The Halo Boundary of Galaxy Clusters in the SDSS

Baxter, Eric J.; Chang, C.; Jain, Bhuvnesh; Adhikari, Susmita; Dalal, Neal; Kravtsov, Andrey V.; More, Surhud; Rozo, Eduardo; Rykoff, E. S.; Sheth, Ravi K.

doi:10.3847/1538-4357/aa6ff0

Cited by 123 publications

(208 citation statements)

References 74 publications

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“…Notably, a similar power law radial distribution of blue galaxies was measured in the SDSS (Baxter et al 2017) and the DES clusters (Shin et al 2018). Given the expectation for the power law profile of infalling population of matter and galaxies, the most straightforward interpretation of this result is that galaxies do not remain blue much beyond the first pericenter passage and that the population of blue galaxies is thus dominated by infalling galaxies on their first approach to the pericenter, as was previously suggested for dwarf galaxy populations in Fornax (Drinkwater et al 2001) and Virgo (Conselice et al 2001) clusters.…”

Section: Discussion Of the Radial Dependence Of Galaxy Stellar Mass Fsupporting

confidence: 63%

Stellar-mass Measurements in A133 with Magellan/IMACS

Starikova

Vikhlinin

Kravtsov

et al. 2020

ApJ

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We present the analysis of deep optical imaging of the galaxy cluster Abell 133 with the IMACS instrument on Magellan. Our multi-band photometry enables stellar mass measurements in the cluster member galaxies down to a mass limit of M = 3×10 8 M (≈ 0.1 of the Large Magellanic Cloud stellar mass). We observe a clear difference in the spatial distribution of large and dwarf galaxies within the cluster. Modeling these galaxies populations separately, we can confidently track the distribution of stellar mass locked in the galaxies to the cluster's virial radius. The extended envelope of the cluster's brightest galaxy can be tracked to ∼ 200 kpc. The central galaxy contributes ∼ 1/3 of the the total cluster stellar mass within the radius r 500c .2 Starikova et al.accessible by current X-ray observations, ∼ 0.5 of the virial radius, are well below the values of the universal baryon fraction derived from Cosmic Microwave Background fluctuations (Vikhlinin et al. 2006;Lin et al. 2012;Eckert et al. 2016), and this is yet to be fully explained by cosmological cluster simulations (e.g., Barnes et al. 2017). Furthermore, the distribution of stellar material and hot gas within clusters should bear the imprint of key processes shaping galaxy formation. Indeed, observed stellar mass fractions and stellar mass function of cluster galaxies have become valuable benchmarks for testing models of feedback in cosmological simulations of cluster formation (e.g., Martizzi et al. 2014Martizzi et al. , 2016Bahé et al. 2017;McCarthy et al. 2017;Cui et al. 2018;Pillepich et al. 2018;Henden et al. 2018). The radial profile of stellar density of the Brightest Cluster Galaxy (BCG), as well as the radial distribution of stellar mass in galaxies are potentially equally powerful constraints on the models (e.g., Martizzi et al. 2014;Bellstedt et al. 2018).Despite recent progress (Gonzalez et al. 2013;Budzynski et al. 2012Budzynski et al. , 2014Kravtsov et al. 2018;Huang et al. 2018), the number of clusters with available accurate measurements of the gas mass, stellar mass in galaxies down to dwarf scales, and stellar material in the outer envelope of the central galaxy remains small. The main goal of this study is to accurately measure the contribution of the stellar populations (individual galaxies and intra-cluster light) to the total baryon budget in the cluster Abell 133.Abell 133 is a massive nearby (z = 0.05695) galaxy cluster with extensive mapping of surrounding distribution of galaxies and filamentary cosmic web structure (Connor et al. 2018(Connor et al. , 2019b, as well as deep X-ray observations by the Chandra X-ray Observatory (Vikhlinin et al. 2006;Vikhlinin 2013; Morandi & Cui 2014, Vikhlinin et al., in preparation). The cluster has a cool core and prominent radio relics indicative of the ongoing merger activity (Randall et al. 2010), although distribution of galaxies does not reveal clear signs of dynamical disturbance (Connor et al. 2018). Hydrostatic equilibrium analysis using X-ray Chandra observations give total mass within t...

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Section: Discussion Of the Radial Dependence Of Galaxy Stellar Mass Fsupporting

confidence: 63%

Stellar-mass Measurements in A133 with Magellan/IMACS

Starikova

Vikhlinin

Kravtsov

et al. 2020

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: 77%

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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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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“…Our main analysis is based on a fiducial cluster sample of 3684 clusters at redshift 0.2<z<0.55 and richness 20<λ<100. We apply the methodology developed in More et al (2016) and Baxter et al (2017) to DES Y1 data and expand the analysis in several aspects compared to previous work in SDSS.…”

Section: Discussionmentioning

confidence: 99%

“…We model the effects of mis-centering following the approach of Melchior et al (2017) and Baxter et al (2017). The mis-centered density profile, Σ, can be related to the profile in the absence of mis-centering, Σ 0 , via…”

Section: Cluster Mis-centeringmentioning

confidence: 99%

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

Chang¹,

Baxter²,

Jain³

et al. 2018

ApJ

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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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The Halo Boundary of Galaxy Clusters in the SDSS

Cited by 123 publications

References 74 publications

Stellar-mass Measurements in A133 with Magellan/IMACS

Stellar-mass Measurements in A133 with Magellan/IMACS

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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