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 .