The build-up of the colour-magnitude relation in galaxy clusters since z ~ 0.8

By G. Lucia, B. Poggianti, A. Aragón-Salamanca, Simon D. M. White, Dennis Zaritsky, D. Clowe, C. Halliday, P. Jablonka, A. V. D. Linden, B. Milvang-Jensen and 4 more. 2006

191 citations recorded by the source corpus.

Using galaxy clusters from the ESO Distant Cluster Survey, we study how the distribution of galaxies along the colour-magnitude relation has evolved since z ~ 0.8. While red-sequence galaxies in all these clusters are well described by an old, passively evolving population, we confirm our previous finding of a significant evolution in their luminosity distribution as a function of redshift. When compared to galaxy clusters in the local Universe, the high-redshift EDisCS clusters exhibit a significant deficit of faint red galaxies. Combining clusters in three different redshift bins, and defining as `faint' all galaxies in the range 0.4 >~ L/L* >~ 0.1, we find a clear decrease in the luminous-to-faint ratio of red galaxies from z ~ 0.8 to ~0.4. The amount of such a decrease appears to be in qualitative agreement with predictions of a model where the blue bright galaxies that populate the colour-magnitude diagram of high-redshift clusters, have their star formation suppressed by the hostile cluster environment. Although model results need to be interpreted with caution, our findings clearly indicate that the red-sequence population of high-redshift clusters does not contain all progenitors of nearby red-sequence cluster galaxies. A significant fraction of these must have moved on to the red sequence below z ~ 0.8.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d3d6ce0b2252825494937c3648aaa9e93833dae6

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Citations in the corpus

A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62 (2010, unknown): “1.4 (e.g., Bower et al. 1992; Ellis et al. 1997; Stanford et al. 1998; van Dokkum et al. 1998a,b; Blakeslee et al. 2003, 2006; De Lucia et al. 2007; Tran et al. 2007; Lidman et al. 2008; Mei et al. 2009).”
ROBUST OPTICAL RICHNESS ESTIMATION WITH REDUCED SCATTER (2011, background): “…in addition to a zero point (mean color) and scatter, the ridgeline has a slope in color–magnitude space: fainter (less massive) galaxies have bluer colors, possibly reflecting trends from the mass–metallicity relation (e.g., Kodama & Arimoto 1997; Bernardi et al. 2005; De Lucia et al. 2007).”
Galaxy Groups in the SDSS DR4. II. Halo Occupation Statistics (2007, result): “Most of our findings are in good agreement with previous studies (e.g., Y05c, Zandivarez et al. 2006; Robotham et al. 2006) and can be linked to the semianalytical modeling of galaxy formations (e.g., Kang et al. 2005; Zheng et al. 2005; Bower et al. 2006; Croton et al. 2006; De Lucia et al. 2007).”
Weighing the Giants – III. Methods and measurements of accurate galaxy cluster weak-lensing masses (2012, background): “Furthermore, with increasing cluster redshift, the faint end of the cluster red sequence is not well populated (e.g. De Lucia et al. 2007).”
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).”
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).”
Galaxy Masses: A Review (2013, methodology): “Modern galaxy formation models embedded in a Λ-Cold Dark Matter universe can also predict the evolution of the galaxy mass assembly over cosmic time (e.g. De Lucia et al. 2007).”
Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: a Sloan Digital Sky Survey perspective (2008, methodology): “Such a diagram is a powerful tool, able to provide clues on the formation and evolutionary processes of galaxies (see e.g. De Lucia et al. 2007).”
zCOSMOS – 10k-bright spectroscopic sample - The bimodality in the galaxy stellar mass function: exploring its evolution with redshift (2009, background): “…in the local Universe exhibit distinctive bimodal colour distributions (Strateva et al. 2001, Hogg et al. 2002, Blanton et al. 2003), which suggests that different evolution histories exist for galaxies lying on the two sequences (Menci et al. 2005; Scarlata et al. 2007b; De Lucia et al. 2007).”
The many manifestations of downsizing: hierarchical galaxy formation models confront observations (2009, background): “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…”