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

Abstract

Galaxy internal structure growth has long been accused of inhibiting star formation in disc galaxies. We investigate the potential physical connection between the growth of dispersion-supported stellar structures (e.g. classical bulges) and the position of galaxies on the star-forming main sequence at z similar to 0. Combining the might of the SAMI and MaNGA galaxy surveys, we measure the lambda(Re) spin parameter for 3289 galaxies over 9.5 < log M-star[M-circle dot] < 12. At all stellar masses, galaxies at the locus of the main sequence possess lambda(Re)values indicative of intrinsically flattened discs. However, above log M-star[M-circle dot] similar to 10.5 where the main sequence starts bending, we find tantalizing evidence for an increase in the number of galaxies with dispersion-supported structures, perhaps suggesting 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 typical spin parameter in galaxies once gravitationally interacting systems are excluded 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[M-circle dot] > 11), do we see a rapid decrease in lambda(Re) once galaxies decline in star formation activity. If this trend is confirmed, it would be indicative of different quenching mechanisms acting on high- and low-mass galaxies. The results suggest that whilst a population of galaxies possessing some dispersion-supported structure is already present on the star-forming main sequence, further growth would be required after the galaxy has quenched to match the kinematic properties observed in passive galaxies at z similar to 0.