X-ray observations of galaxy clusters have shown that the intracluster gas presents iron abundances of one third of about the solar value. These observations also show that part (if not all) of the intra-cluster gas metals were produced within the member galaxies. We observe the presence of $\alpha$-elements, which are produced in supernovae type IIand the iron group elements which are essentially produced in supernovae type Ia.The ratio between the $\alpha$ elements and the iron abundance can constraint the metal enrichment historyof the intracluster gas.Since the red population is dominant in galaxy clusters,it is natural to assume that it is the main responsible for the metal enrichment of the intracluster gas. However, the role of the different morphological galaxy types to the gas enrichment is not yet well understood.In this post-doc project we propose to investigate the gas enrichment process and the role of galaxies. To do so, we will select a sample of galaxies observed in conjunction with the XMM-Newton and the Sloan Digital Sky Survey (SDSS). The sensitivity of the XMM-Newton is absolutely necessary to the spectroscopical analysis of the gas. We will select at least 20 galaxy clusters within the redshift interval 0.1 < z < 0.3 and with X-ray exposure times grater than 10ks.From the spectroscopic analysis we will be able to determine the metallicity and the gas temperature distribution. From the optical analysis we will compute the contribution of the different morphological types to the total luminosity. Using a multi-wavelength study of clusters of galaxies we will investigate possible correlations between optical and X-ray properties and give new constraints to the history of intracluster gasenrichment.
News published in Agência FAPESP Newsletter about the scholarship: