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We use comparisons between the SAMI Galaxy Survey and equilibrium galaxymodels to infer the importance of disc fading in the transition of spirals intolenticular (S0) galaxies. The local S0 population has both higher photometricconcentration and lower stellar spin than spiral galaxies of comparable massand we test whether this separation can be accounted for by passive agingalone. We construct a suite of dynamically self--consistent galaxy models, witha bulge, disc and halo using the GalactICS code. The dispersion-dominated bulgeis given a uniformly old stellar population, while the disc is given a currentstar formation rate putting it on the main sequence, followed by suddeninstantaneous quenching. We then generate mock observables (r-band images,stellar velocity and dispersion maps) as a function of time since quenching fora range of bulge/total (B/T) mass ratios. The disc fading leads to a decline inmeasured spin as the bulge contribution becomes more dominant, and also leadsto increased concentration. However, the quantitative changes observed after 5Gyr of disc fading cannot account for all of the observed difference. We seesimilar results if we instead subdivide our SAMI Galaxy Survey sample by starformation (relative to the main sequence). We use EAGLE simulations to alsotake into account progenitor bias, using size evolution to infer quenchingtime. The EAGLE simulations suggest that the progenitors of current passivegalaxies typically have slightly higher spin than present day star-forming discgalaxies of the same mass. As a result, progenitor bias moves the data furtherfrom the disc fading model scenario, implying that intrinsic dynamicalevolution must be important in the transition from star-forming discs topassive discs.

The SAMI Galaxy Survey: The role of disc fading and progenitor bias in kinematic transitions