  Many processes have been proposed to explain the quenching of star formation
in spiral galaxies and their transformation into S0s. These processes affect
the bulge and disc in different ways, and so by isolating the bulge and disc
spectra, we can look for these characteristic signatures. In this work, we used
BUDDI to cleanly extract the spectra of the bulges and discs of 78 S0 galaxies
in the MaNGA Survey. We compared the luminosity and mass weighted stellar
populations of the bulges and discs, finding that bulges are generally older
and more metal rich than their discs. When considering the mass and environment
of each galaxy, we found that the galaxy stellar mass plays a more significant
role on the formation of the bulges. Bulges in galaxies with masses
$\geq10^{10}M_\odot$ built up the majority of their mass rapidly early in their
lifetimes, while those in lower mass galaxies formed over more extended
timescales and more recently. No clear difference was found in the formation or
quenching processes of the discs as a function of galaxy environment. We
conclude that more massive S0 galaxies formed through an inside-out scenario,
where the bulge formed first and evolved passively while the disc underwent a
more extended period of star formation. In lower mass S0s, the bulges and discs
either formed together from the same material, or through an outside-in
scenario. Our results therefore imply multiple formation mechanisms for S0
galaxies, the pathway of which is chiefly determined by a galaxy's current
stellar mass.
