The origin of the chemical elements in cluster cores
  Metals play a fundamental role in ICM cooling processes in cluster cores
through the emission of spectral lines. But when and how were these metals
formed and distributed through the ICM? The X-ray band has the unique property
of containing emission lines from all elements from carbon to zinc within the
0.1-10 keV band. Using XMM-Newton, the abundances of about 11 elements are
studied, which contain valuable information about their origin. Most elements
were formed in type Ia and core-collapse supernovae, which have very different
chemical yields. Massive stars and AGB stars also contribute by providing most
of the carbon and nitrogen in the ICM. Because feedback processes suppress star
formation in the cluster centre, the element abundances allow us to directly
probe the star formation history of the majority of stars that are thought to
have formed between z=2-3. The spatial distribution in the core and the
evolution with redshift also provide information about how these elements are
transported from the member galaxies to the ICM. I review the current progress
in chemical enrichment studies of the ICM and give an outlook to the future
opportunities provided by XMM-Newton's successors, like Astro-H.
