EVOLUTION OF THE COLOR–MAGNITUDE RELATION IN GALAXY CLUSTERS AT z ∼ 1 FROM THE ACS INTERMEDIATE REDSHIFT CLUSTER SURVEY

By S. Mei, B. Holden, J. Blakeslee, H. C. Ford, M. Franx, N. Homeier, G. Illingworth, M. J. Jee, R. Overzier, M. Postman and 3 more. 2008

157 citations recorded by the source corpus.

We apply detailed observations of the color–magnitude relation (CMR) with the Advanced Camera for Surveys on the Hubble Space Telescope to study galaxy evolution in eight clusters at z≈ 1. The early-type red sequence is well defined and elliptical and lenticular galaxies lie on similar CMRs. We analyze CMR parameters—scatter, slope, and zero point—as a function of redshift, galaxy properties and cluster mass. For bright galaxies (MB < −21 mag), the CMR scatter of the elliptical population in cluster cores is smaller than that of the S0 population, although the two become similar at faint magnitudes (MB > − 21 mag). While the bright S0 population consistently shows larger scatter than the ellipticals, the scatter of the latter increases in the peripheral cluster regions. If we interpret these results as due to age differences, bright elliptical galaxies in cluster cores are, on average, older than S0 galaxies and peripheral elliptical galaxies (by about 0.5 Gyr, using a simple, single-burst solar metallicity stellar population model). The CMR zero point, slope, and scatter in the (U − B)z = 0 rest-frame show no significant evolution out to redshift z ≈ 1.3 or significant dependence on cluster mass. Two of our clusters display CMR zero points that are redder (by ≈2σ) than the average (U − B)z = 0 of our sample. We also analyze the fraction of morphological early-type and late-type galaxies on the red sequence. We find that, while in the majority of the clusters most (80% to 90%) of the CMR population is composed of early-type galaxies, in the highest-redshift, low-mass cluster of our sample, the CMR late-type/early-type fractions are similar (≈50%), with most of the late-type population composed of galaxies classified as S0/a. This trend is not correlated with the cluster's X-ray luminosity, or with its velocity dispersion, and could be a real evolution with redshift.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

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Citations in the corpus

The XMM Cluster Survey:Optical analysis methodology and the first data release (2011, methodology): “…red-sequence has been found to be remarkably homogeneous between clusters at the same redshift and has been detected to z > 1 (Lidman et al. 2008; Mei et al. 2009; Hilton et al. 2009; Papovich et al. 2010), meaning it can be used as a tool for cluster detection out to high redshifts (e.g.…”
A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62 (2010, background): “There is a marked increase in the scatter in the (U − B) color with redshift, which is expected because the cluster galaxies are observed closer in time to when they formed their stellar populations (e.g., Mei et al. 2009; Hilton et al. 2009).”
The realm of the galaxy protoclusters (2016, background): “Massive clusters at z ∼ 1 generally have strong red sequences (e.g., Postman et al., 2005; Blakeslee et al., 2006; van der Wel et al., 2007; Patel et al., 2009; Mei et al., 2009; Muzzin et al., 2012; Foltz et al., 2015).”
REVERSAL OF FORTUNE: CONFIRMATION OF AN INCREASING STAR FORMATION–DENSITY RELATION IN A CLUSTER AT z = 1.62 (2010, background): “However, to reproduce the relatively homogeneous stellar ages measured in massive cluster galaxies atz < 1 (e.g. Blakeslee et al. 2006; Tran et al. 2007; Mei et al. 2009), these IR luminous members cannot maintain such a high SSFR for even a Gyr.”
THE ERA OF STAR FORMATION IN GALAXY CLUSTERS (2013, background): “…NY 12211 ies formed in short, vigorous bursts of star formation at high redshift (z & 2), and evolved passively thereafter (e.g., Stanford et al. 1998; Blakeslee et al. 2006; van Dokkum and van der Marel 2007; Eisenhardt et al. 2008, hereafter E08; Mei et al. 2009; Mancone et al. 2010).”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2014, background): “Here g encodes the color and magnitude of the galaxies, and σrs = 0.05 (Koester et al. 2007; Mei et al. 2009) is the intrinsic spread of the red sequence.”
THE ATACAMA COSMOLOGY TELESCOPE: ACT-CL J0102−4915 “EL GORDO,” A MASSIVE MERGING CLUSTER AT REDSHIFT 0.87 (2011, background): “The high degree of homogeneity observed in these relations and in their stellar population suggests formation at high redshift followed by passive evolution of their galaxies (Bower, Lucey, & Ellis 1992; Barrientos, Schade, & Lopez-Cruz 1996; Ellis et al. 1997; Holden et al. 2005; Mei et al. 2009).”
THE DEAD SEQUENCE: A CLEAR BIMODALITY IN GALAXY COLORS FROM z = 0 to z = 2.5 (2009, background): “Such studies of red sequence galaxies found among the field are complementary to others that target the higher density environments of clusters at z & 1 (e.g., Mei et al. 2009) and proto-clusters at z ∼ 2 (Zirm et al. 2008).”
Galaxy Protoclusters as Drivers of Cosmic Star Formation History in the First 2 Gyr (2017, background): “Stellar population synthesis applied to observational data of cluster galaxies implies high formation redshifts of their stellar content (e.g., Poggianti et al. 1999; Mei et al. 2009; Rettura et al. 2010).”
THE NEXT GENERATION VIRGO CLUSTER SURVEY (NGVS). I. INTRODUCTION TO THE SURVEY (2012, background): “To date, even the most ambitious studies of the CMD have tended to focus on high- and intermediate-luminosity galaxies (e.g., Faber et al. 2007; Brown et al. 2007; Cassata et al. 2007; Mei et al. 2009).”
A GMBCG GALAXY CLUSTER CATALOG OF 55,424 RICH CLUSTERS FROM SDSS DR7 (2010, background): “…colors) and a slightly tilted color magnitude relation, the study of which has a long history, e.g. (Visvanathan & Sandage 1977; Bower et al. 1992; Gladders et al. 1998; López-Cruz et al. 2004; Blakeslee et al. 2003, 2006; De Lucia et al. 2007; Stott et al. 2009; Mei et al. 2009; Hao et al. 2009).”