Chemical enrichment of galaxy clusters from hydrodynamical simulations

By Luca Tornatore, Stefano Borgani, Klaus Dolag, F. Matteucci. 2007

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We present cosmological hydrodynamical simulations of galaxy clusters aimed at studying the process of metal enrichment of the intra-cluster medium (ICM). These simulations have been performed by implementing a detailed model of chemical evolution in the TREE-PM+SPM GADGET-2 code. This model allows us to follow the metal release from Type II supernovae (SNII), Type Ia supernovae (SNIa) and asymptotic giant branch (AGB) stars by properly accounting for the lifetimes of stars of different mass, as well as to change the stellar initial mass function (IMF), the lifetime function and the stellar yields. As such, our implementation of chemical evolution represents a powerful instrument to follow the cosmic history of metal production. The simulations presented here have been performed with the twofold aim of checking numerical effects, as well as the impact of changing the model of chemical evolution and the efficiency of stellar feedback. In general, we find that the distribution of metals produced by SNII is more clumpy than for the product of low-mass stars, as a consequence of the different time-scales over which they are released. Using a standard Salpeter IMF produces a radial profile of iron abundance which is in fairly good agreement with observations available out to ≃0.6R 500 . This result holds almost independent of the numerical scheme adopted to distribute metals around star-forming regions. The mean age of enrichment of the ICM corresponds to redshift z ∼ 0.5, which progressively increases outside the virial region. Increasing resolution, we improve the description of a diffuse high-redshift enrichment of the inter-galactic medium (IGM). This turns into a progressively more efficient enrichment of the cluster outskirts, while having a smaller impact at R ≤ 0.5R 500 . As for the effect of the model of chemical evolution, we find that changing the IMF has the strongest impact. Using an IMF, which is top-heavier than the Salpeter one, provides a larger iron abundance, possibly in excess of the observed level, also significantly increasing the [O/Fe] relative abundance. Our simulations always show an excess of low-redshift star formation and, therefore, of the abundance of oxygen in central cluster regions, at variance with observations. This problem is not significantly ameliorated by increasing the efficiency of the stellar feedback.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3174008ba15fbef2879d6d5f95b592b25de4a101

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Citations in the corpus

The relation between velocity dispersion and mass in simulated clusters of galaxies: dependence on the tracer and the baryonic physics (2013, methodology): “We also include a description of metal production from chemical enrichment contributed by SN-II, SNIa and low and intermediate mass stars (Tornatore et al. 2007).”
Lensing and x-ray mass estimates of clusters (simulations) (2012, methodology): “We also include a detailed description of metal enrichment from different stellar populations, using the model originally described by Tornatore et al. (2007).”
THE METALLICITY EVOLUTION OF INTERACTING GALAXIES (2011, background): “…is transferred from a single stellar particle to a set of nearest SPH neighbors (e.g. Steinmetz & Mueller 1994; Kawata 2001; Kawata & Gibson 2003; Okamoto et al. 2005; Scannapieco et al. 2005; Stinson et al. 2006; Tornatore et al. 2007; Wiersma et al. 2009; Montuori et al. 2010; Perez et al. 2011).”
Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters (2009, methodology): “Therefore, our simulations predict tha diffuse intra-cluster stars provide a significant contribution to the enrichment of the intra-cluster medium (see also Tornatore et al. 2007).”
Baryon impact on the halo mass function: Fitting formulae and implications for cluster cosmology (2015, methodology): “Our simulations also incorporate a detailed treatment of stellar evolution and chemical enrichment following Tornatore et al. (2007), a multiphase model for star-formation (Springel & Hernquist 2003), and feedback processes associated with supernovae driven galactic winds and AGN (Springel &…”
Cosmological simulations of black hole growth: AGN luminosities and downsizing (2013, methodology): “MNRAS 442, 2304–2324 (2014) Downloaded from https://academic.oup.com/mnras/article-abstract/442/3/2304/1039443 by guest on 29 July 2018 Our simulations also include a detailed model of chemical evolution according to Tornatore et al. (2007).”
The case for AGN feedback in galaxy groups (2009, result): “In addition, we note that the profiles presented here appear to be very similar in shape to those found in the zoomed cosmological simulations of massive clusters in Tornatore et al. (2007) and Borgani et al. (2008).”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, background): “…Katz et al. 1996; Wiersma et al. 2009a), and chemical enrichment (e.g., Steinmetz & Mueller 1994; Mosconi et al. 2001; Lia et al. 2002; Springel & Hernquist 2003a; Kobayashi 2004; Scannapieco et al. 2005; Tornatore et al. 2007; Oppenheimer & Davé 2008; Wiersma et al. 2009b; Few et al. 2012).”
The physics driving the cosmic star formation history (2009, background): “Oppenheimer & Davé 2006; Tornatore et al. 2007; Choi & Nagamine 2009), but under the assumption of collisional ionization equilibrium and fixed relative abundances.”
Weighing simulated galaxy clusters using lensing and X-ray (2009, methodology): “…in the ICM (see Saro et al. 2006), (ii) a numerical scheme to suppress artificial viscosity far from the shock regions (see Dolag et al. 2005), and (iii) a treatment of chemical enrichment from both SNIa and SNII, as well as from low and intermediate mass stars (Tornatore et al. 2004, 2007).”
The First Billion Years project: the impact of stellar radiation on the co-evolution of Populations II and III (2012, methodology): “We follow the prescription for metal enrichment presented in Wiersma et al. (2009a), which is similar to that also employed by Tornatore et al. (2007b).”
Theoretical Challenges in Galaxy Formation (2016, background): “…equilibrium cooling (for specific implementations see e.g. Ceverino & Klypin 2009; Kravtsov 2003; Oppenheimer & Davé 2006; Scannapieco et al. 2005; Tornatore et al. 2007; Vogelsberger et al. 2013; Wiersma, Schaye & Smith 2009) of gas in the presence of the UV/X-ray background radiation from…”
CONNECTING ANGULAR MOMENTUM AND GALACTIC DYNAMICS: THE COMPLEX INTERPLAY BETWEEN SPIN, MASS, AND MORPHOLOGY (2015, unknown): “Our simulations also include a detailed model of chemical evolution according to Tornatore et al. (2007).”
LSD: Lyman-break galaxies Stellar populations and Dynamics – I. Mass, metallicity and gas at z∼ 3.1 (2009, methodology): “When taken at face value, some other models (e.g. Brooks et al. 2007; Tornatore et al. 2007) provide a better match with the observations, but a meaningful comparison can only be obtained by taking into account all the selection effects and observational biases, and by comparing not only stellar…”
The transition from population III to population II-I star formation (2010, methodology): “Our findings are consistent with the study of theZcrit = 10−4Z⊙ case by Tornatore et al. (2007).”
The First Billion Years project: the escape fraction of ionizing photons in the epoch of reionization (2015, methodology): “For Pop II stars the abundances are calculated from yields for asymptotic giant branch stars and type Ia and type II SNe (Tornatore et al. 2007; Wiersma et al. 2009b).”
Constraints on the distribution and energetics of fast radio bursts using cosmological hydrodynamic simulations (2014, methodology): “Our simulations also include a detailed model of chemical evoluti n (Tornatore et al. 2007).”
The Dynamical and Chemical Evolution of Dwarf Spheroidal Galaxies with GEAR (2009, methodology): “In galaxy cluster simulations, Tornatore et al. (2007) varied Nngb from 16 to 128.”