The enrichment history of cosmic metals

Abstract

We use a suite of cosmological, hydrodynamical simulations to investigate the chemical enrichment history of the Universe. Specifically, we trace the origin of the metals back in time to investigate when various gas phases were enriched and by what halo masses. We find that the age of the metals decreases strongly with the density of the gas in which they end up. At least half of the metals that reside in the diffuse intergalactic medium (IGM) at redshift zero (two) were ejected from galaxies above redshift two (three). The mass of the haloes that last contained the metals increases rapidly with the gas density. More than half of the mass in intergalactic metals was ejected by haloes with total masses less than 1e11 solar masses and stellar masses less than 1e9 solar masses. The range of halo masses that contributes to the enrichment is wider for the hotter part of the IGM. By combining the `when' and `by what' aspects of the enrichment history, we show that metals residing in lower density gas were typically ejected earlier and by lower mass haloes.

14 pages, 10 figures, accepted by MNRAS, minor changes to the submitted version

References in corpus (16)

• The effect of photo-ionization on the cooling rates of enriched, astrophysical plasmas
• Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations
• Cosmological Simulations of Intergalactic Medium Enrichment from Galactic Outflows
• Mass, Metal, and Energy Feedback in Cosmological Simulations
• Time-Dependent Ionization in Radiatively Cooling Gas
• The Low-z Intergalactic Medium. III. HI and Metal Absorbers at z<0.4
• Simulations of Cosmic Chemical Enrichment
• A large population of metal-rich, compact, intergalactic C IV absorbers - Evidence for poor small-scale metal mixing
• On the Origin of Cores in Simulated Galaxy Clusters
• The Nature and Origin of Low-Redshift O VI Absorbers
• Metallicity of the intergalactic medium using pixel statistics: IV. Oxygen
• The Enrichment History of Baryons in the Universe
• The chemical enrichment of the ICM from hydrodynamical simulations
• Galactic Wind Signatures around High Redshift Galaxies
• Where are the Cosmic Metals at z~3?
• The association between gas and galaxies II: The 2-point correlation function

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