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The integrated galactic initial mass function (IGIMF) is computed from thecombination of the stellar initial mass function (IMF) and the embedded clustermass function, described by a power law with index beta. The result of thecombination is a time-varying IMF which depends on the star formation rate. Weapplied the IGIMF formalism to a chemical evolution model for the solarneighbourhood and compared the results obtained by assuming three possiblevalues for beta with the ones obtained by means of a standard, well-tested,constant IMF. In general, a lower absolute value of beta implies a flatterIGIMF, hence a larger number of massive stars, higher Type Ia and II supernovarates, higher mass ejection rates and higher [alpha/Fe] values at a givenmetallicity. Our suggested fiducial value for beta is 2, since with this valuewe can account for most of the local observables. We discuss our results in abroader perspective, with some implications regarding the possible universalityof the IMF and the importance of the star formation threshold.

The Role of the IGIMF in the chemical evolution of the solar neighbourhood