An environmental dependence of the physical and structural properties in
  the Hydra Cluster galaxies
  The nearby Hydra Cluster ($\sim$50 Mpc) is an ideal laboratory to understand,
in detail, the influence of the environment on the morphology and quenching of
galaxies in dense environments. We study the Hydra cluster galaxies in the
inner regions ($1R_{200}$) of the cluster using data from the Southern
Photometric Local Universe Survey (S-PLUS), which uses 12 narrow and broad band
filters in the visible region of the spectrum. We analyse structural (S\'ersic
index, effective radius) and physical (colours, stellar masses and star
formation rates) properties. Based on this analysis, we find that $\sim$88
percent of the Hydra cluster galaxies are quenched. Using the
Dressler-Schectman test approach, we also find that the cluster shows possible
substructures. Our analysis of the phase-space diagram together with DBSCAN
algorithm indicates that Hydra shows an additional substructure that appears to
be in front of the cluster centre, which is still falling into it. Our results,
thus, suggest that the Hydra Cluster might not be relaxed. We analyse the
median S\'ersic index as a function of wavelength and find that for red
($(u-r)\geq$2.3) and early-type galaxies it displays a slight increase towards
redder filters (13 and 18 percent, for red and early-type respectively) whereas
for blue+green ($(u-r)$<2.3) galaxies it remains constant. Late-type galaxies
show a small decrease of the median S\'ersic index toward redder filters. Also,
the S\'ersic index of galaxies, and thus their structural properties, do not
significantly vary as a function of clustercentric distance and density within
the cluster; and this is the case regardless of the filter.
