SDSS-IV MaNGA: The kinematic-morphology of galaxies on the mass vs
  star-formation relation in different environments
  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 (SFR). Our sample consists of $\sim 3200$ galaxies with
integral-field spectroscopic data from the MaNGA survey 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 $\lambda_{R_e}$
values remain large and almost unchanged over about two orders of magnitude in
stellar mass, with the exception of the lowest masses
$\mathcal{M}_{\star}\lesssim2\times10^{9} \mathcal{M}_{\odot}$, 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
$\mathcal{M}_{\rm crit}\approx2\times10^{11} \mathcal{M}_{\odot}$, there is a
sharp decrease in $\lambda_{R_e}$ with decreasing star formation rate: massive
galaxies well below the SFMS are mainly slow-rotator early-type galaxies,
namely genuinely spheroidal galaxies without disks. Below the SFMS and below
$\mathcal{M}_{\rm crit}$ 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 disks like
their star-forming counterparts. We also find a small but clear environmental
dependence for the massive galaxies: in the mass range $10^{10.9}-10^{11.5}
\mathcal{M}_{\odot}$, 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
our results can be understood as due to the different star formation and mass
assembly histories of galaxies with varying mass.
