The Buildup of the Red Sequence in Galaxy Clusters since z ∼ 0.8

By G. Lucia, B. Poggianti, A. Aragón-Salamanca, D. Clowe, C. Halliday, P. Jablonka, B. Milvang-Jensen, R. Pell'o, S. Poirier, G. Rudnick and 15 more. 2004

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We study the rest-frame (U - V) color-magnitude relation in four clusters at redshifts 0.7-0.8, drawn from the ESO Distant Cluster Survey (EDisCS). We confirm that the red-sequence galaxies in these clusters can be described as an old, passively evolving population, and we demonstrate that, by comparison with the Coma Cluster, there has been significant evolution in the stellar mass distribution of red-sequence galaxies since z ∼ 0.75. The EDisCS clusters exhibit a deficiency of low-luminosity passive red galaxies. Defining as "faint" all galaxies in the passive evolution-corrected range 0.4 ≳ L/L* ≳ 0.1, the luminous-to-faint ratio of red-sequence galaxies varies from 0.34 ± 0.06 for the Coma Cluster to 0.81 ± 0.18 for the high-redshift clusters. These results exclude a synchronous formation of all red-sequence galaxies and suggest that a large fraction of the faint red galaxies in current clusters moved on to the red sequence relatively recently. Their star formation activity presumably came to an end at z ≲ 0.8.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

EVOLUTION OF THE COLOR–MAGNITUDE RELATION IN GALAXY CLUSTERS AT z ∼ 1 FROM THE ACS INTERMEDIATE REDSHIFT CLUSTER SURVEY (2008, background): “…et al. 2007, MNRAS, 376, 1445 Couch, W.J. et al. 1998, ApJ, 497, 188 Croton, D.J. et al. 2006, MNRAS, 365, 11 Cucciati et al. 2006, A&A, 458, 39 De Lucia et al. 2004, ApJL, 610, 77 De Lucia, G. et al., 2006, MNRAS, 366, 499 De Lucia, G. et al., 2007, MNRAS, 374, 809 Demarco, R., et al. 2005, A&A,…”
Ages and metallicities of early-type galaxies in the SDSS: new insight into the physical origin of the colour-magnitude and the Mg2-sigmaV relations (2006, background): “…models have been able to reproduce the observed slope and scatter of the CMR and of the Mg2–σV relation by including chemical evolution and strong feedback even in massive galaxies together with metallicity-dependent population synthesis models (Kauffmann & Charlot 1998; De Lucia et al. 2004).”
Galaxy Luminosity Functions to z~1 from DEEP2 and COMBO-17: Implications for Red Galaxy Formation (2005, background): “For example, de Lucia et al. (2004) see a deficit in the number of faint red galaxies in rich clusters at z = 0.8 compared to Coma, and Kodama et al. (2004) detect a similar deficit of faint red galaxies in overdense field regions at z ∼ 1.”
The Evolution of the Star Formation Activity in Galaxies and Its Dependence on Environment (2005, background): “…and in the field (Cowie et al. 1996, Smail et al. 1998, Kodama & Bower 2001, Poggianti et al. 2001, Gavazzi et al. 2002, Kauffmann et al. 2003, De Lucia et al. 2004, Poggianti et al. 2004), galaxies terminating their star formation at higher redshift (e.g. primordial passive galaxies) will be on…”
NOAO Fundamental Plane Survey. II. Age and Metallicity along the Red Sequence from Line-Strength Data (2005, background): “At a somewhat higher redshift of z ≈ 0.75 (lookback time of 7Gyr), De Lucia et al (2004) examined the red sequence in clusters and found a deficiency of a factor of two (compared to Coma) for galaxies with 0.1L∗ L 0.4L∗.”
The stellar masses of 25 000 galaxies at 0.2 ≤ z ≤ 1.0 estimated by the COMBO-17 survey (2006, background): “Importantly, this stellar 8 Kodama et al. (2004) and de Lucia et al. (2004) present deeper data which show some evidence for a deficit of faint red-sequence galaxies at z ∼ 1 compared to the present-day red-sequence galaxy stellar mass function.”
The Origin of Dwarf Ellipticals in the Virgo Cluster (2008, result): “…is consistent with the most recent analysis of the color magnitude relation of clusters at different redshift which all indicate a significant decrease of the fraction of low luminosity objects on the red sequence with increasing z (De Lucia et al. 2004; 2007) from z=0.24 (Smail et al. 1998).”
The many manifestations of downsizing: hierarchical galaxy formation models confront observations (2009, methodology): “A possibly related trend is the increase with time of faint red-sequence galaxies in galaxy clusters (see e.g. De Lucia et al. 2004b, 2007; Gilbank et al. 2008), which may be due to a differential decline of the SSFR. DS in stellar mass: the high-mass end of the stellar mass function (MF) evolves…”
The Rest-Frame Optical Properties of SCUBA Galaxies (2004, background): “…end of the luminosity function in more local clusters may be built up through a different process, involving passive fading or more active threshing/harassment of mid- / late-type disk galaxies accreted by the clusters since z 0:5 1 (Dressler et al. 1997; de Lucia et al. 2004; Kodama et al. 2004).”
Galaxy bimodality versus stellar mass and environment (2006, result): “This supported the suggestion of a transition in galaxy properties around 1010.5 M⊙ (Kauffmann et al. 2003b) and the former is consistent with faint red-sequence galaxies forming more recently (De Lucia et al. 2004; Kodama et al. 2004) but not necessarily in the richest clusters (Andreon 2006).”
Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, background): “These conclusions were reinforced by several other investigators, e.g., Gladders et al. (1998), Kodama et al. (1998), Nelson et al. (2001), De Lucia et al. (2004), and by van Dokkum et al. (2000), who also cautioned about the “progenitor bias” (see below).”
The formation history of elliptical galaxies (2005, methodology): “…descriptions we adopted for modelling the various mixing and exchange processes occurring between different galactic phases (stars and cold gas, hot diffuse gas in the dark matter haloes, and intergalactic gas outside virialized haloes) are essentially the same as those in De Lucia et al. (2004b).”
Dry Mergers in GEMS: The Dynamical Evolution of Massive Early-Type Galaxies (2005, unknown): “There is a deficit of faint redsequence galaxies in z 1 galaxy clusters (Kodama et al. 2004; de Lucia et al. 2004), and those that are present appear to have rather young stellar populations (van der Wel et al. 2004).”
THE STAR FORMATION HISTORIES OF LOCAL GROUP DWARF GALAXIES. I. HUBBLE SPACE TELESCOPE/WIDE FIELD PLANETARY CAMERA 2 OBSERVATIONS (2014, background): “Naively, this trend could be interpreted as evidence against an extension of galaxy ‘downsizing’ (e.g., Cowie et al. 1996; De Lucia et al. 2004; Thomas et al. 2005) to the lowest masses.”
The Build-up of the Colour-Magnitude Relation (2005, background): “Kajisawa et al. (2000), Nakata et al. (2001), Kodama et al. (2004), Toft et al. (2004), and De Lucia et al. (2004) reported the deficit of red faint galaxies in high-redshift (z > 0.7) clusters compared with local clusters.”
Stellar populations of early-type galaxies in different environments - II. Ages and metallicities (2006, result): “This latter possibility is favoured by some recent studies that found a depletion in the luminosity function of red galaxies towards the faint end (Smail et al. 2001; de Lucia et al. 2004).”
The build-up of the colour-magnitude relation in galaxy clusters since z ~ 0.8 (2006, methodology): “The luminous–to–faint ratio we measure for Coma is 0.32 ± 0.06.4 4 In De Lucia et al. (2004) we erroneously used a distance modulus equal to 35.16 (instead of 35.00 used here) corresponding to We have complemented our low redshift comparison sample with a sample of clusters selected from the SDSS.”
Mass-to-Light Ratios of Field Early-Type Galaxies at z ~ 1 from Ultradeep Spectroscopy: Evidence for Mass-dependent Evolution (2005, background): “…such as the decrease of the mass of ’E+A’ galaxies with time (Tran et al. 2003), the lack of star formation in massive galaxies at redshifts z ≤ 1 (De Lucia et al. 2004), the fossil record of star formation in local early-type galaxies (Thomas et al. 2004), and the claim of mass-dependent…”