  We compare the observed peaked iron abundance profiles for a small sample of
groups and clusters with the predictions of a simple model involving the metal
ejection from the brightest galaxy and the subsequent diffusion of metals by
stochastic gas motions. Extending the analysis of Rebusco et al. (2005) we
found that for 5 out of 8 objects in the sample an effective diffusion
coefficient of the order of $10^{29}$ cm$^{2}$ s$^{-1}$ is needed. For AWM4,
Centaurus and AWM7 the results are different suggesting substantial
intermittence in the process of metal spreading across the cluster. There is no
obvious dependence of the diffusion coefficient on the mass of the system.
  We also estimated the characteristic velocities and the spatial scales of the
gas motions needed to balance the cooling losses by the dissipation of the same
gas motions. A comparison of the derived spatial scales and the sizes of
observed radio bubbles inflated in the ICM by a central active galactic nucleus
(AGN) suggests that the AGN/ICM interaction makes an important (if not a
dominant) contribution to the gas motions in the cluster cores.
