The neutral hydrogen content of galaxies in cosmological hydrodynamic simulations

By R. Dav'e, Neal Katz, B. Oppenheimer, Juna A. Kollmeier, D. Weinberg. 2013

174 citations recorded by the source corpus.

We examine the global Hi properties of galaxies in quarter-billion particle cosmological simulations using Gadget-2, focusing on how galactic outflows impact Hi content. We consider four outflow models, including a new one (ezw) motivated by recent interstellar medium simulations in which the wind speed and mass loading factor scale as expected for momentum-driven outflows for larger galaxies and energy-driven outflows for dwarfs (� < 75 kms 1 ). To obtain predicted Hi masses, we employ a simple but effective local correction for particle self-shielding, and an observationally-constrained transition from neutral to molecular hydrogen. Our ezw simulation produces an Hi mass function whose faint-end slope of 1.3 agrees well with observations from the ALFALFA survey; other models agree less well. Satellite galaxies have a bimodal distribution in Hi fraction versus halo mass, with smaller satellites and/or those in larger halos more often being Hi-deficient. At a given stellar mass, Hi content correlates with star formation rate and inversely correlates with metallicity, as expected if driven by stochasticity in the accretion rate. To higher redshifts, massive Hi galaxies disappear and the mass function steepens. The global cosmic Hi density conspires to remain fairly constant from z � 5 ! 0, but the relative contribution from smaller galaxies increases with redshift.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/0187bcee4d4efaade49c6f895e17963700c354f5

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Citations in the corpus

THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, background): “See Davé et al. (2013) for a full description.”
The z ∼ 6 Luminosity Function Fainter than −15 mag from the Hubble Frontier Fields: The Impact of Magnification Uncertainties (2016, methodology): “Star formation is added using the Kennicutt-Schmidt law, with supernovae feedback included following the ”ezw” prescription from Davé et al. (2013) and metal enrichment from supernovae as implemented as in Oppenheimer & Davé (2008).”
Cold gas stripping in satellite galaxies: from pairs to clusters (2016, methodology): “While remaining a dramatical improvement on the detail afforded by semi-analytics, the moderate resolution of Davé et al. (2013) simulations means that there is a possibility of DM particles being spuriously heated due to two-body interaction, this leads to artificial heating and momentum transfer…”
Gravitational torque-driven black hole growth and feedback in cosmological simulations (2016, background): “M relation. driven winds but not AGN feedback (Oppenheimer & Davé 2008; Davé et al. 2013).”
Ingredients for 21 cm Intensity Mapping (2018, background): “We note that previous works have studied the HI content of simulated galaxies in detail (Crain et al. 2017; Bahé et al. 2016; Davé et al. 2013; Bird et al. 2014; Lagos et al. 2014; Faucher-Giguère et al. 2016; Marinacci et al. 2017; Zoldan et al. 2017; Xie et al. 2017).”
Star formation sustained by gas accretion (2014, methodology): “/M ) goes from 11.5 to 8, with the same range of variation from red early type galaxies to blue late types (Kannappan 2004; Pilyugin et al. 2004; Davé et al. 2013).”
Theoretical Challenges in Galaxy Formation (2016, methodology): “…finite mass method with star formation feedback scaling motivated by higher resolution simulations and an improved empirical gas heating model to Davé et al. (2013) for massive halos; from Puchwein & Springel (2013) using traditional SPH with momentum driven winds and thermal and ’bubble’…”
THE COS-DWARFS SURVEY: THE CARBON RESERVOIR AROUND SUB-L* GALAXIES (2014, methodology): “These simulations were introduced in Davé et al. (2013), including the constant wind (cw) and the energy-driven wind (ezw) models.”
MUFASA: Galaxy Formation Simulations With Meshless Hydrodynamics (2016, background): “In previous studies (e.g. Davé et al. 2013; Liang et al. 2016) we have simply rescaled metallicities in post-processing, arguing that such c© 0000 RAS, MNRAS 000, 000–000 changes do not greatly impact the dynamics, and that the predicted yields are uncertain at this level.”
Cosmological simulations of black hole growth: AGN luminosities and downsizing (2013, result): “…wind models can significantly reduce the baryon conversion efficiencies (e.g. Hirschmann et al. 2013, and references therein) and thus, also the low-mass end of the stellar mass function resulting in an improved match with the observational data (e.g. Davé et al. 2013; Puchwein & Springel 2013).”
THE SYSTEMATIC PROPERTIES OF THE WARM PHASE OF STARBURST-DRIVEN GALACTIC WINDS (2015, methodology): “Hybrid models with a mass-loading factor∝ v−2out at low velocities and ∝ v−1out at higher velocities have also been adopted (Davé et al. 2013; Vogelsberger et al. 2013; Ford et al. 2015).”
The mass evolution of the first galaxies: stellar mass functions and star formation rates at 4 < z < 7 in the CANDELS GOODS-South field (2014, methodology): “The SPH predictions are taken from the hybrid energy/momentum-driven wind model of Davé et al. (2013).”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, methodology): “…predictions from numerical hydrodynamic simulations: EAGLE simulations (Schaye et al. 2014, dark red), ezw simulations of Davé and collaborators (Davé et al. 2013, bright red) and the Illustris simulations (Vogelsberger et al. 2014b, orange). at reproducing the SMF of galaxies at z ∼ 0 by…”
Cold gas properties of the Herschel Reference Survey - II. Molecular and total gas scaling relations (2014, background): “On the other hand, stellar feedback plays a key role in loweringthe gas fractions and bringing the models back into agreement with the observations (see also Dave et al. 2013).”
Cosmology with Phase 1 of the Square Kilometre Array Red Book 2018: Technical specifications and performance forecasts (2018, background): “There have been numerous efforts to build accurate halo models of the HI distribution (e.g. Bagla et al. 2010; Davé et al. 2013; Villaescusa-Navarro et al. 2014, 2018a; Padmanabhan & Refregier 2017; Padmanabhan, Refregier, & Amara 2017, 2018), with free parameters typically constrained using some…”
The Neutral Hydrogen Cosmological Mass Density at z = 5 (2015, methodology): “One view is that H I represents a transitory phase fuelling star formation (e.g. Prochaska et al. 2005; Davé et al. 2013), which is continually replenished by more highly ionized gas from either the intergalactic medium (IGM) or recycled galactic outflows.”
THE UNIVERSAL RELATION OF GALACTIC CHEMICAL EVOLUTION: THE ORIGIN OF THE MASS–METALLICITY RELATION (2014, background): “Several authors have recognized variations in the gas content of galaxies as the basis of the observed relation between stellar mass, metallicity and SFR (e.g., Davé et al. 2012; Dayal et al. 2013; Bothwell et al. 2013; Lilly et al. 2013; Davé et al. 2013).”