  Aims. We measured radial metallicity profiles for a sample of ~50 hot,
intermediate redshift galaxy clusters, selected from the XMM-Newton archive.
  Methods. As in our previous paper, we used background modeling rather than
background subtraction, and the Cash statistic rather than the chi square. This
method requires a careful characterization of all background components. We
also performed montecarlo simulations to assess systematic effects.
  Results. The mean metallicity profile shows a peak in the center, and gently
declines out to 0.2 R_{180}. Beyond 0.2 R_{180} the metallicity is roughly 0.2
solar and, at variance with recently published expectations based on
simulations, consistent with being flat. We find no evidence of profile
evolution from z=0.1 to z=0.3. When comparing our mean profile to those
obtained by recent works with BeppoSAX and Chandra, we find remarkable
agreement over the entire radial range.
