  We investigate how a single generation galactic mass function (SGMF) depends
on the existence of variations in the initial stellar mass functions (IMF) of
stellar clusters. We show that cluster-to-cluster variations of the IMF lead to
a multicomponent SGMF where each component in a given mass range can be
described by a distinct power-law function. We also show that a dispersion of
$\approx 0.3$ M$_{\odot}$ in the characteristic mass of the IMF, as observed
for young Galactic clusters, leads to a low mass slope of the SGMF that matches
the observed Galactic stellar mass function even when the IMFs in the low mass
end of individual clusters are much steeper.
