Galaxy Systems in the Optical and Infrared by A. Biviano

By A. Biviano

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44 A. Biviano Fig. 19. – The morphological mix of galaxies as a function of clustercentric radius in simulations (dashed line; filled and open squares correspond to bright and faint galaxies) as compared to real data (solid line, from [309]). The agreement is excellent but the definition of ’numerical S0s’ has been widened to include ’numerical early-spirals’, otherwise a deficit of S0s compared to the observational sample would have resulted. From [166]. g. [466]), galaxies in denser environments form earlier, and are more massive than those formed later, because they form with an initially larger mass and undergo more mergers during their lifetime.

Galaxy systems in the optical and infrared 37 population of IR-bright emitters in medium-z clusters, not seen in nearby clusters [356, 357, 358, 359, 360, 361, 362], a phenomenology known as the IR-BOe. The BOe is stronger for fainter galaxies [363, 364] and in the more external parts of galaxy clusters [365, 195]. Altogether, studies of the CMR and BOe indicate that the color evolution of cluster galaxies occurs later for fainter galaxies, in lower-density regions, and in less massive clusters.

The analyses of the CMR, the FP, and the ETG spectra also show that the average age of the ETG stellar population increases with the local density. 44 A. Biviano Fig. 19. – The morphological mix of galaxies as a function of clustercentric radius in simulations (dashed line; filled and open squares correspond to bright and faint galaxies) as compared to real data (solid line, from [309]). The agreement is excellent but the definition of ’numerical S0s’ has been widened to include ’numerical early-spirals’, otherwise a deficit of S0s compared to the observational sample would have resulted.

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