The impact of stochastic gas motions on the metal distribution in cluster core is evaluated .
Peaked abundance profiles are a characteristic feature of clusters with cool cores and abundance peaks are likely associated with the brightest cluster galaxies ( BCGs ) which dwell in cluster cores .
The width of the abundance peaks is however significantly broader than the BCG light distribution , suggesting that some gas motions are transporting metals originating from within the BCG .
Assuming that this process can be treated as diffusive and using the brightest X-ray cluster A426 ( Perseus ) as an example , we estimate that a diffusion coefficient of the order of 2 \times 10 ^ { 29 } ~ { } { cm ^ { 2 } ~ { } s ^ { -1 } } is needed to explain the width of the observed abundance profiles .
Much lower ( higher ) diffusion coefficients would result in too peaked ( too shallow ) profiles .
Such diffusion could be produced by stochastic gas motions and our analysis provides constraints on the product of their characteristic velocity and their spatial coherence scale .
We speculate that the activity of the supermassive black hole of the BCG is driving the stochastic gas motions in cluster cores .
When combined with the assumption that the dissipation of the same motions is a key gas heating mechanism , one can estimate both the velocity and the spatial scale of such a diffusive processes .