  We qualitatively assess and map the relative contribution of pre-processing
and cluster related processes to the build-up of A963, a massive cluster at
z=0.2 showing an unusually high fraction of star forming galaxies in its
interior. We use Voronoi binning of positions of cluster members on the plane
of the sky in order to map the 2D variations of galaxy properties in the centre
and infall region of A963. We map four galaxy parameters (fraction of star
forming galaxies, specific star formation rate, HI deficiency and age of the
stellar population) based on full SED fitting, 21cm imaging and optical
spectroscopy. We find an extended region dominated by passive galaxies along a
north-south axis crossing the cluster centre, possibly associated with known
filaments of the large-scale structure. There are signs that the passive
galaxies in this region were quenched long before their arrival in the vicinity
of the cluster. Contrary to that, to the east and west of the cluster centre
lie regions of recent accretion dominated by gas rich, actively star forming
galaxies not associated with any substructure or filament. The few passive
galaxies in this region appear to be recently quenched, and some gas rich
galaxies show signs of ongoing ram-pressure stripping. We report the first
tentative observations at 21cm of ongoing ram-pressure stripping at z=0.2, as
well as observed inflow of low-entropy gas into the cluster along filaments of
the large-scale structure. The observed galaxy content of A963 is a result of
strongly anisotropic accretion of galaxies with different properties. Gas rich,
star forming galaxies are being accreted from the east and west of the cluster
and these galaxies are being quenched at r<R200, while the bulk of the
accretion, containing multiple groups, happens along the north-south axis and
brings mostly passive galaxies.
