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We test whether the universal initial mass function (UIMF) or the integratedgalaxial IMF (IGIMF) can be employed to explain the metallicity distribution(MD) of giants in the Galactic bulge. We make use of a single-zone chemicalevolution model developed for the Milky Way bulge in the context of aninside-out model for the formation of the Galaxy. We checked whether it ispossible to constrain the yields above $80 M_{\sun}$ by forcing the UIMF andrequired that the resulting MD matches the observed ones. We also extended theanalysis to the bulge of M31 to investigate a possible variation of the IMFamong galactic bulges. Several parameters that have an impact on stellarevolution (star-formation efficiency, gas infall timescale) are varied. We showthat it is not possible to satisfactorily reproduce the observed metallicitydistribution in the two galactic bulges unless assuming a flatter IMF ($x \leq1.1$) than the universal one. We conlude that it is necessary to assume avariation in the IMF among the various environments.

Testing the universal stellar IMF on the metallicity distribution in the bulges of the Milky Way and M 31