The Build-up of the Colour-Magnitude Relation

By Masayuki Tanaka, T. Kodama, N. Arimoto, S. Okamura, Keiichi Umetsu, K. Shimasaku, I. Tanaka, Toru Yamada. Proceedings of the International Astronomical Union, 2005

166 citations recorded by the source corpus.

Abstract We discuss the build-up of the colour-magnitude relation. The colour-magnitude relation first appears at the bright end and the faint end appears later. Interestingly, the build-up of colour-magnitude relation is delayed in low density environments. We suggest that galaxies follow the environment-dependent down-sizing evolution.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/302fcfd42b5b6e9ad30f2fbf9f3f3028d9a0519d

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Citations in the corpus

The DEEP2 Galaxy Redshift Survey: the relationship between galaxy properties and environment at z∼ 1 (2006, background): “…probed in such studies has been limited, with galaxies grouped into coarse classifications (such as field, group and cluster populations) and with statistically small spectroscopic sample sizes (e.g. Couch et al. 1998; Treu et al. 2003; Smith et al. 2005; Tanaka et al. 2005; Poggianti et al. 2006).”
Determining the Properties and Evolution of Red Galaxies from the Quasar Luminosity Function (2005, background): “…velocity dispersion or spheroid mass (e.g., Jørgensen 1999; Trager et al. 2000; Kuntschner et al. 2001; Caldwell et al. 2003; Fontana et al. 2004; Bernardi et al. 2005; Faber et al. 2005; Howell 2005; Tanaka et al. 2005; Gallazzi et al. 2005; Nelan et al. 2005), as we have considered in Figure 21.”
The build-up of the colour-magnitude relation in galaxy clusters since z ~ 0.8 (2006, background): “In a recent study, Tanaka et al. (2005) have investigated the build up of the colour–magnitude relation using deep panoramic imaging of two clusters at z = 0.83 and z = 0.55 respectively.”
Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, unknown): “In a comprehensive study also based on deep, wide-field imaging with the Suprime-Cam at the Subaru Telescope, Tanaka et al. (2005) obtained photometric redshifts based on four or five optical bands and constructed the C-M relations for the two clusters (at z = 0.55 and 0.83) included in the field,…”
UV CONTINUUM SLOPE AND DUST OBSCURATION FROM z ∼ 6 TO z ∼ 2: THE STAR FORMATION RATE DENSITY AT HIGH REDSHIFT (2009, background): “Galaxies in such environments are known to show much greater evolution than galaxies in more typical environments (e.g., Tanaka et al. 2005) and show much greater metal enrichment.”
The importance of satellite quenching for the build-up of the red sequence of present-day galaxies (2007, background): “…C© 2008 RAS Recent studies have shown that the bimodality of the galaxy population already exists at least out to z 1 (e.g. Bell et al. 2004; Tanaka et al. 2005; Cooper et al. 2006; Cucciati et al. 2006; Willmer et al. 2006), and that the total stellar mass density on the red sequence has…”
EVOLUTION OF THE COLOR–MAGNITUDE RELATION IN GALAXY CLUSTERS AT z ∼ 1 FROM THE ACS INTERMEDIATE REDSHIFT CLUSTER SURVEY (2008, background): “…1998; van Dokkum et al. 2000, 2001; Blakeslee et al. 2003a; Bell et al. 2004; De Lucia et al. 2004, 2007; Holden et al. 2004; Lidman et al. 2004; Tanaka et al. 2005; Blakeslee et al. 2006; Cucciati et al. 2006; Franzetti et al. 2007; Homeier et al. 2006; Mei et al. 2006a,b; Stanford et al.…”
Mass downsizing and ``top-down'' assembly of early-type galaxies (2006, background): “…galaxies than in lower mass ones, a trend for which ample evidence is growing both at low and high redshift (Cowie et al. 1996; Thomas et al. 2005; Tanaka et al. 2005; Kodama et al. 2004; van der Wel et al. 2005; Treu et al. 2005; di Serego et al. 2005; Juneau et al. 2005; Feulner et al. 2005;…”
The STAGES view of red spirals and dusty red galaxies: Mass-dependent quenching of star formation in cluster infall (2008, background): “…have similarities with lower redshift cluster outskirts giving rise to a ‘double downsizing’ picture where SF moves progressively to lower mass objects as you move either forward in cosmic time or higher in density of the environment (Kauffmann et al. 2004; Smith et al. 2005; Tanaka et al. 2005).”
Properties of galaxy groups in the Sloan Digital Sky Survey – I. The dependence of colour, star formation and morphology on halo mass (2005, background): “Important hints come from the observed correlations between galaxy properties and environment: galaxies in dense environments (i.e. clusters) have predominantly early-type morphologies (e.g. Oemler 1974; Dressler 1980; Whitmore, Gilmore & Jones 1993) and low SFRs (e.g. Balogh et al. 1997, 1999; Pogg”
A STELLAR MASS THRESHOLD FOR QUENCHING OF FIELD GALAXIES (2012, background): “A well-established color bimodality is seen in the local distribution of luminous galaxies (e.g., Baldry et al. 2006; Tanaka et al. 2005; Blanton et al. 2005a; Blanton & Moustakas 2009) and appears already in place at redshifts above z ∼ 1 (Bell et al. 2004; Cooper et al. 2007).”
Environment and self-regulation in galaxy formation (2009, background): “The same colour evolution for both field and cluster galaxies is found in recent redshift surveys (Wolf et al. 2003; Bell et al. 2004; Koo et al. 2005; Tanaka et al. 2005; Bundy et al. 2006).”