SDSS-IV MaNGA: The kinematic-morphology of galaxies on the mass versus star-formation relation in different environments

We study the link between the kinematic-morphology of galaxies, as inferred from integralfield stellar kinematics, and their relation between mass and star formation rate. Our sample consists of similar to 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 lambda R-e. We find that for star-forming galaxies, namely along the star formation main sequence (SFMS), the.Re values remain large and almost unchanged over about two orders of magnitude in stellar mass, with the exception of the lowest masses M-* less than or similar to 2 x 10(9) M-circle dot, where lambda R-e slightly decreases. The SFMS is dominated by spiral galaxies with small bulges. Below the SFMS, but above the characteristic stellar mass M-crit approximate to 2 x 10(11) M-circle dot, there is a sharp decrease in lambda R-e with decreasing star formation rate (SFR): massive galaxies well below the SFMS are mainly slowrotator early-type galaxies, namely genuinely spheroidal galaxies without discs. Below the SFMS and below M-crit the decrease of lambda R-e 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-circle dot, galaxies in rich groups or denser regions or classified as central galaxies have lower values of lambda R-e. 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.