Detection of the Splashback Radius and Halo Assembly Bias of Massive Galaxy Clusters

More, Surhud; Miyatake, Hironao; Takada, Masahiro; Diemer, Benedikt; Kravtsov, Andrey V.; Dalal, Neal; More, Anupreeta; Murata, Ryoma; Mandelbaum, Rachel; Rozo, Eduardo; Rykoff, E. S.; Oguri, Masamune; Spergel, David N.

doi:10.3847/0004-637x/825/1/39

Cited by 196 publications

(299 citation statements)

References 69 publications

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“…It refers to the dark matter halo assembly bias (Gao et al 2005;Croton et al 2007), whose inference requires the identification of isolated halo samples. Supporting evidence has been reported by Miyatake et al (2016) in massive clusters, and later expanded by More et al (2016).…”

Section: Introductionsupporting

confidence: 59%

A 3D Voronoi+Gapper Galaxy Cluster Finder in Redshift Space to z ∼ 0.2 I: an Algorithm Optimized for the 2dFGRS

Pereira

Campusano

Hitschfeld

et al. 2017

ApJ

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This paper is the first in a series, presenting a new galaxy cluster finder based on a three-dimensional Voronoi Tesselation plus a maximum likelihood estimator, followed by gapping-filtering in radial velocity(VoML+G). The scientific aim of the series is a reassessment of the diversity of optical clusters in the local universe. A mock galaxy database mimicking the southern strip of the magnitude(blue)-limited 2dF Galaxy Redshift Survey (2dFGRS), for the redshift range 0.009<z<0.22, is built on the basis of the Millennium Simulation of the LCDM cosmology and a reference catalog of "Millennium clusters," spannning across the 1.0×1012 -1.0×1015 M e h −1 dark matter (DM) halo mass range, is recorded. The validation of VoML+G is performed through its application to the mock data and the ensuing determination of the completeness and purity of the cluster detections by comparison with the reference catalog. The execution of VoML+G over the 2dFGRS mock data identified 1614 clusters, 22% with N g 10, 64 percent with 10>N g 5, and 14% with N g <5. The ensemble of VoML+G clusters has a ∼59% completeness and a ∼66% purity, whereas the subsample with N g 10, to z∼0.14, has greatly improved mean rates of ∼75% and ∼90%, respectively. The VoML+G cluster velocity dispersions are found to be compatible with those corresponding to "Millennium clusters" over the 300-1000 km s −1 interval, i.e., for cluster halo masses in excess of ∼3.0×1013 M e h −1 .

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Section: Introductionsupporting

confidence: 59%

A 3D Voronoi+Gapper Galaxy Cluster Finder in Redshift Space to z ∼ 0.2 I: an Algorithm Optimized for the 2dFGRS

Pereira

Campusano

Hitschfeld

et al. 2017

ApJ

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“…More et al (2015) adopted the definition of R sp as the radius where the density profile reaches its steepest slope and investigated its dependence on mass accretion rate and redshift. Finally, More et al (2016, see also Adhikari et al 2016and Baxter et al 2017) detected a sharp drop in the stacked density …”

mentioning

confidence: 78%

“…The measurement of R sp performed by More et al (2016) and confirmed by Baxter et al (2017) indicates a surprisingly small splashback radius, namely, R sp /R 200m = 0.837 ± 0.031 for a cluster sample with ν = 2.4 at z = 0.24. While we cannot directly measure the mass accretion rate of the clusters, Figure 3 clearly shows that the theoretically expected value is higher.…”

Section: Compatibility With Observationsmentioning

confidence: 89%

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

Diemer

Mansfield

Kravtsov

et al. 2017

ApJ

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143

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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“…However, the Einasto model is sufficiently flexible that even without such a truncation, it can still reproduce a splashbacklike steepening in the outer halo profile. Consequently, the evidence for splashback quantified either with a Δχ 2 (as in More et al 2016) or with a Bayesian evidence ratio (as in B17) can be misleadingly low, even when there is significant steeping of the outer halo profile. This problem becomes more severe when additional flexibility is introduced to the model to account for halo mis-centering, for example.…”

Section: Introductionmentioning

confidence: 99%

The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles

Chang¹,

Baxter²,

Jain³

et al. 2018

ApJ

101

131

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Splashback refers to the process of matter that is accreting onto a dark matter halo reaching its first orbital apocenter and turning around in its orbit. The clustercentric radius at which this process occurs, r sp , defines a halo boundary that is connected to the dynamics of the cluster. A rapid decline in the halo profile is expected near r sp . We measure the galaxy number density and weak lensing mass profiles around REDMAPPER galaxy clusters in the first-year Dark Energy Survey (DES) data. For a cluster sample with mean M 200m mass ≈2.5×1014 M e , we find strong evidence of a splashback-like steepening of the galaxy density profile and measure r sp =1.13± 0.07 h −1 Mpc, consistent with the earlier Sloan Digital Sky Survey measurements of More et al. and Baxter et al. Moreover, our weak lensing measurement demonstrates for the first time the existence of a splashback-like steepening of the matter profile of galaxy clusters. We measure r sp =1.34±0.21 h −1 Mpc from the weak lensing data, in good agreement with our galaxy density measurements. For different cluster and galaxy samples, we find that, consistent with ΛCDM simulations, r sp scales with R 200m and does not evolve with redshift over the redshift range of 0.3-0.6. We also find that potential systematic effects associated with the REDMAPPER algorithm may impact the location of r sp . We discuss the progress needed to understand the systematic uncertainties and fully exploit forthcoming data from DES and future surveys, emphasizing the importance of more realistic mock catalogs and independent cluster samples.

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Detection of the Splashback Radius and Halo Assembly Bias of Massive Galaxy Clusters

Cited by 196 publications

References 69 publications

A 3D Voronoi+Gapper Galaxy Cluster Finder in Redshift Space to z ∼ 0.2 I: an Algorithm Optimized for the 2dFGRS

A 3D Voronoi+Gapper Galaxy Cluster Finder in Redshift Space to z ∼ 0.2 I: an Algorithm Optimized for the 2dFGRS

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

The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles

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