  It is frequently debated in literature whether a "standard" Initial Mass
Function (IMF) - meaning an IMF of the kind usually adopted to explain the
chemical evolution in the local Solar Neighbourhood - can account for the
observed metal enrichment and Iron Mass-to-Light Ratio in clusters of galaxies.
We address this problem by means of straightforward estimates that should hold
independently of the details of chemical evolution models.
  It is crucial to compute self-consistently the amount of mass and metals
locked-up in stars, by accounting for the stellar mass-to-light ratio predicted
by a given IMF. It becomes then clear that a "standard" Solar Neighbourhood IMF
cannot provide enough metals to account for the observed chemical properties in
clusters: clusters of galaxies and the local environment must be characterized
by different IMFs.
  Alternatively, if we require the IMF to be universal, in order to explain
clusters such an IMF must be much more efficient in metal production than
usually estimated for the Solar Vicinity. In this case, substantial loss of
metals is required from the Solar Neighbourhood and from disc galaxies in
general. This "non-standard" scenario for the local chemical evolution would
challenge our present understanding of the Milky Way and of disc galaxy
formation.
