Mass Accretion and Its Effects on the Self-Similarity of Gas Profiles in the Outskirts of Galaxy Clusters

Lau, Erwin T.; Nagai, Daisuke; Avestruz, Camille; Nelson, Keith E.; Vikhlinin, A.

doi:10.1088/0004-637x/806/1/68

Cited by 121 publications

(158 citation statements)

References 72 publications

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“…The accretion speed reaches a maximum at a radius 2R200,m as found by previous authors (Wetzel & Nagai 2014;More et al 2015;Lau et al 2015). Within this radius the metallicity of the ICM is well described by an equilibrium model in which accretion of low metallicity gas from the intergalactic medium is balanced by the production of metals from star formation events.…”

Section: Summary and Discussionsupporting

confidence: 75%

“…Most state-of-the-art cosmological zoom-in simulations of galaxy clusters reach a spatial resolution of "kpc (Puchwein et al 2008;Teyssier et al 2011;Ettori et al 2012;Martizzi et al 2014b;Le Brun et al 2014;Lau et al 2015;Sembolini et al 2015). Such simulations are challenging since they require a very large dynamic range of scales to be captured: from the scales at which galaxies assemble their stars to the scale at which cosmological gas accretion onto clusters happens.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Summary and Discussionsupporting

confidence: 75%

Section: Introductionmentioning

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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“…where M = M vir and the a 0 -a 1 pairs were chosen manually to correspond to roughly a crossing time (see also Lau et al 2015;More et al 2015;Mansfield et al 2017). As in Paper I, we instead choose M = M 200m and measure the accretion rate over one dynamical time, a 1 ≡ a(t − t dyn ).…”

Section: Tablementioning

confidence: 99%

The Splashback Radius of Halos from Particle Dynamics. II. Dependence on Mass, Accretion Rate, Redshift, and Cosmology

Diemer

Mansfield

Kravtsov

et al. 2017

ApJ

145

159

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The splashback radius R sp , the apocentric radius of particles on their first orbit after falling into a dark matter halo, has recently been suggested as a physically motivated halo boundary that separates accreting from orbiting material. Using the Sparta code presented in Paper I, we analyze the orbits of billions of particles in cosmological simulations of structure formation and measure R sp for a large sample of halos that span a mass range from dwarf galaxy to massive cluster halos, reach redshift 8, and include WMAP, Planck, and self-similar cosmologies. We analyze the dependence of R sp /R 200m and M sp /M 200m on the mass accretion rate Γ, halo mass, redshift, and cosmology. The scatter in these relations varies between 0.02 and 0.1 dex. While we confirm the known trend that R sp /R 200m decreases with Γ, the relationships turn out to be more complex than previously thought, demonstrating that R sp is an independent definition of the halo boundary that cannot trivially be reconstructed from spherical overdensity definitions. We present fitting functions for R sp /R 200m and M sp /M 200m as a function of accretion rate, peak height, and redshift, achieving an accuracy of 5% or better everywhere in the parameter space explored. We discuss the physical meaning of the distribution of particle apocenters and show that the previously proposed definition of R sp as the radius of the steepest logarithmic density slope encloses roughly three-quarters of the apocenters. Finally, we conclude that no analytical model presented thus far can fully explain our results.

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“… - (Lau et al 2015), move in bulk with the halo peculiar velocity, v los (see Section 6.2 for a discussion of velocity substructures), where R 500 is defined in Equation (15). For such an object, we can take v los out of the integrandand write its kSZ contribution as…”

Section: The Ksz Effectmentioning

confidence: 99%

Constraints on the Optical Depth of Galaxy Groups and Clusters

Flender

Nagai

McDonald

2017

ApJ

Self Cite

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Future data from galaxy redshift surveys, combined with high-resolutions maps of the cosmic microwave background, will enable measurements of the pairwise kinematic Sunyaev-Zel'dovich (kSZ) signal with unprecedented statistical significance. This signal probes the matter-velocity correlation function, scaled by the average optical depth (τ) of the galaxy groups and clusters in the sample, and is thus of fundamental importance for cosmology. However, in order to translate pairwise kSZ measurements into cosmological constraints, external constraints on τ are necessary. In this work, we present a new model for the intracluster medium, which takes into account star formation, feedback, non-thermal pressure, and gas cooling. Our semi-analytic model is computationally efficient and can reproduce results of recent hydrodynamical simulations of galaxy cluster formation. We calibrate the free parameters in the model using recent X-ray measurements of gas density profiles of clusters, and gas masses of groups and clusters. Our observationally calibrated model predicts the average 500 t (i.e., the integrated τ within a disk of size R 500 ) to better than 6% modeling uncertainty (at 95% confidence level). If the remaining uncertainties associated with other astrophysical uncertainties and X-ray selection effects can be better understood, our model for the optical depth should break the degeneracy between optical depth and cluster velocity in the analysis of future pairwise kSZ measurements and improve cosmological constraints with the combination of upcoming galaxy and CMB surveys, including the nature of dark energy, modified gravity, and neutrino mass.

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Mass Accretion and Its Effects on the Self-Similarity of Gas Profiles in the Outskirts of Galaxy Clusters

Cited by 121 publications

References 72 publications

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

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

The Splashback Radius of Halos from Particle Dynamics. II. Dependence on Mass, Accretion Rate, Redshift, and Cosmology

Constraints on the Optical Depth of Galaxy Groups and Clusters

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