Clash: The Concentration-Mass Relation of Galaxy Clusters

Merten, Julian; Meneghetti, M.; Postman, Marc; Umetsu, Keiichi; Zitrin, Adi; Medezinski, Elinor; Nonino, M.; Koekemoer, Anton M.; Melchior, P.; Gruen, David; Moustakas, Leonidas A.; Bartelmann, Matthias; Host, Ö.; Donahue, M.; Coe, Dan; Molino, A.; Jouvel, S.; Monna, A.; Seitz, S.; Czakon, Nicole G.; Lemze, Doron; Sayers, Jack; Balestra, I.; Rosati, P.; Benı́tez, N.; Biviano, A.; Bouwens, Rychard; Bradley, Larry; Broadhurst, Tom; Carrasco, Mauricio; Ford, H. C.; Grillo, C.; Infante, L.; Kelson, Daniel D.; Lahav, O.; Massey, Richard; Moustakas, John; Rasia, Elena; Rhodes, Jason; Vega, Jesús; Zheng, Wei

doi:10.1088/0004-637x/806/1/4

Cited by 196 publications

(296 citation statements)

References 161 publications

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“…However, an arguably better comparison is with the lensing analyses of the CLASH sample of clusters (0.19 < z < 0.89), which mostly consists of relaxed or nearly relaxed clusters (by our definition). Using CLASH strong+weak lensing, Merten et al (2015) found κm = −0.32 ± 0.18 and κ ζ = −0.14±0.52, consistent with our results; incorporating magnification, Umetsu et al (2016) found κm = −0.44±0.19 while fixing κ ζ = −0.668.…”

Section: Nfw Concentration-mass Relationsupporting

confidence: 88%

“…Nevertheless, an extensive body of work now exists, using primarily X-ray and gravitational lensing observations of galaxy clusters (Vikhlinin et al 2006;Voigt & Fabian 2006;Zhang et al 2006;Schmidt & Allen 2007;Mandelbaum et al 2008;Host & Hansen 2011;Newman et al 2013;Okabe et al 2013;Du et al 2015;Merten et al 2015;Shan et al 2015;van Uitert et al 2016). In this work, we revisit the subject using Chandra X-ray observations of a sample of massive, highly dynamically relaxed clusters.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Nfw Concentration-mass Relationsupporting

confidence: 88%

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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“…Among these, the Weighing the Giants (WtG, von der Linden et al 2014a), CLASH (Postman et al 2012;Merten et al 2015;Umetsu et al 2014), and Canadian Cluster Comparison Project (CCCP, Hoekstra et al 2015) programmes offer constraints on our mass bias factor, 1−b, through direct comparison of the lensing masses to the Planck mass proxy, M Yz .…”

Section: Constraints From Gravitational Shearmentioning

confidence: 99%

Planck2015 results

Ade

Aghanim

Arnaud

et al. 2016

A&A

578

156

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We present cluster counts and corresponding cosmological constraints from the Planck full mission data set. Our catalogue consists of 439 clusters detected via their Sunyaev-Zeldovich (SZ) signal down to a signal-to-noise ratio of 6, and is more than a factor of 2 larger than the 2013 Planck cluster cosmology sample. The counts are consistent with those from 2013 and yield compatible constraints under the same modelling assumptions. Taking advantage of the larger catalogue, we extend our analysis to the two-dimensional distribution in redshift and signal-to-noise. We use mass estimates from two recent studies of gravitational lensing of background galaxies by Planck clusters to provide priors on the hydrostatic bias parameter, (1 − b). In addition, we use lensing of cosmic microwave background (CMB) temperature fluctuations by Planck clusters as an independent constraint on this parameter. These various calibrations imply constraints on the present-day amplitude of matter fluctuations in varying degrees of tension with those from the Planck analysis of primary fluctuations in the CMB; for the lowest estimated values of (1 − b) the tension is mild, only a little over one standard deviation, while it remains substantial (3.7σ) for the largest estimated value. We also examine constraints on extensions to the base flat ΛCDM model by combining the cluster and CMB constraints. The combination appears to favour non-minimal neutrino masses, but this possibility does little to relieve the overall tension because it simultaneously lowers the implied value of the Hubble parameter, thereby exacerbating the discrepancy with most current astrophysical estimates. Improving the precision of cluster mass calibrations from the current 10%-level to 1% would significantly strengthen these combined analyses and provide a stringent test of the base ΛCDM model.

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“…Even more difficult is the estimate of clusters masses and mass profiles that are biased by various effects depending on the applied methods. The masses inferred from either X-ray (e.g., Ettori et al 2013;Maughan et al 2016) or optical data are, for example, based on the assumption of dynamical equilibrium, while those obtained by gravitational lensing (e.g., Umetsu et al 2014;Merten et al 2015) require a good knowledge of the geometry of the potential well. Discrepancies by a factor of 2-3 between the masses obtained by various methods have been reported (e.g., Wu & Fang 1997).…”

Section: Introductionmentioning

confidence: 99%

Characterization of Omega-WINGS galaxy clusters

Cariddi

D’Onofrio

Fasano

et al. 2018

A&A

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Context. Galaxy clusters are the largest virialized structures in the observable Universe. Knowledge of their properties provides many useful astrophysical and cosmological information. Aims. Our aim is to derive the luminosity and stellar mass profiles of the nearby galaxy clusters of the Omega-WINGS survey and to study the main scaling relations valid for such systems. Methods. We merged data from the WINGS and Omega-WINGS databases, sorted the sources according to the distance from the brightest cluster galaxy (BCG), and calculated the integrated luminosity profiles in the B and V bands, taking into account extinction, photometric and spatial completeness, K correction, and background contribution. Then, by exploiting the spectroscopic sample we derived the stellar mass profiles of the clusters. Results. We obtained the luminosity profiles of 46 galaxy clusters, reaching r 200 in 30 cases, and the stellar mass profiles of 42 of our objects. We successfully fitted all the integrated luminosity growth profiles with one or two embedded Sérsic components, deriving the main clusters parameters. Finally, we checked the main scaling relation among the clusters parameters in comparison with those obtained for a selected sample of early-type galaxies (ETGs) of the same clusters. Conclusions. We found that the nearby galaxy clusters are non-homologous structures such as ETGs and exhibit a color-magnitude (CM) red-sequence relation very similar to that observed for galaxies in clusters. These properties are not expected in the current cluster formation scenarios. In particular the existence of a CM relation for clusters, shown here for the first time, suggests that the baryonic structures grow and evolve in a similar way at all scales.

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Clash: The Concentration-Mass Relation of Galaxy Clusters

Cited by 196 publications

References 161 publications

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

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

Planck2015 results

Characterization of Omega-WINGS galaxy clusters

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