The Origin and Evolution of the Galaxy Mass-Metallicity Relation

Abstract

We use high-resolution cosmological zoom-in simulations from the Feedback in Realistic Environment (FIRE) project to study the galaxy mass-metallicity relations (MZR) from z=0-6. These simulations include explicit models of the multi-phase ISM, star formation, and stellar feedback. The simulations cover halo masses Mhalo=10^9-10^13 Msun and stellar mass Mstar=10^4-10^11 Msun at z=0 and have been shown to produce many observed galaxy properties from z=0-6. For the first time, our simulations agree reasonably well with the observed mass-metallicity relations at z=0-3 for a broad range of galaxy masses. We predict the evolution of the MZR from z=0-6 as log(Zgas/Zsun)=12+log(O/H)-9.0=0.35[log(Mstar/Msun)-10]+0.93 exp(-0.43 z)-1.05 and log(Zstar/Zsun)=[Fe/H]-0.2=0.40[log(Mstar/Msun)-10]+0.67 exp(-0.50 z)-1.04, for gas-phase and stellar metallicity, respectively. Our simulations suggest that the evolution of MZR is associated with the evolution of stellar/gas mass fractions at different redshifts, indicating the existence of a universal metallicity relation between stellar mass, gas mass, and metallicities. In our simulations, galaxies above Mstar=10^6 Msun are able to retain a large fraction of their metals inside the halo, because metal-rich winds fail to escape completely and are recycled into the galaxy. This resolves a long-standing discrepancy between "sub-grid" wind models (and semi-analytic models) and observations, where common sub-grid models cannot simultaneously reproduce the MZR and the stellar mass functions.

17 pages, 14 figures, re-submitted to MNRAS after revisions on referee comments

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• Constraints on Population I/II neutron star-black hole binary formation by gravitational wave and radio observations
• The Phoenix stellar stream rose from the ashes of an ancient star cluster
• Euclid: Early Release Observations -- The star cluster systems of the Local Group dwarf galaxies IC 10 and NGC 6822
• Properties of Globular Clusters in Galaxy Clusters: Sensitivity from the Formation and Evolution of Globular Clusters
• Looking into the faintEst WIth MUSE (LEWIS): on the nature of ultra-diffuse galaxies in the Hydra I cluster. V. Integrated stellar population properties
• A theoretical investigation of far-infrared fine structure lines at $z>6$ and of the origin of the [OIII]88/[CII]158 enhancement
• Compact dust-obscured star-formation and the origin of the galaxy bimodality
• Past, present and Future of the Scaling Relations of Galaxies and Active Galactic Nuclei
• HE0144-4657: A Carbon-Enhanced Ultra Metal-Poor Star ([Fe/H] ~ -4.1) from the Helmi Stream Disrupted Dwarf Galaxy
• Origin of Weak MgII and Higher Ionization Absorption Lines in an Outflow from an Intermediate-Redshift Dwarf Satellite Galaxy
• Metal-THINGS: gas metallicity gradients in nearby galaxies
• MUSEQuBES: Physical conditions, origins, and multi-element abundances of the circumgalactic medium of an isolated, star-forming dwarf galaxy at z=0.57
• The Stellar Chemical Abundances of Simulated Massive Galaxies at $z=2$
• Chemical evolution history of MaNGA galaxies
• Impact of Massive Binary Star and Cosmic Evolution on Gravitational Wave Observations II: Double Compact Object Rates and Properties
• GRB 160410A: the first Chemical Study of the Interstellar Medium of a Short GRB
• Probing possible effects of circumgalactic media on the metal content of galaxies through the mass-metallicity relationship
• Extreme Metallicity Dwarf Galaxies in IllustrisTNG
• Cold vs. Hot Gas Accretion and Angular Momentum in FIRE Simulations: From Halo to Galaxy Scales
• Merging massive black holes: the right place and the right time
• New Insights into Uncertainties in the Relic Neutrino Background and Effects from the Nuclear Equation of State
• A deep ALMA Band 3 survey of HDFS/MUSE3D: Survey description and initial results
• 3D elemental abundances of stars at formation across the histories of Milky Way-mass galaxies in the FIRE simulations