Chromodynamical Analysis of Lenticular Galaxies using Globular Clusters
  and Planetary Nebulae
  Recovering the origins of lenticular galaxies can shed light on the
understanding of galaxy formation and evolution, since they present properties
that can be found in both elliptical and spiral galaxies. In this work we study
the kinematics of the globular cluster (GC) systems of three lenticular
galaxies located in low density environments (NGC 2768, NGC 3115 and NGC 7457),
and compare them with the kinematics of planetary nebulae (PNe). The PNe and GC
data come from the Planetary Nebulae Spectrograph and the SLUGGS Surveys.
Through photometric spheroid-disc decomposition and PNe kinematics we find the
probability for a given GC to belong to either the spheroid or the disc of its
host galaxy or be rejected from the model. We find that there is no correlation
between the components that the GCs are likely to belong to and their colours.
Particularly, for NGC 2768 we find that its red GCs display rotation
preferentially at inner radii (Re<1). In the case of the GC system of NGC 3115
we find a group of GCs with similar kinematics that are not likely to belong to
either its spheroid nor disc. For NGC 7457 we find that 70% of its GCs are
likely to belong to the disc. Overall, our results suggest that these galaxies
assembled into S0s through different evolutionary paths. Mergers seem to have
been very important for NGC 2768 and NGC 3115 while NGC 7457 is more likely to
have experienced secular evolution.
