  When a galaxy falls into a cluster, its outermost parts are the most affected
by the environment. In this paper, we are interested in studying the influence
of a dense environment on different galaxy's components to better understand
how this affects the evolution of galaxies. We use, as laboratory for this
study, the Hydra cluster which is close to virialization; yet it still shows
evidence of substructures. We present a multi-wavelength bulge-disc
decomposition performed simultaneously in 12 bands from S-PLUS data for 52
galaxies brighter than m$_{r}$= 16. We model the galaxies with a Sersic profile
for the bulge and an exponential profile for the disc. We find that the
smaller, more compact, and bulge-dominated galaxies tend to exhibit a redder
colour at a fixed stellar mass. This suggests that the same mechanisms
(ram-pressure stripping and tidal stripping) that are causing the compaction in
these galaxies are also causing them to stop forming stars. The bulge size is
unrelated to the galaxy's stellar mass, while the disc size increases with
greater stellar mass, indicating the dominant role of the disc in the overall
galaxy mass-size relation found. Furthermore, our analysis of the environment
unveils that quenched galaxies are prevalent in regions likely associated with
substructures. However, these areas also harbour a minority of star-forming
galaxies, primarily resulting from galaxy interactions. Lastly, we find that
~37 percent of the galaxies exhibit bulges that are bluer than their discs,
indicative of an outside-in quenching process in this type of dense
environments.
