Thermodynamical Properties of the ICM from Hydrodynamical Simulations

Borgani, S.; Diaferio, Antonaldo; Dolag, K.; Schindler, S.

doi:10.1007/s11214-008-9317-4

Cited by 38 publications

(27 citation statements)

References 101 publications

(121 reference statements)

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“…Kaiser 1986). Attempts to reproduce the observed L X − T relation with hydrodynamic simulations of clusters have been pursued by several groups (see Borgani et al 2008a, for a recent review). Simulations of galaxy clusters including the effect of star formation and SN feedback in the form of energy‐driven galactic winds produce results which are close to observations at the scale of clusters, while generally producing too luminous galaxy groups (e.g.…”

Section: Thermal Properties Of the Icmmentioning

confidence: 99%

Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters

Fabjan¹,

Borgani²,

Tornatore³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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311

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We present a study of the effect of active galactic nuclei (AGN) feedback on metal enrichment and thermal properties of the intracluster medium (ICM) in hydrodynamical simulations of galaxy clusters. The simulations are performed using a version of the TreePM–sphgadget‐2 code, which also follows chemodynamical evolution by accounting for metal enrichment contributed by different stellar populations. We carry out cosmological simulations for a set of galaxy clusters, covering the mass range M200≃ (0.1–2.2) × 1015 h−1 M⊙. Besides runs not including any efficient form of energy feedback, we carry out simulations including three different feedback schemes: (i) kinetic feedback in the form of galactic winds triggered by supernova explosions; (ii) AGN feedback from gas accretion on to supermassive black holes (BHs) and (iii) AGN feedback in which a ‘radio mode’ is included with an efficient thermal coupling of the extracted energy, whenever BHs enter in a quiescent accretion phase. Besides investigating the resulting thermal properties of the ICM, we analyse in detail the effect that these feedback models have on the ICM metal enrichment. We find that AGN feedback has the desired effect of quenching star formation in the brightest cluster galaxies at z < 4 and provides correct temperature profiles in the central regions of galaxy groups. However, its effect is not yet sufficient to create ‘cool cores’ in massive clusters while generating an excess of entropy in central regions of galaxy groups. As for the pattern of metal distribution, AGN feedback creates a widespread enrichment in the outskirts of clusters, thanks to its efficiency in displacing enriched gas from galactic haloes to the intergalactic medium. This turns into profiles of iron abundance, ZFe, which are in better agreement with observational results, and into a more pristine enrichment of the ICM around and beyond the cluster virial regions. Following the pattern of the relative abundances of silicon and iron, we conclude that a significant fraction of the ICM enrichment is contributed in simulations by a diffuse population of intracluster stars. Our simulations also predict that profiles of the ZSi/ZFe abundance ratio do not increase at increasing radii, at least out to 0.5Rvir. Our results clearly show that different sources of energy feedback leave distinct imprints in the enrichment pattern of the ICM. They further demonstrate that such imprints are more evident when looking at external regions, approaching the cluster virial boundaries.

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Section: Thermal Properties Of the Icmmentioning

confidence: 99%

Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters

Fabjan¹,

Borgani²,

Tornatore³

et al. 2010

Monthly Notices of the Royal Astronomical Society

Self Cite

250

311

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“…This model also assumes clusters to have spherical symmetry and to be in HE (e.g. Borgani et al 2008; see also Kravtsov & Borgani 2012 for a recent review and extensions of this model).…”

Section: Galaxy Clusters: Self-similar Modelmentioning

confidence: 99%

Large-Scale Structure Formation: From the First Non-linear Objects to Massive Galaxy Clusters

2014

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The large-scale structure of the Universe formed from initially small perturbations in the cosmic density field, leading to galaxy clusters with up to 10 15 M at the present day. Here, we review the formation of structures in the Universe, considering the first primordial galaxies and the most massive galaxy clusters as extreme cases of structure formation where fundamental processes such as gravity, turbulence, cooling and feedback are particularly relevant. The first non-linear objects in the Universe formed in dark matter halos with 10 5 − 10 8 M at redshifts 10 − 30, leading to the first stars and massive black holes. At later stages, larger scales became non-linear, leading to the formation of galaxy clusters, the most massive objects in the Universe. We describe here their formation via gravitational processes, including the self-similar scaling relations, as well as the observed deviations from such self-similarity and the related non-gravitational physics (cooling, stellar feedback, AGN). While on intermediate cluster scales the self-similar model is in good agreement with the observations, deviations from such self-similarity are apparent in the core regions, where numerical simulations do not reproduce the current observational results. The latter indicates that the interaction of different feedback processes may not be correctly accounted for in current simulations. Both in the most massive clusters of galaxies as well as during the formation of the first objects in the Universe, turbulent structures and shock waves appear to be common, suggesting them to be ubiquitous in the non-linear regime.

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“…11 we show the L X − M relation for four redshift bins, namely 0 < z ≤ 0.25, 0.25 < z ≤ 0.5, 0.5 < z ≤ 0.75, and 0.75 < z ≤ 1. Numerical simulations are known to be poor at describing the X-ray properties of the cosmic structures on the scales of groups (Borgani et al 2008). Thus, we limit our analysis to clusters of masses M vir > 10 14 h −1 M .…”

Section: X-ray Luminositiesmentioning

confidence: 99%

Strong lensing in the MARENOSTRUM UNIVERSE

Meneghetti

Fedeli

Pace

et al. 2010

A&A

152

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Context. Strong lensing is one of the most direct probes of mass distribution in the inner regions of galaxy clusters. It can be used to constrain the density profiles and to measure the mass of the lenses. Moreover, the abundance of strong lensing events can be used to constrain structure formation and cosmological parameters through the so-called "arc-statistics" approach. However, several issues related to the use of strong lensing clusters in cosmological applications are still controversial, leading to the suspicion that several biases may affect this very peculiar class of objects. Aims. With this study we aim a better understanding of the properties of galaxy clusters that can potentially act as strong lenses. Methods. We do so by investigating the properties of a large sample of galaxy clusters extracted from the N-body/hydrodynamical simulation MareNostrum Universe. We perform ray-tracing simulations with each of them and identify those objects capable of producing strong lensing effects. We explore the correlation between the cross section for lensing and many properties of clusters, such as mass, three-dimensional and projected shapes, their concentrations, the X-ray luminosity, and the dynamical activity. Results. We quantify the minimal cluster mass required for producing both multiple images and large distortions. While we do not measure a significant excess of triaxiality in strong lensing clusters, we find that the probability of strong alignments between the major axes of the lenses and the line of sight is a growing function of the lensing cross section. In projection, the strong lenses appear rounder within R 200 , but we find that their cores tend to be more elliptical as the lensing cross section increases. As a result of the orientation bias, we also find that the cluster concentrations estimated from the projected density profiles tend to be biased high. The X-ray luminosity of strong lensing clusters tend to be higher than for normal lenses of similar mass and redshift. This is particularly significant for the least massive lenses. Finally, we find that the strongest lenses generally exhibit an excess of kinetic energy within the virial radius, thus indicating that they are more dynamically active than the usual clusters. Conclusions. We conclude that strong lensing clusters are a very peculiar class of objects, affected by many selection biases that need to be properly modeled when using them to study the inner structure of galaxy clusters or to constrain the cosmological parameters.

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Thermodynamical Properties of the ICM from Hydrodynamical Simulations

Cited by 38 publications

References 101 publications

Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters

Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters

Large-Scale Structure Formation: From the First Non-linear Objects to Massive Galaxy Clusters

Strong lensing in the MARENOSTRUM UNIVERSE

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