Iron abundances and heating of the intracluster medium in hydrodynamical simulations of galaxy clusters

Valdarnini, R.

doi:10.1046/j.1365-8711.2003.06163.x

Cited by 81 publications

(90 citation statements)

References 87 publications

(207 reference statements)

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“…Mechanisms such as ram pressure (Domainko et al 2004;Cora 2006) or tidal stripping (e.g. Murante et al 2004) are currently being investigated with numerical simulations (see also Valdarnini 2003;Tornatore et al 2004). The same mechanisms are often invoked to explain the morphological evolution of the cluster galaxies' population.…”

Section: Discussionmentioning

confidence: 99%

Tracing the evolution in the iron content of the intra-cluster medium

Balestra

Tozzi

Ettori

et al. 2006

A&A

158

237

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Context. We present a Chandra analysis of the X-ray spectra of 56 clusters of galaxies at z > ∼ 0.3, which cover a temperature range of 3 < ∼ kT < ∼ 15 keV. Aims. Our analysis is aimed at measuring the iron abundance in the intra-cluster medium (ICM) out to the highest redshift probed to date. Methods. We made use of combined spectral analysis performed over five redshift bins at 0.3 < ∼ z < ∼ 1.3 to estimate the average emission weighted iron abundance. We applied non-parametric statistics to assess correlations between temperature, metallicity, and redshift. Results. We find that the emission-weighted iron abundance measured within (0.15−0.3) R vir in clusters below 5 keV is, on average, a factor of ∼2 higher than in hotter clusters, following Z(T ) 0.88 T −0.47 Z , which confirms the trend seen in local samples. We also find a constant average iron abundance Z Fe 0.25 Z as a function of redshift, but only for clusters at z > ∼ 0.5. The emission-weighted iron abundance is significantly higher (Z Fe 0.4 Z ) in the redshift range z 0.3−0.5, approaching the value measured locally in the inner 0.15 R vir radii for a mix of cool-core and non cool-core clusters in the redshift range 0.1 < z < 0.3. The decrease in metallicity with redshift can be parametrized by a power law of the form ∼(1 + z) −1.25 . We tested our results against selection effects and the possible evolution in the occurrence of metallicity and temperature gradients in our sample, and we do not find any evidence of a significant bias associated to these effects. Conclusions. The observed evolution implies that the average iron content of the ICM at the present epoch is a factor of ∼2 larger than at z 1.2. We confirm that the ICM is already significantly enriched (Z Fe 0.25 Z ) at a look-back time of 9 Gyr. Our data provide significant constraints on the time scales and physical processes that drive the chemical enrichment of the ICM.

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Section: Discussionmentioning

confidence: 99%

Tracing the evolution in the iron content of the intra-cluster medium

Balestra

Tozzi

Ettori

et al. 2006

A&A

158

237

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“…Cosmological hydrodynamical simulations have been used with similar goals (Valdarnini 2003;Romeo et al 2006;Tornatore et al 2007;Davé et al 2008;Wiersma et al 2011;Crain et al 2013;Skory et al 2013): the results by Tornatore et al (2007) showed good agreement of metal abundances in simulated clusters in absence of AGN feedback at the price of significant over-production of galaxy stellar masses. More recent papers highlighted that much better agreement between stellar masses and cluster metallicities with observational results can be achieved when AGN feedback is included (Wiersma et al 2011;Crain et al 2013;Skory et al 2013).…”

Section: Comparison To Recent Simulationsmentioning

confidence: 99%

Rhapsody-G simulations – II. Baryonic growth and metal enrichment in massive galaxy clusters

Martizzi

Hahn

et al. 2016

Mon. Not. R. Astron. Soc.

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We study the evolution of the stellar component and the metallicity of both the intracluster medium and of stars in massive (M vir « 6ˆ10 14 M d {h) simulated galaxy clusters from the Rhapsody-G suite in detail and compare them to observational results. The simulations were performed with the AMR code RAMSES and include the effect of AGN feedback at the sub-grid level. AGN feedback is required to produce realistic galaxy and cluster properties and plays a role in mixing material in the central regions and regulating star formation in the central galaxy. In both our low and high resolution runs with fiducial stellar yields, we find that stellar and ICM metallicities are a factor of two lower than in observations. We find that cool core clusters exhibit steeper metallicity gradients than non-cool core clusters, in qualitative agreement with observations. We verify that the ICM metallicities measured in the simulation can be explained by a simple "regulator" model in which the metallicity is set by a balance of stellar yield and gas accretion. It is plausible that a combination of higher resolution and higher metal yield in AMR simulation would allow the metallicity of simulated clusters to match observed values; however this hypothesis needs to be tested with future simulations. Comparison to recent literature highlights that results concerning the metallicity of clusters and cluster galaxies might depend sensitively on the scheme chosen to solve the hydrodynamics.

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“…Moreover, energy and metal feedback that follows from supernova explosions should also be considered. Hydrodynamical simulations in which these physical processes have been taken into account (Muanwong et al 2002;Tornatore et al 2003;Valdarnini 2003;Kay et al 2004;Nagai et al 2007b) have shown that there is substantial agreement between the predicted ICM properties, such as the temperature profiles, and the corresponding measurements, though significant discrepancies still remain (Borgani & Kravtsov 2009). In particular, the model overpredicts the star mass fraction, which is found in simulations to be a factor ∼2−3 higher than that estimated from observations.…”

Section: Simulations With Cooling and Star Formationmentioning

confidence: 99%

The impact of numerical viscosity in SPH simulations of galaxy clusters

Valdarnini

2011

A&A

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The goal of this paper is to investigate in N-body/SPH hydrodynamical cluster simulations the impact of artificial viscosity on the ICM thermal and velocity field statistical properties. To properly reduce the effects of artificial viscosity, a time-dependent artificial viscosity scheme is implemented in an SPH code in which each particle has its own viscosity parameter, whose time evolution is governed by the local shock conditions. The new SPH code is verified in a number of test problems with known analytical or numerical reference solutions and is then used to construct a large set of N-body/SPH hydrodynamical cluster simulations. These simulations are designed to study in SPH simulations the impact of artificial viscosity on the thermodynamics of the ICM and its velocity field statistical properties by comparing results extracted at the present epoch from runs with different artificial viscosity parameters, cluster dynamical states, numerical resolution, and physical modeling of the gas. Spectral properties of the gas velocity field are investigated by measuring the velocity power spectrum E(k) for the simulated clusters. Over a limited range, the longitudinal component E c (k) exhibits a Kolgomorov-like scaling ∝k −5/3 , whilst the solenoidal power spectrum component E s (k) is strongly influenced by numerical resolution effects. The dependence of the spectra E(k) on dissipative effects is found to be significant at length scales < ∼ 100−300 kpc, with viscous damping of the velocities being less pronounced in the runs with the lowest artificial viscosity. The turbulent energy density radial profile E turb (r) is strongly affected by the numerical viscosity scheme adopted in the simulations, with the turbulent-to-total energy density ratios being higher in the runs with the lowest artificial viscosity settings and lying in the range between a few percent and ∼10%. These values are in accord with the corresponding ratios extracted from previous cluster simulations based on mesh-based codes. The radial entropy profiles show a weak dependence on the artificial viscosity parameters of the simulations, with a small amount of entropy mixing being present in cluster cores. At large cluster radii, the mass correction terms to the hydrostatic equilibrium equation are affected little by the numerical viscosity of the simulations, indicating that the X-ray mass bias is already accurately estimated in standard SPH simulations. The results presented here indicate that in individual SPH cluster simulations at least N > ∼ 256 3 gas particles are necessary to provide a correct description of turbulent spectral properties over a decade in wavenumbers, whilst radial profiles of thermodynamic variables can be reliably obtained using N > ∼ 64 3 particles. Finally, simulations in which the gas can cool radiatively are characterized by the presence in the cluster inner regions of high levels of turbulence, generated by the interaction of the compact cool gas core with the ambient medium. These findings strongly support t...

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Iron abundances and heating of the intracluster medium in hydrodynamical simulations of galaxy clusters

Cited by 81 publications

References 87 publications

Tracing the evolution in the iron content of the intra-cluster medium

Tracing the evolution in the iron content of the intra-cluster medium

Rhapsody-G simulations – II. Baryonic growth and metal enrichment in massive galaxy clusters

The impact of numerical viscosity in SPH simulations of galaxy clusters

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