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Galaxy internal structure growth has long been accused of inhibiting starformation in disc galaxies. We investigate the potential physical connectionbetween the growth of dispersion-supported stellar structures (e.g. classicalbulges) and the position of galaxies on the star-forming main sequence at$z\sim0$. Combining the might of the SAMI and MaNGA galaxy surveys, we measurethe $\lambda_{Re}$ spin parameter for 3781 galaxies over $9.5 < \log M_{\star}[\rm{M}_{\odot}] < 12$. At all stellar masses, galaxies at the locus of themain sequence possess $\lambda_{Re}$ values indicative of intrinsicallyflattened discs. However, above $\log M_{\star}[\rm{M}_{\odot}]\sim10.5$ wherethe main sequence starts bending, we find tantalising evidence for an increasein the number of galaxies with dispersion-supported structures, perhapssuggesting a connection between bulges and the bending of the main sequence.Moving above the main sequence, we see no evidence of any change in the typicalspin parameter in galaxies once gravitationally-interacting systems areexcluded from the sample. Similarly, up to 1 dex below the main sequence,$\lambda_{Re}$ remains roughly constant and only at very high stellar masses($\log M_{\star}[\rm{M}_{\odot}]>11$), do we see a rapid decrease in$\lambda_{Re}$ once galaxies decline in star formation activity. If this trendis confirmed, it would be indicative of different quenching mechanisms actingon high- and low-mass galaxies. The results suggest that while a population ofgalaxies possessing some dispersion-supported structure is already present onthe star-forming main sequence, further growth would be required after thegalaxy has quenched to match the kinematic properties observed in passivegalaxies at $z\sim0$.

A SAMI and MaNGA view on the stellar kinematics of galaxies on the star-forming main sequence