  We produce a kinematic analysis of AGN-hosting cluster galaxies from a sample
33 galaxy clusters selected using the X-ray Clusters Database (BAX) and
populated with galaxies from the Sloan Digital Sky Survey (SDSS) Data Release 8
(DR8). The 33 galaxy clusters are delimited by their relative intensity of
member galaxy substructuring as a proxy to core merging to derive two smaller
sub-samples of 8 dynamically active (merging) and 25 dynamically relaxed
(non-merging) states. The AGN were selected for each cluster sub-sample by
employing the WHAN diagram to the strict criteria of
log$_{10}$([NII]/H$\alpha$)$\geq-0.32$ and EW$_{\mathrm{H}\alpha}$ $\geq$
6{\AA}, providing pools of 70 merging and 225 non-merging AGN sub-populations.
By co-adding the clusters to their respective dynamical states to improve the
signal-to-noise of our AGN sub-populations we find that merging galaxy clusters
on average host kinematically active AGN between 0-1.5 $r_{200}$ as
$r_{200}\rightarrow0$, where their velocity dispersion profile (VDP) presents a
significant deviation from the non-AGN sub-population VDP by $\gtrsim3\sigma$.
This result is indicative that the AGN-hosting cluster galaxies have recently
coalesced onto a common potential. Further analysis of the composite
distributions illustrate non-merging AGN-hosting sub-populations have, on
average, already been accreted and predominantly lie within backsplash regions
of the projected phase-space. This suggests merging cluster dynamical states
hold relatively younger AGN sub-populations kinematically compared with those
found in non-merging cluster dynamical states.
