  We present a systematic analysis of XMM-Newton observations of 8 cool-core
clusters of galaxies and determine the Fe distribution in the intracluster
medium relative to the stellar distribution in the central dominant galaxy
(CDG). Our analysis shows that the Fe is significantly more extended than the
stellar mass in the CDG in all of the clusters in our sample, with a slight
trend of increasing extent with increasing central cooling time. The excess Fe
within the central 100 kpc in these clusters can be produced by Type Ia
supernovae from the CDG over the past 3-7 Gyr. Since the excess Fe primarily
originates from the CDG, it is a useful probe for determining the motion of the
gas and the mechanical energy deposited by AGN outbursts over the past $\sim$ 5
Gyr in the centers of clusters. We explore two possible mechanisms for
producing the greater extent of the Fe relative to the stars in the CDG,
including: bulk expansion of the gas and turbulent diffusion of Fe. Assuming
the gas and Fe expand together, we find that a total energy of $10^{60} -
10^{61}$~erg~s$^{-1}$ must have been deposited into the central 100 kpc of
these clusters to produce the presently observed Fe distributions. Since the
required enrichment time for the excess Fe is approximately 5 Gyr in these
clusters, this gives an average AGN mechanical power over this time of $10^{43}
- 10^{44}$~erg~s$^{-1}$. The extended Fe distribution in cluster cores can also
arise from turbulent diffusion. Assuming steady-state (i.e., the outward mass
flux of Fe across a given surface is equal to the mass injection rate of Fe
within that surface) we find that diffusion coefficients of $10^{29} - 10^{30}$
cm$^2$~s$^{-1}$ are required to maintain the presently observed Fe profiles
(abridged).
