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Fig. 1.


Left panel: B–V colour and total stellar mass distributions for the galaxies inside the nine clusters. On the upper panel we show the distribution for all WINGS galaxies of the nine clusters (grey colour) with available B–V colours from Varela et al. (2009) and at the bottom we show the histogram of the galaxies of this study (red for cluster galaxies and green for non-member galaxies). Right panel: same as on the left, but for the stellar mass. Galaxies of this study have secure structural parameters (available redshift measurements and available morphological classifications). The fact that the total number galaxies of this study (790) is much smaller than the 36414 galaxies of Varela et al. (2009) is due to the lack of spectroscopic data and morphological classification values. The lack of spectroscopic measurements is also responsible for the small number of galaxies (1271) with available stellar mass estimates. Our sample includes the majority (more than 95%) of galaxies (both cluster members and non-members) that have spectroscopic measurements.

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