  The expected metal enrichment of the intra-cluster medium (ICM) and the
partition of metals between cluster galaxies and the hot ICM depends on the
stellar Initial Mass Function (IMF). The choice of the IMF in simulations of
clusters has also important consequences on the "cold fraction", which is a
fundamental constraint on cluster physics.
  We discuss the chemical enrichment and the cold fraction in clusters as
predicted with different IMFs, by means of a straightforward approach that is
largely independent of the details of chemical evolution models or simulations.
We suggest this simple approach as a guideline to select the input parameters
and interpret the results of more complex models and hydrodynamical
simulations.
