The Formation of Massive Cluster Galaxies

Mancone, Conor L.; Gonzalez, Anthony H.; Brodwin, M.; Stanford, S. A.; Eisenhardt, Peter; Stern, Daniel; Jones, Christine

doi:10.1088/0004-637x/720/1/284

Cited by 101 publications

(238 citation statements)

References 39 publications

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“…The flat faint-end slope, and the measured M * close to passive evolution predictions of the local cluster galaxy LF, point toward the LF bright end being similar to that of local clusters, beside evolution of the stellar populations. This extends to z ∼ 1.4 previous findings on the early assembly of the massive galaxy populations in the cluster core regions (De Propris et al 1999;Nakata et al 2001;Kodama & Bower 2003;Toft et al 2003;Ellis & Jones 2004;Toft et al 2004;Andreon 2006;Strazzullo et al 2006;De Propris et al 2007;Muzzin et al 2008;Mancone et al 2010). …”

Section: Figsupporting

confidence: 84%

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Strazzullo

Rosati

Pannella

et al. 2010

A&A

130

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We present a multi-wavelength study of galaxy populations in the core of the massive, X-ray luminous cluster XMMU J2235 at z = 1.39, based on high quality VLT and HST photometry at optical and near-infrared wavelengths. We derive luminosity functions in the z, H, and K s bands, approximately corresponding to restframe U, R and z band. These show a faint-end slope consistent with being flat, and a characteristic magnitude M * close to passive evolution predictions of M * of local massive clusters, with a formation redshift z > 2. The color−magnitude and color-mass diagrams show evidence of a tight red sequence (intrinsic scatter < ∼ 0.08) of massive galaxies already in place, with overall old stellar populations and generally early-type morphology. Beside the red colors, these massive (>6 × 10 10 M ) galaxies typically show early-type spectral features, and rest-frame far-UV emission consistent with very low star formation rates (SFR < 0.2 M yr −1 ). Star forming spectroscopic members, with SFR of up to ∼100 M /yr, are all located at clustercentric distances > ∼ 250 kpc, with the central cluster region already appearing effectively quenched. Most part of the cluster galaxies more massive than 6 × 10 10 M within the studied area do not appear to host significant levels of star formation. The high-mass end of the galaxy populations in the core of this cluster appears to be in a very advanced evolutionary stage, not only in terms of formation of the stellar populations, but also of the assembly of the stellar mass. The high-mass end of the galaxy stellar mass function is essentially already in place. The stellar mass fraction estimated within r 500 (∼1%, Kroupa IMF) is already similar to that of local massive clusters. On the other hand, surface brightness distribution modeling of the massive red sequence galaxies may suggest that their size is often smaller than expected based on the local stellar mass vs. size relation. An evolution of the stellar mass vs. size relation might imply that, in spite of the overall early assembly of these sources, their evolution is not complete, and processes like minor (and likely dry) merging might still shape the structural properties of these objects to resemble those of their local counterparts, without substantially affecting their stellar mass or host stellar populations. Nonetheless, a definite conclusion on the actual relevance of size evolution for the studied early-type sample is precluded by possible systematics and biases.

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Section: Figsupporting

confidence: 84%

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Strazzullo

Rosati

Pannella

et al. 2010

A&A

130

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“…These studies show that the number density of passive galaxies rapidly falls beyond z > 1, so that by z ∼ 2 passive sources are no longer the dominant population, even among massive galaxies. However, the observed evolution of massive cluster galaxies up to z ∼ 1 (and also theoretical models, e.g., De Lucia et al 2006) typically suggests early (z 2−3) formation epochs for their stellar populations (e.g., Mei et al 2009;Mancone et al 2010;Strazzullo et al 2010). We might thus expect that the surge in passive galaxies around ten billion years ago occurred differently in different environments.…”

Section: Introductionmentioning

confidence: 95%

Passive galaxies as tracers of cluster environments atz~ 2

Strazzullo

Daddi

Gobat

et al. 2015

A&A

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Even 10 billion years ago, the cores of the first galaxy clusters are often found to host a characteristic population of massive galaxies with already suppressed star formation. Here we search for distant cluster candidates at z ∼ 2 using massive passive galaxies as tracers. With a sample of ∼40 spectroscopically confirmed passive galaxies at 1.3 < z < 2.1, we tuned photometric redshifts of several thousand passive sources in the 2 sq. deg COSMOS field. This allowed us to map their density in redshift slices, probing the largescale structure in the COSMOS field as traced by passive sources. We report here on the three strongest passive galaxy overdensities that we identify in the range 1.5 < z < 2.5. While the actual nature of these concentrations still needs to be confirmed, we discuss their identification procedure and the arguments supporting them as candidate galaxy clusters (probably in the mid-10 13 M range). Although this search approach is probably biased toward more evolved structures, it has the potential of selecting still rare, clusterlike environments close to their epoch of first appearance, enabling new investigations of the evolution of galaxies in the context of structure growth.

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“…They form such a distinctive population that their colours can be used to search for high redshift clusters in wide-field images (e.g., Gladders & Yee 2000;Eisenhardt et al 2008). These predominantly early type galaxies have little or no ongoing star formation subsequent to forming the bulk of their stellar populations and assembling their stellar masses at high redshift (e.g., Kodama & Arimoto 1997;Stanford et al 1998;De Propris et al 1999;Mancone et al 2010;Mei et al 2012 and references herein). However, while their stellar populations and luminosities evolve passively, their morphologies may not, and may also evolve differently from those of similarly passive field galaxies.…”

Section: Introductionmentioning

confidence: 99%

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Propris¹,

Bremer²,

Phillipps³

2016

Mon. Not. R. Astron. Soc.

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Galaxies arrive on the red sequences of clusters at high redshift (z > 1) once their star formation is quenched and evolve passively thereafter. However, we have previously found that cluster red sequence galaxies (CRSGs) undergo significant morphological evolution subsequent to the cessation of star formation, at some point in the past 9-10 Gyr. Through a detailed study of a large sample of cluster red sequence galaxies spanning 0.2 < z < 1.4 we elucidate the details of this evolution. Below z ∼ 0.5 − 0.6 (in the last 5-6 Gyr) there is little or no morphological evolution in the population as a whole, unlike in the previous 4-5 Gyrs. Over this earlier time (i) disklike systems with Sérsic n < 2 progressively disappear, as (ii) the range of their axial ratios similarly decreases, removing the most elongated systems (those consistent with thin disks seen at an appreciable inclination angle), and (iii) radial colour gradients (bluer outwards) decrease in an absolute sense from significant age-related gradients to a residual level consistent with the metallicity-induced gradients seen in low redshift cluster members. The distribution of their effective radii shows some evidence of evolution, consistent with growth of at most a factor < 1.5 between z ∼ 1.4 and z ∼ 0.5, significantly less than for comparable field galaxies, while the distribution of their central (< 1kpc) bulge surface densities shows no evolution at least at z < 1. A simple model involving the fading and thickening of a disk component after comparatively recent quenching (after z ∼ 1.5) around an otherwise passively evolving older spheroid component is consistent with all of these findings.

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The Formation of Massive Cluster Galaxies

Cited by 101 publications

References 39 publications

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Passive galaxies as tracers of cluster environments atz~ 2

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

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