Abell 2384: the galaxy population of a cluster post-merger
  We combine multi-object spectroscopy from the 2dF and EFOSC2 spectrographs
with optical imaging of the inner 30'x30' of A2384 taken with the ESO Wide
Field Imager. We carry out a kinematical analysis using the EMMIX algorithm and
biweight statistics. We address the possible presence of cluster substructures
with the Dressler-Shectman test. Cluster galaxies are investigated with respect
to [OII] and H{\alpha} equivalent width. Galaxies covered by our optical
imaging observations are additionally analysed in terms of colour, star
formation rate and morphological descriptors such as Gini coefficient and M20
index. We study cluster galaxy properties as a function of clustercentric
distance and investigate the distribution of various galaxy types in
colour-magnitude and physical space. The Dressler-Shectman test reveals a
substructure in the east of the 2dF field-of-view. We determine the mass ratio
between the northern and southern subcluster to be 1.6:1. In accordance with
other cluster studies, we find that a large fraction of the disk galaxies close
to the cluster core show no detectable star formation. Probably these are
systems which are quenched due to ram-pressure stripping. The sample of
quenched disks populates the transition area between the blue cloud and the red
sequence in colour-magnitude space. We also find a population of
morphologically distorted galaxies in the central cluster region. The
substructure in the east of A2384 might be a group of galaxies falling onto the
main cluster. We speculate that our sample of quenched spirals represents an
intermediate phase in the ram-pressure driven transformation of infalling field
spirals into cluster S0s. This is motivated by their position in
colour-magnitude space. The occurrence of morphologically distorted galaxies in
the cluster core complies with the hypothesis of A2384 representing a post
merger system.
