The Relative Supernovae Contribution to the Chemical Enrichment History of Abell 1837

TL;DR

This study investigates the relative contributions of different supernova types to the metal enrichment of the galaxy cluster Abell 1837 using X-ray data and a new modeling code, revealing a consistent early enrichment pattern.

Contribution

It introduces the SNeRatio code utilizing recent nucleosynthesis models to determine supernova contributions to cluster metal enrichment.

Findings

SNIa contribution is approximately 39% across the cluster.

Metal enrichment likely occurred early in the cluster formation.

The enrichment pattern supports an early, uniform supernova contribution scenario.

Abstract

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.