disc truncation -such as ram-pressure stripping -scarcely affect the H i size-mass relation. This is tested with the IllustrisTNG(100) cosmological, hydrodynamic simulation and the Dark Sage semi-analytic model of galaxy formation, both of which capture radially resolved disc structure. For galaxies with m * ≥ 10 9 M and m H i ≥ 10 8 M , both simulations predict H i size-mass relations that align with observations, show no difference between central and satellite galaxies, and show only a minor, second-order dependence on host halo mass for satellites. Ultimately, the universally tight H i size-mass relation is mathematically inevitable and robust. Only by completely disrupting the structure of H i discs, e.g. through overly powerful feedback, could a simulation predict the relation poorly.

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Atomic hydrogen in IllustrisTNG galaxies: the impact of environment parallelled with local 21-cm surveys

Cited by 110 publications

References 149 publications

Angular momentum-related probe of cold gas deficiencies

Angular momentum-related probe of cold gas deficiencies

L-GALAXIES 2020: Spatially resolved cold gas phases, star formation, and chemical enrichment in galactic discs

Origin of the galaxy H i size–mass relation

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