On the Origin of the Scatter in the Red Sequence: An Analysis of Four CLASH Clusters

Connor, Thomas; Kelson, Daniel D.; Donahue, M.; Moustakas, John

doi:10.3847/1538-4357/ab0d84

Cited by 15 publications

(10 citation statements)

References 55 publications

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“…Other works (e.g., Muzzin et al 2007;Strazzullo et al 2006;De Propris 2017) have found that the faint-end of the cluster LF is dominated by blue galaxies, which would explain the discrepancy between our results and red-sequence-only results. Alternatively, Connor et al (2019) found that the traditional model of the red sequence as a sloped line does not hold at fainter magnitudes. This could cause a drop-off in the measured…”

Section: Comparisons At Similar Redshiftmentioning

confidence: 96%

The Massive and Distant Clusters of WISE Survey XI: Stellar Mass Fractions and Luminosity Functions of MaDCoWS Clusters at $z \sim 1$

Decker,

Brodwin,

Saha

et al. 2021

Preprint

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We present stellar mass fractions and composite luminosity functions (LFs) for a sample of 12 clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS) at a redshift range of 0.951 ≤ z ≤ 1.43. Using SED fitting of optical and deep mid-infrared photometry, we establish the membership of objects along the lines-of-sight to these clusters and calculate the stellar masses of member galaxies. We find stellar mass fractions for these clusters largely consistent with previous works, including appearing to display a negative correlation with total cluster mass. We measure a composite 3.6 µm LF down to m * + 2.5 for all 12 clusters. Fitting a Schechter function to the LF, we find a characteristic 3.6 µm magnitude of m * = 19.83 ± 0.12 and faint-end slope of α = −0.81 ± 0.10 for the full sample at a mean redshift of z = 1.18. We also divide the clusters into high-and low-redshift bins at z = 1.29 and z = 1.06 respectively and measure a composite LF for each bin. We see a small, but statistically significant evolution in m * and α-consistent with passive evolution-when we study the joint fit to the two parameters, which is probing the evolution of faint cluster galaxies at z ∼ 1. This highlights the importance of deep IR data in studying the evolution of cluster galaxy populations at high-redshift.

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Section: Comparisons At Similar Redshiftmentioning

confidence: 96%

The Massive and Distant Clusters of WISE Survey XI: Stellar Mass Fractions and Luminosity Functions of MaDCoWS Clusters at $z \sim 1$

Decker,

Brodwin,

Saha

et al. 2021

Preprint

Self Cite

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“…Very effective star formation quenching is observed in clusters at all redshifts, where the fraction of star-forming galaxies is lower than in the field (Hashimoto et al 1998), and the fraction of early-type morphologies (lenticulars, ellipticals) is the highest (Dressler 1980). A major thrust of ongoing research is to understand these transitions, particularly using deep HST imaging of clusters (Martinet et al 2017;Wagner et al 2017;Marian et al 2018;Olave-Rojas et al 2018;Connor et al 2019;Rodríguez-Muñoz et al 2019).…”

Section: Galaxy Evolutionmentioning

confidence: 99%

The BUFFALO HST Survey

Steinhardt

Jauzac

Acebrón

et al. 2020

ApJS

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The Beyond Ultra-deep Frontier Fields and Legacy Observations (BUFFALO) is a 101 orbit + 101 parallel Cycle 25 Hubble Space Telescope (HST) Treasury program taking data from 2018 to 2020. BUFFALO will expand existing coverage of the Hubble Frontier Fields (HFF) in Wide Field Camera 3/IR F105W, F125W, and F160W and Advanced Camera for Surveys/WFC F606W and F814W around each of the six HFF clusters and flanking fields. This additional area has not been observed by HST but is already covered by deep multiwavelength data sets, including Spitzer and Chandra. As with the original HFF program, BUFFALO is designed to take advantage of gravitational lensing from massive clusters to simultaneously find high-redshift galaxies that would otherwise lie below HST detection limits and model foreground clusters to study the properties of dark matter and galaxy assembly. The expanded area will provide the first opportunity to study both cosmic variance at high redshift and galaxy assembly in the outskirts of the large HFF clusters. Five additional orbits are reserved for transient followup. BUFFALO data including mosaics, value-added catalogs, and cluster mass distribution models will be released via MAST on a regular basis as the observations and analysis are completed for the six individual clusters.

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“…Some of the galaxies within the cluster, e.g. those with recent bursts of star formation, can be bluer than the red sequence (e.g., Connor et al 2019a). However, there should be very few, if any, galaxies redder than the red sequence members because those members have the oldest stellar Our source detection algorithm fails for such galaxies because it splits them into several objects.…”

Section: Red Sequencementioning

confidence: 99%

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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On the Origin of the Scatter in the Red Sequence: An Analysis of Four CLASH Clusters

Cited by 15 publications

References 55 publications

The Massive and Distant Clusters of WISE Survey XI: Stellar Mass Fractions and Luminosity Functions of MaDCoWS Clusters at $z \sim 1$

The Massive and Distant Clusters of WISE Survey XI: Stellar Mass Fractions and Luminosity Functions of MaDCoWS Clusters at $z \sim 1$

The BUFFALO HST Survey

Stellar-mass Measurements in A133 with Magellan/IMACS

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