The double galaxy cluster Abell 2465 - II. Star formation in the cluster
  We investigate the star formation rate and its location in the major merger
cluster Abell 2465 at $z$ = 0.245. Optical properties of the cluster are
described in Paper I. Measurements of the H$\alpha$ and infrared dust emission
of galaxies in the cluster were made with an interference filter centred on the
redshifted line at a wavelength of 817 nm and utilized data from the WISE
satellite 12 $\mu$m band. Imaging in the Johnson $U$ and $B$ bands was
obtained, and along with SDSS $u$ and $r$ was used to study the blue fraction,
which appears enhanced, as a further signatures of star formation in the
cluster. Star formation rates were calculated using standard calibrations. The
total star formation rate normalized by the cluster mass, $\Sigma SFR/M_{cl}$
compared to compilations for other clusters indicate that the components of
Abell 2465 lie above the mean $z$ and $M_{cl}$ relations, suggestive that
interacting galaxy clusters have enhanced star formation. The projected radial
distribution of the star forming galaxies does not follow a NFW profile and is
relatively flat indicating that fewer star forming galaxies are in the cluster
centre. The morphologies of the H$\alpha$ sources within $R_{200}$ for the
cluster as a whole indicate that many are disturbed or merging, suggesting that
a combination of merging or harassment is working.
