Virial Scaling of Massive Dark Matter Halos: Why Clusters Prefer a High Normalization Cosmology

Evrard, A. E.; Bialek, J. J.; Busha, Michael T.; White, Martin; Habib, Salman; Heitmann, Katrin; Warren, Michael S.; Rasia, Elena; Tormen, Giuseppe; Moscardini, L.; Power, Chris; Jenkins, Adrian; Gao, Liang; Frenk, Carlos S.; Springel, Volker; White, Simon D. M.; Diemand, Juerg

doi:10.1086/521616

Cited by 347 publications

(530 citation statements)

References 117 publications

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“…Numerical simulations confirmed that the σv-M∆ relation is consistent with the self-similar scaling with mass (Evrard et al 2008;Munari et al 2013;Saro et al 2013). Some differences may arise from the galaxy population used to estimate the velocity dispersion and from the impact of selection using galaxy colour, projected separation from the cluster centre, galaxy luminosity, and spectroscopic redshift (Saro et al 2013).…”

Section: σV-m∆supporting

confidence: 65%

See 1 more Smart Citation

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

Sereno¹,

Ettori²

2015

Monthly Notices of the Royal Astronomical Society

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The scaling of observable properties of galaxy clusters with mass evolves with time. Assessing the role of the evolution is crucial to study the formation and evolution of massive halos and to avoid biases in the calibration. We present a general method to infer the mass and the redshift dependence, and the time-evolving intrinsic scatter of the mass-observable relations. The procedure self-calibrates the redshift dependent completeness function of the sample. The intrinsic scatter in the mass estimates used to calibrate the relation is considered too. We apply the method to the scaling of mass M ∆ versus line of sight galaxy velocity dispersion σ v , optical richness, X-ray luminosity, L X , and Sunyaev-Zel'dovich signal. Masses were calibrated with weak lensing measurements. The measured relations are in good agreement with time and mass dependencies predicted in the self-similar scenario of structure formation. The lone exception is the L X -M ∆ relation whose time evolution is negative in agreement with formation scenarios with additional radiative cooling and uniform preheating at high redshift. The intrinsic scatter in the σ v -M ∆ relation is notably small, of order of 14 per cent. Robust predictions on the observed properties of the galaxy clusters in the CLASH sample are provided as cases of study. Catalogs and scripts are publicly available at

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Section: σV-m∆supporting

confidence: 65%

“…This is the approach usually followed in numerical simulations (Evrard et al 2008;Munari et al 2013;Saro et al 2013) to built mass proxies based on the velocity dispersion without assuming dynamical equilibrium and without exploiting the properties of the infall patterns.…”

Section: Discussionmentioning

confidence: 99%

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

Sereno¹,

Ettori²

2015

Monthly Notices of the Royal Astronomical Society

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“…These biases are always a result of the velocity dispersion. The virial mass is biased simply because it is directly related to the velocity dispersion (Evrard et al 2008). The caustic mass is biased because the standard "caustic" technique calibrates the escape edge to the velocity dispersion (Diaferio 1999;.…”

Section: Particles Versus Subhalosmentioning

confidence: 99%

Inferring Gravitational Potentials From Mass Densities in Cluster-Sized Halos

Miller

Stark

Gifford

et al. 2016

ApJ

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We use N-body simulations to quantify how the escape velocity in cluster-sized halos maps to the gravitational potential in a ΛCDM universe. Using spherical density-potential pairs and the Poisson equation, we find that the matter density inferred gravitational potential profile predicts the escape velocity profile to within a few percent accuracy for group and cluster-sized halos (10 < < M 1013 200 15 M  , with respect to the critical density). The accuracy holds from just outside the core to beyond the virial radius. We show the importance of explicitly incorporating a cosmological constant when inferring the potential from the Poisson equation. We consider three density models and find that the Einasto and Gamma profiles provide a better joint estimate of the density and potential profiles than the Navarro, Frenk, and White profile, which fails to accurately represent the escape velocity. For individual halos, the 1σ scatter between the measured escape velocity and the density-inferred potential profile is small (<5%). Finally, while the sub-halos show 15% biases in their representation of the particle velocity dispersion profile, the sub-halo escape velocity profile matches the dark matter escape velocity profile to high accuracy with no evidence of velocity bias outside 0.4r 200 .

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“…One of more traditional methods is to apply the virial theorem to the projected phase space distribution of member galaxies (e.g., Zwicky 1937;Yahil & Vidal 1977;Evrard et al 2008), maintaining the assumption that the cluster is in virial equilibrium (and sometimes including the surface term, see The & White 1986). Perhaps the simplest of approaches to measure the mass is to use richness: the number of galaxies associated with the cluster above a certain magnitude limit (e.g., Yee & Ellingson 2003).…”

Section: Introductionmentioning

confidence: 99%

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

Old

Wojtak

Mamon

et al. 2015

Monthly Notices of the Royal Astronomical Society

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This article is the second in a series in which we perform an extensive comparison of various galaxy-based cluster mass estimation techniques that utilise the positions, velocities and colours of galaxies. Our aim is to quantify the scatter, systematic bias and completeness of cluster masses derived from a diverse set of 25 galaxy-based methods using two contrasting mock galaxy catalogues based on a sophisticated halo occupation model and a semi-analytic model. Analysing 968 clusters, we find a wide range in the RMS errors in log M 200c delivered by the different methods (0.18 to 1.08 dex, i.e., a factor of ∼1.5 to 12), with abundance matching and richness methods providing the best results, irrespective of the input model assumptions. In addition, certain methods produce a significant number of catastrophic cases where the mass is under-or over-estimated by a factor greater than 10. Given the steeply falling high-mass end of the cluster mass function, we recommend that richness or abundance matching-based methods are used in conjunction with these methods as a sanity check for studies selecting high mass clusters. We see a stronger correlation of the recovered to input number of galaxies for both catalogues in comparison with the group/cluster mass, however, this does not guarantee that the correct member galaxies are being selected. We do not observe significantly higher scatter for either mock galaxy catalogues. Our results have implications for cosmological analyses that utilise the masses, richnesses, or abundances of clusters, which have different uncertainties when different methods are used.

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Virial Scaling of Massive Dark Matter Halos: Why Clusters Prefer a High Normalization Cosmology

Cited by 347 publications

References 117 publications

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

Inferring Gravitational Potentials From Mass Densities in Cluster-Sized Halos

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

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