  We investigate the spatial distribution of iron in the intra-cluster medium
in a selected sample of 41 relaxed clusters in the redshift range $0.05 < z <
1.03$ using {\sl Chandra} archival data. We compute the azimuthally-averaged,
deprojected $Z_{\rm Fe}$ profile of each cluster out to $\sim 0.4r_{500}$, and
identify a peak in the distribution of iron followed by a flatter distribution
at larger radii. Due to the steep gradient both in gas density and abundance,
we find that the emission-weighted iron abundance within $0.2r_{500}$, which
entirely includes the iron peak in most of the cases, is on average $\sim$25\%
higher than the mass-weighted value, showing that spatially resolved analysis
and accurate deprojection are key to study the evolution of iron enrichment in
the very central regions of cool core clusters. We quantify the extent of the
iron distribution in each cluster with a normalized scale parameter $r_{\rm
Fe}$, defined as the radius where the iron abundance excess is half of its peak
value. We find that $r_{\rm Fe}$ increases by a factor of $\sim 3$ from $z\sim
1$ to $z\sim 0.1$, suggesting that the spatial distribution of iron in the ICM
extends with time, possibly due to the mixing with the mechanical-mode feedback
from the central galaxy. We also find that the iron mass excess within
$0.3r_{500}$, when normalized to the total baryonic mass within the same
region, does not evolve significantly, showing that this iron mass component is
already established at $z\sim 1$.
