Resumo:
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.
