The insignificant evolution of the richness-mass relation of galaxy clusters

Andreon, S.; Congdon, Peter

doi:10.1051/0004-6361/201423616

Cited by 40 publications

(50 citation statements)

References 49 publications

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“…They found that richness scales almost linearly with the projected weak-lensing mass (β Y |X = 1.3 ± 0.3), with a statistically insignificant evolution (γz = −0.7 ± 0.7). The evolution with mass measured in Andreon & Congdon (2014) is steeper than a previous result by Andreon & Bergé (2012), which used spherical masses and projected richnesses to find β Y |X = 0.46 ± 0.12.…”

Section: λ-M∆contrasting

confidence: 70%

“…Wen, Han & Liu (2009) considered a compilation of clusters whose masses had been estimated by X-ray or weak-lensing methods to infer a slope of βY -Z = 1.17 ± 0.03. Andreon & Congdon (2014) studied the mass-richness scaling for a sub-sample of the CCCP clusters (The Canadian Cluster Comparison Project, Hoekstra et al 2012). They found that richness scales almost linearly with the projected weak-lensing mass (β Y |X = 1.3 ± 0.3), with a statistically insignificant evolution (γz = −0.7 ± 0.7).…”

Section: λ-M∆mentioning

confidence: 99%

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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: λ-M∆contrasting

confidence: 70%

Section: λ-M∆mentioning

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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“…Note that the results of this fit have been used to obtain the completeness and purity curves for different observable M * CL in §5.2. The M * CL |M h relation appears not to evolve with redshift, in agreement with other works (Lin et al 2006;Andreon & Congdon 2014;Saro et al 2015). In Fig.…”

Section: Observable-dark Matter Halo Mass Relationsupporting

confidence: 92%

“…Lin et al 2006;Andreon 2010;Andreon & Congdon 2014;Saro et al 2015), we have model the M * CL |M h relation with a log-log relation as follows:…”

Section: Observable-dark Matter Halo Mass Relationmentioning

confidence: 99%

An accurate cluster selection function for the J-PAS narrow-band wide-field survey

Ascaso

Benı́tez

Dupke

et al. 2016

Mon. Not. R. Astron. Soc.

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The impending Javalambre Physics of the accelerating universe Astrophysical Survey (J-PAS) will be the first wide-field survey of 8500 deg 2 to reach the 'stage IV' category. Because of the redshift resolution afforded by 54 narrow-band filters, J-PAS is particularly suitable for cluster detection in the range z<1. The photometric redshift dispersion is estimated to be only ∼ 0.003 with few outliers 4% for galaxies brighter than i ∼ 23 AB, because of the sensitivity of narrow band imaging to absorption and emission lines. Here we evaluate the cluster selection function for J-PAS using N-body+semi-analytical realistic mock catalogues. We optimally detect clusters from this simulation with the Bayesian Cluster Finder, and we assess the completeness and purity of cluster detection against the mock data. The minimum halo mass threshold we find for detections of galaxy clusters and groups with both >80% completeness and purity is M h ∼ 5 × 10 13 M ⊙ up to z ∼ 0.7. We also model the optical observable, M * CL -halo mass relation, finding a non-evolution with redshift and main scatter of σ M * CL |M h ∼ 0.14 dex down to a factor two lower in mass than other planned broad-band stage IV surveys, at least. For the M h ∼ 1 × 10 14 M ⊙ Planck mass limit, J-PAS will arrive up to z ∼ 0.85 with a σ M * CL |M h ∼ 0.12 dex. Therefore J-PAS will provide the largest sample of clusters and groups up to z ∼ 0.8 with a mass calibration accuracy comparable to X-ray data.

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“…However, we would expect the richness and luminosity mass proxies to be strongly dependent on the evolution of the galaxy LF within galaxy groups and clusters. Recent work implies that there may be little evolution in the mass-richness proxy (Andreon & Congdon 2014), though as this work uses a specific subset of galaxies to define richness, the result cannot necessarily be extrapolated to our richness proxy.…”

Section: Uncorrected Effectsmentioning

confidence: 98%