tokens: are fully available in the machine-readable version. We present one catalog for each band, containing the 1730 SDSS+ATLAS cluster galaxies for which the pipelines ProFound + ProFit work. 4. Results We aim to shed light on the formation of S0 galaxies in clusters. In particular, we focus on understanding the relative importance of environmental processes acting in the cluster core and preprocessing acting in the cluster outskirts. We study the g − i colors separately for bulges and disks up to ∼2.5 R 200 , including the infalling cluster regions where galaxies are mainly in groups or isolated. We explore the color–magnitude relations for the two galaxy components. To understand the impact of the environment, we investigate the dependence of the bulge and disk g − i colors on the projected cluster-centric distance R / R 200 and the local galaxy density. We disentangle backsplash and infalling galaxy populations in the PPS. Finally, we compare the results for double-component galaxies with single-component disk-dominated galaxies. 4.1. Color–Magnitude Relations We aim to understand whether the bulge, disk, or both are responsible for the global galaxy color–magnitude relation observed in clusters. The study of the bulge and disk color–magnitude trends helps us to assess the mechanisms that drove the evolution history of the two components. We explore the extinction- and k -corrected bulge and disk g − i colors for the 469 double-component galaxies within 2.5 R 200 and with reliable bulge and disk measurements as described in Section 3.3 . Figure 9 shows the g − i color distributions for the bulges and disks. The disks are mainly shifted toward bluer colors with respect to the bulges. The median g − i offset separating the two distributions is 0.11 ± 0.02 mag. We find that 67% ± 2% of the galaxies have a bulge that is redder than the disk, while for the remaining 33% ± 2%, the bulge is bluer than the disk. Figure 9. Histogram in g − i color for bulges and disks of the 469 double-component galaxies within 2.5 R 200 . The dashed lines represent the median values. Disks are shifted toward bluer colors with respect to bulges by 0.11 ± 0.02 mag. We investigate the g − i color–magnitude relations for double-component galaxies and for bulges and disks in the left and right panels of Figure 10 , respectively. The total absolute magnitude of the galaxy M g has been estimated using , where D L is the luminosity distance measured using the cluster redshift. The k -correction and Milky Way extinction corrections are applied. We fit the g − i color–magnitude values using the Hyper-fit software, which takes into account the random uncertainties associated with the data (Robotham Obreschkow 2015 ). Figure 10. Color–magnitude diagrams for the 469 double-component galaxies within 2.5 R 200 (left panel) and the bulges (red and magenta) and disks (blue and light blue; right panel). In both panels, M g is the total absolute magnitude of the galaxy. The
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