  We use models of the rates of Type Ia supernovae (SNe Ia) and core-collapse
supernovae, built in such a way that both are consistent with recent
observational constraints at z<1.6 and can reproduce the measured cosmic star
formation rate, to recover the history of the metals accumulation in the
intra-cluster medium. We show that these SN rates, in unit of SN number per
comoving volume and rest-frame year, provide on average a total amount of Iron
that is marginally consistent with the value measured in galaxy clusters in the
redshift range 0-1, and a relative evolution with redshift that is in agreement
with the observational constraints up to z~1.2. Moreover, we verify that the
predicted metals to Iron ratios reproduce the measurements obtained in nearby
clusters through X-ray analysis, implying that (1) about half of the Iron mass
and >75 per cent of the Nickel mass observed locally are produced by SN Ia
ejecta, (2) the SN Ia contribution to the metal budget decreases steeply with
redshift and by z~1 is already less than half of the local amount and (3) a
transition in the abundance ratios relative to the Iron is present between
redshifts ~0.5 and 1.4, with core-collapse SN products becoming dominant at
higher redshifts.
