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It has been proposed that S0 galaxies are either fading spirals or the resultof galaxy mergers. The relative contribution of each pathway, and theenvironments in which they occur remains unknown. Here we investigate stellarand gas kinematics of 219 S0s in the SAMI Survey to look for signs of multipleformation pathways occurring across the full range of environments. We identifya large range of rotational support in their stellar kinematics, whichcorrespond to ranges in their physical structure. We find thatpressure-supported S0s with $v/{\sigma}$ below 0.5 tend to be more compact andfeature misaligned stellar and gas components, suggesting an external originfor their gas. We postulate that these S0s are consistent with being formedthrough a merger process. Meanwhile, comparisons of ellipticity, stellar massand S\'ersic index distributions with spiral galaxies shows that therotationally supported S0s with $v/{\sigma}$ above 0.5 are more consistent witha faded spiral origin. In addition, a simulated merger pathway involving acompact elliptical and gas-rich satellite results in an S0 that lies within thepressure-supported group. We conclude that two S0 formation pathways areactive, with mergers dominating in isolated galaxies and small groups, and thefaded spiral pathway being most prominent in large groups ($10^{13} < M_{halo}< 10^{14}$).

The SAMI Galaxy Survey: A Range in S0 Properties Indicating Multiple Formation Pathways