Evolution of the metal content of the intra-cluster medium with hydrodynamical simulations
arXiv:0802.2224 · doi:10.1111/j.1365-2966.2008.13122.x
Abstract
We present a comparison between simulation results and X-ray observational data on the evolution of the metallicity of the intra-cluster medium (ICM). The simulations of galaxy clusters were performed with the Tree-SPH Gadget2 code that includes a detailed model of chemical evolution, by assuming three different shapes for the stellar initial mass function (IMF), namely the Salpeter (1955), Kroupa (2001) and Arimoto-Yoshii (1987) IMF. Our simulations predict significant radial gradients of the Iron abundance, which extend over the whole cluster virialized region. At larger radii, we do not detect any flattening of the metallicity profiles. As for the evolution of the ICM metal (Iron) abundance out to z=1, we find that it is determined by the combined action of (i) the sinking of already enriched gas, (ii) the ongoing metal production in galaxies and (iii) the locking of ICM metals in newborn stars. As a result, rather than suppressing the metallicity evolution, stopping star formation at z=1 has the effect of producing an even too fast evolution of the emission-weighted ICM metallicity with too high values at low redshift. Finally, we compare simulations with the observed rate of type-Ia supernovae per unit B-band luminosity (SnU_B). We find that our simulated clusters do not reproduce the decreasing trend of SnU_B at low redshift, unless star formation is truncated at z=1.
9 pages, 7 figures, to appear in MNRAS
References in corpus (16)
- Chandra temperature profiles for a sample of nearby relaxed galaxy clusters
- A Catalog of Galaxy Clusters Observed by XMM-Newton
- Chemical enrichment of galaxy clusters from hydrodynamical simulations
- Images, structural properties and metal abundances of galaxy clusters observed with Chandra ACIS-I at 0.1<z<1.3
- The Importance of Mergers for the Origin of Intracluster Stars in Cosmological Simulations of Galaxy Clusters
- Ram pressure stripping of disc galaxies orbiting in clusters. I. Mass and radius of the remaining gas disc
- Tracing the evolution in the iron content of the ICM
- Temperature and abundance profiles of hot gas in galaxy groups - I. Results and statistical analysis
- Observations of metals in the intra-cluster medium
- Physical viscosity in smoothed particle hydrodynamics simulations of galaxy clusters
- X-MAS2: Study Systematics on the ICM Metallicity Measurements
- Properties of the galaxy population in hydrodynamical simulations of clusters
- Metal mixing by buoyant bubbles in galaxy clusters
- The chemical enrichment of the ICM from hydrodynamical simulations
- On the evolution of the Fe abundance and of the Type Ia SN rate in clusters of galaxies
- On Iron Enrichment, Star Formation, and Type Ia Supernovae in Galaxy Clusters