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Observational and theoretical arguments increasingly suggest that the initialmass function (IMF) of stars may depend systematically on environment, yet mostgalaxy formation models to date assume a universal IMF. Here we investigatesimulations of the formation of Milky Way analogues run with an empiricallyderived metallicity-dependent IMF and the moving-mesh code AREPO in order tocharacterize the associated uncertainties. In particular, we compare a constantChabrier and a varying metallicity-dependent IMF in cosmological,magneto-hydrodynamical zoom-in simulations of Milky Way-sized halos. We findthat the non-linear effects due to IMF variations typically have a limitedimpact on the morphology and the star formation histories of the formedgalaxies. Our results support the view that constraints on stellar-to-halo massratios, feedback strength, metallicity evolution and metallicity distributionsare in part degenerate with the effects of a non-universal,metallicity-dependent IMF. Interestingly, the empirical relation we use betweenmetallicity and the high mass slope of the IMF does not aid in the quenchingprocess. It actually produces up to a factor of 2-3 more stellar mass iffeedback is kept constant. Additionally, the enrichment history and the z = 0metallicity distribution are significantly affected. In particular, the alphaenhancement pattern shows a steeper dependence on iron abundance in themetallicity-dependent model, in better agreement with observationalconstraints.

Simulating a metallicity-dependent initial mass function: Consequences for feedback and chemical abundances