The colors of bulges and disks in the core and outskirts of galaxy
  clusters
  The role of the environment on the formation of S0 galaxies is still not well
understood, specifically in the outskirts of galaxy clusters. We study eight
low-redshift clusters, analyzing galaxy members up to cluster-centric distances
$\sim2.5\,R_{200}$. We perform 2D photometric bulge-disk decomposition in the
$g$-, $r$- and $i$-bands from which we identify 469 double-component galaxies.
We analyze separately the colors of the bulges and the disks and their
dependence on the projected cluster-centric distance and on the local galaxy
density. For our sample of cluster S0 galaxies, we find that bulges are redder
than their surrounding disks, show a significant color-magnitude trend, and
have colors that do not correlate with environment metrics. On the other hand,
the disks associated with our cluster S0s become significantly bluer with
increasing cluster-centric radius, but show no evidence for a color-magnitude
relation. The disk color-radius relation is mainly driven by galaxies in the
cluster core at $0\leq R/ R_{200}<0.5$. No significant difference is found for
the disk colors of backsplash and infalling galaxies in the projected phase
space. Beyond $R_{200}$, the disk colors do not change with the local galaxy
density, indicating that the colors of double-component galaxies are not
affected by pre-processing. A significant color-density relation is observed
for single-component disk-dominated galaxies beyond $R_{200}$. We conclude that
the formation of cluster S0 galaxies is primarily driven by cluster core
processes acting on the disks, while evidence of pre-processing is found for
single-component disk-dominated galaxies.
  We publicly release the data from the bulge-disk decomposition.
