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Recovering the origins of lenticular galaxies can shed light on theunderstanding of galaxy formation and evolution, since they present propertiesthat can be found in both elliptical and spiral galaxies. In this work we studythe kinematics of the globular cluster (GC) systems of three lenticulargalaxies 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 GCdata come from the Planetary Nebulae Spectrograph and the SLUGGS Surveys.Through photometric spheroid-disc decomposition and PNe kinematics we find theprobability for a given GC to belong to either the spheroid or the disc of itshost galaxy or be rejected from the model. We find that there is no correlationbetween the components that the GCs are likely to belong to and their colours.Particularly, for NGC 2768 we find that its red GCs display rotationpreferentially at inner radii (Re<1). In the case of the GC system of NGC 3115we find a group of GCs with similar kinematics that are not likely to belong toeither its spheroid nor disc. For NGC 7457 we find that 70% of its GCs arelikely to belong to the disc. Overall, our results suggest that these galaxiesassembled into S0s through different evolutionary paths. Mergers seem to havebeen very important for NGC 2768 and NGC 3115 while NGC 7457 is more likely tohave experienced secular evolution.

Chromodynamical Analysis of Lenticular Galaxies using Globular Clusters and Planetary Nebulae