The ICM and the IGM show metal lines in the X-ray spectra. These
metals cannot have been produced in the gas, but they must have
been produced in the galaxies and subsequently transported from
the galaxies into the ICM/IGM by certain processes like e.g.
ram-pressure stripping, galactic winds, galaxy-galaxy
interaction or jets from active galaxies. The metallicity is the
best indicator for finding out which of these processes are most
important. Of special interest is the distribution of metals. So
far there are only few examples of measured metallicity
variations in real 2D maps and not only profiles. In CL0939+4713
we find different metallicity in the different subclusters (De
Filippis et al. 2002). In the Perseus cluster also clear
metallicity variations were found (Schmidt et al. 2002). 1D
profiles are not very useful in this context because photons
from regions in the cluster which are very far apart are
accumulated in the same spectrum. Apart from the metallicity
distribution also the evolution of the me