  [arXiv Abridged] In this work, we explore new spatially-resolved measurements
of the IMF for three edge-on lenticular galaxies in the Fornax cluster.
Specifically, we utilise existing orbit-based dynamical models, which
re-produce the measured stellar kinematics, in order to fit the new IMF maps
within this orbital framework. We then investigate correlations between
intrinsic orbital properties and the local IMF. We find that, within each
galaxy, the high-angular-momentum, disk-like stars exhibit an IMF which is rich
in dwarf stars. The centrally-concentrated pressure-supported orbits have IMF
which are similarly rich in dwarf stars. Conversely, orbits at large radius
which have intermediate angular momentum exhibit IMF which are markedly less
dwarf-rich relative to the other regions of the same galaxy. Assuming that the
stars which, in the present-day, reside on dynamically-hot orbits at large
radii are dominated by accreted populations, we can interpret these findings as
a correlation between the dwarf-richness of a population of stars, and the mass
of the host in which it formed. Specifically, deeper gravitational potentials
would produce more dwarf-rich populations, resulting in the relative deficiency
of dwarf stars which originated in the lower-mass accreted satellites.
Conversely, the central and high angular-momentum populations are likely
dominated by in-situ stars, which were formed in the more massive host itself.
There are also global differences between the three galaxies studied here, of
up to $\sim 0.3\ \mathrm{dex}$ in the IMF parameter $\xi$. We find no local
dynamical or chemical property which alone can fully account for the IMF
variations.
