The dwarf galaxy population in nearby clusters from the KIWICS survey
  We analyse a sample of twelve galaxy clusters, from the Kapteyn IAC WEAVE INT
Cluster Survey (KIWICS) looking for dwarf galaxy candidates. By using
photometric data in the $r$ and $g$ bands from the Wide Field Camera (WFC) at
the 2.5-m Isaac Newton telescope (INT), we select a sample of bright dwarf
galaxies (M$_r$ $\leq$ -15.5 mag) in each cluster and analyse their spatial
distribution, stellar colour, and as well as their S\'ersic index and effective
radius. We quantify the dwarf fraction inside the $R_{200}$ radius of each
cluster, which ranges from $\sim$ 0.7 to $\sim$ 0.9. Additionally, when
comparing the fraction in the inner region with the outermost region of the
clusters, we find that the fraction of dwarfs tends to increase going to the
outer regions. We also study the clustercentric distance distribution of dwarf
and giant galaxies (M$_r$ $<$ -19.0 mag), and in half of the clusters of our
sample, the dwarfs are distributed in a statistically different way as the
giants, with the giant galaxies being closer to the cluster centre. We analyse
the stellar colour of the dwarf candidates and quantify the fraction of blue
dwarfs inside the $R_{200}$ radius, which is found to be less than $\sim$ 0.4,
but increases with distance from the cluster centre. Regarding the structural
parameters, the S\'ersic index for the dwarfs we visually classify as early
type dwarfs tends to be higher in the inner region of the cluster. These
results indicate the role that the cluster environment plays in shaping the
observational properties of low-mass halos.
