ANÁLISE COMPARATIVA DE MODELOS DE EXPLOSÃO DE SUPERNOVAS ATRAVÉS DO GÁS INTRA-AGLOMERADO E SEU IMPACTO NOS MECANISMOS DE AQUECIMENTO CENTRAL DE GRUPOS FÓSSEIS DE GALÁXIAS

Abstract

This PhD thesis investigates the transport of metals from member galaxies of clusters and groups of galaxies to the intragroup/cluster medium and the efficiency of the mechanisms involved in the enrichment of metals in these mediums. The intracluster medium (ICM) is a reservoir of heavy elements synthesized by different types of supernovae (SNe) throughout cosmic history. Different enrichment mechanisms contribute a different relative metal production, predominantly caused by different SNe type dominance. However, to quantify such relative importance between these enrichment mechanisms it is necessary to adopt SN models, i.e., a core collapse supernova model (SNcc) and a type Ia supernova model (SNIa). Such a choice is crucial, since the SN models predict theoretical yields quite different from each other. To reduce this uncertainty, we implemented a probability density function analysis of metal abundance ratios and classified 7192 SNe explosion models from the literature that provide \textit{yields} comparing their performance with eight abundance ratios of observations Suzaku of 18 nearby galaxy systems (clusters and groups) ($z\leq0.0391$) to test their predictions. Among the best performing pairs of SN models, we selected the theoretical pair (SNIa+SNcc) with the most flexibility of combinations to determine the evolution of a special type of galaxy groups called Fossil Groups (FGs). For this, we determined elemental abundance ratios for different regions of 3 FGs at intermediate redshifts (z~0.1) with EPIC/XMM-Newton observations, which were later used to calculate the excess/deficit of the Fe mass fraction from type II supernova (SNII) in the central regions of these objects. In addition, we analyzed the fraction of intracluster light from RXJ1007+3800 and RXJ0856+0553 as an indicator of their dynamic state and age using Hubble, Gemini and XMM-Newton observations. Our results indicate that the hot cores of the RXJ1007+3800, RXJ1410+4145 and RXJ0856+0553 systems can be efficiently enriched and heated in this region by injection of energy by galactic superwinds energized by SNeII.