  In this paper, we report the relative SNe contributions on the metal budget
of the ICM of Abell 1837 galaxy cluster at redshift z $=$ 0.069. For this
purpose, we analysed the hot ICM of the cluster and obtained radial metal
distributions by using XMM-Newton archival data with total exposure $\sim$100
ks. These metal measurements consist of Mg, Si, S, Fe and Ni within 0.7
R$_{500}$ radius which is divided into three concentric annuli. In order to
explain the observed metal abundance pattern in terms of relative supernova
contributions, we used our newly developed code SNeRatio which utilizes
theoretical nucleosynthesis models. This study covers the most recent 3D SNIa
and SNcc yield tables. All combinations of these theoretical yields were fitted
with our measured abundance ratios and statistically acceptable ones were
selected. Each of these models were found to predict a uniform SNIa percentage
contribution to the total SNe from the cluster center to the outskirts and form
an SNIa ratio distribution with a mean 39 $\pm$ 14$\%$. This uniformity is
consistent with the early enrichment scenario which assumes that the metal
production processes begin in early phase of cluster formation, namely
proto-cluster phase at epoch z $\geq$ 2.
