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ABSTRACT We study the link between the kinematic-morphology of galaxies, as inferred from integral-field stellar kinematics, and their relation between mass and star formation rate. Our sample consists of ∼3200 galaxies with integral-field spectroscopic data from the MaNGA survey (Mapping Nearby Galaxies at Apache Point Observatory) with available determinations of their effective stellar angular momentum within the half-light radius ₑ䂰. We find that for star-forming galaxies, namely along the star formation main sequence (SFMS), the ₑ䂰 values remain large and almost unchanged over about two orders of magnitude in stellar mass, with the exception of the lowest masses M 2 10^9 \, M, where ₑ䂰 slightly decreases. The SFMS is dominated by spiral galaxies with small bulges. Below the SFMS, but above the characteristic stellar mass M ₂ₑ₈ₓ 2 10^11 \, M, there is a sharp decrease in ₑ䂰 with decreasing star formation rate (SFR): massive galaxies well below the SFMS are mainly slow-rotator early-type galaxies, namely genuinely spheroidal galaxies without discs. Below the SFMS and below M ₂ₑ₈ₓ the decrease of ₑ䂰 with decreasing SFR becomes modest or nearly absent: low-mass galaxies well below the SFMS, are fast-rotator early-type galaxies, and contain fast-rotating stellar discs like their star-forming counterparts. We also find a small but clear environmental dependence for the massive galaxies: in the mass range 10^10. 9\!-\!10^11. 5 \, M, galaxies in rich groups or denser regions or classified as central galaxies have lower values of ₑ䂰. While no environmental dependence is found for galaxies of lower mass. We discuss how the above results can be understood as due to the different star formation and mass assembly histories of galaxies with varying mass.
Wang et al. (Wed,) studied this question.
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