Variations of the Initial Mass Function in Semi-Analytical models
  Deviations from a universal, MW-like, Stellar Initial Mass Function (IMF)
have been reported for distant galaxies, although the physical reason behind
the observed variations is still matter of ongoing debate. In this paper, we
present an exploratory study to assess the impact of the proposed IMF evolution
on the statistical galaxy properties, as predicted by the Semi-Analytical model
of galaxy formation and evolution MORGANA. In particular, we test different
dependencies for the IMF shape, as a function of both model galaxy properties
(such as star formation rate, velocity dispersion or stellar mass) and
environment, and compare the predicted stellar mass functions and star
formation rate functions with reference runs at fixed IMF. In most cases,
MORGANA predictions show deviations of the order of a few tenths of dex with
respect to a run assuming an Universal Kroupa IMF. Among the proposed IMF
variations, an increasing Top-Heavy IMF at increasing star formation rates has
the largest impact on predicted galaxy properties, while most of the models
assuming an increasing Bottom-Heavy IMF at higher masses/velocity dispersion
lead to variations in galaxy properties that are of the same order as the
uncertainty on the mass and star formation rate determination. By comparing the
predicted galaxy stellar mass functions, we conclude that the study of the
high-mass end can provide useful constraints to disentangle models assuming an
increasing Top-Heavy IMF in high star forming or Bottom-Heavy IMF in massive
systems.
