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 .