Cosmological Simulations of Galaxy Clusters

Borgani, S.; Kravtsov, Andrey V.

doi:10.1166/asl.2011.1209

Cited by 162 publications

(171 citation statements)

References 246 publications

(312 reference statements)

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“…The evolution of the collision-less dark matter is relatively easily implemented, but including the effects of baryons has proven to be more complicated. For a recent review on cosmological simulations of galaxy clusters we refer the interested reader to Borgani & Kravtsov (2011).…”

Section: Interpretation Of Scaling Relations With Simulationsmentioning

confidence: 99%

Scaling Relations for Galaxy Clusters: Properties and Evolution

et al. 2013

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Well-calibrated scaling relations between the observable properties and the total masses of clusters of galaxies are important for understanding the physical processes that give rise to these relations. They are also a critical ingredient for studies that aim to constrain cosmological parameters using galaxy clusters. For this reason much effort has been spent during the last decade to better understand and interpret relations of the properties of the intra-cluster medium. Improved X-ray data have expanded the mass range down to galaxy groups, whereas SZ surveys have openened a new observational window on the intracluster medium. In addition, continued progress in the performance of cosmological simulations has allowed a better understanding of the physical processes and selection effects affecting the observed scaling relations. Here we review the recent literature on various scaling relations, focussing on the latest observational measurements and the progress in our understanding of the deviations from self similarity.

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Section: Interpretation Of Scaling Relations With Simulationsmentioning

confidence: 99%

Scaling Relations for Galaxy Clusters: Properties and Evolution

et al. 2013

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“…For an extensive review, see Borgani & Kravtsov (2011). However in the near future, many wide-field surveys are expected to use the cluster mass function to constrain cosmological parameters (Pillepich et al 2012;Laureijs et al 2011;Sartoris et al 2015;Boldrin et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The universality of the virial halo mass function and models for non-universality of other halo definitions

Despali¹,

Giocoli²,

Angulo³

et al. 2015

Mon. Not. R. Astron. Soc.

246

323

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The abundance of galaxy clusters can constrain both the geometry and growth of structure in our Universe. However, this probe could be significantly complicated by recent claims of nonuniversality -non-trivial dependences with respect to the cosmological model and redshift. In this work we analyse the dependance of the mass function on the way haloes are identified and establish if this can cause departures from universality. In order to explore this dependance, we use a set of different N-body cosmological simulations (Le SBARBINE simulations), with the latest cosmological parameters from the Planck collaboration; this first suite of simulations is followed by a lower resolution set, carried out with different cosmological parameters. We identify dark matter haloes using a Spherical Overdensity algorithm with varying overdensity thresholds (virial, 2000ρ c , 1000ρ c , 500ρ c , 200ρ c and 200ρ b ) at all redshifts. We notice that, when expressed in term of the rescaled variable ν, the mass function for virial haloes is a nearly universal as a function of redshift and cosmology, while this is clearly not the case for the other overdensities we considered. We provide fitting functions for the halo mass function parameters as a function of overdensity, that allow to predict, to within a few percent accuracy, the halo mass function for a wide range of halo definitions, redshifts and cosmological models. We then show how the departures from universality associated with other halo definitions can be derived by combining the universality of the virial definition with the expected shape of the density profile of halos.

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“…Jenkins et al 2001;Evrard et al 2002;Tinker et al 2008), the ratio of baryonic mass to CDM in galaxy clusters (e.g. Eke et al 1998;Kay et al 2004;Borgani & Kravtsov 2011), and the distribution of mass within the structures that form hierarchically in the Universe (e.g. Bullock et al 2001;Navarro et al 2004Navarro et al , 1997Gao et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Cosmology and astrophysics from relaxed galaxy clusters – V. Consistency with cold dark matter structure formation

Mantz

Allen

Morris

2016

Mon. Not. R. Astron. Soc.

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This is the fifth in a series of papers studying the astrophysics and cosmology of massive, dynamically relaxed galaxy clusters. Our sample comprises 40 clusters identified as being dynamically relaxed and hot in Papers I and II of this series. Here we use constraints on cluster mass profiles from X-ray data to test some of the basic predictions of cosmological structure formation in the Cold Dark Matter (CDM) paradigm. We present constraints on the concentration-mass relation for massive clusters, finding a power-law mass dependence with a slope of κ m = −0.16 ± 0.07, in agreement with CDM predictions. For this relaxed sample, the relation is consistent with a constant as a function of redshift (power-law slope with 1 + z of κ ζ = −0.17 ± 0.26), with an intrinsic scatter of σ ln c = 0.16 ± 0.03. We investigate the shape of cluster mass profiles over the radial range probed by the data (typically ∼ 50 kpc-1 Mpc), and test for departures from the simple Navarro, Frenk & White (NFW) form, for which the logarithmic slope of the density profile tends to −1 at small radii. Specifically, we consider as alternatives the generalized NFW (GNFW) and Einasto parametrizations. For the GNFW model, we find an average value of (minus) the logarithmic inner slope of β = 1.02 ± 0.08, with an intrinsic scatter of σ β = 0.22 ± 0.07, while in the Einasto case we constrain the average shape parameter to be α = 0.29 ± 0.04 with an intrinsic scatter of σ α = 0.12 ± 0.04. Our results are thus consistent with the simple NFW model on average, but we clearly detect the presence of intrinsic, cluster-to-cluster scatter about the average.

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Cosmological Simulations of Galaxy Clusters

Cited by 162 publications

References 246 publications

Scaling Relations for Galaxy Clusters: Properties and Evolution

Scaling Relations for Galaxy Clusters: Properties and Evolution

The universality of the virial halo mass function and models for non-universality of other halo definitions

Cosmology and astrophysics from relaxed galaxy clusters – V. Consistency with cold dark matter structure formation

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