  We investigate the relationship between environment, morphology, and the star
formation rate -- stellar mass relation derived from a sample of star-forming
galaxies (commonly referred to as the `star formation main sequence') in the
COSMOS field from 0 < z < 3.5. We constructed and fit the FUV--FIR SEDs of our
stellar mass-selected sample of 111,537 galaxies with stellar and dust emission
models using the public packages MAGPHYS and SED3FIT. From the best fit
parameter estimates, we construct the star formation rate -- stellar mass
relation as a function of redshift, local environment, NUVrJ color diagnostics,
and morphology. We find that the shape of the main sequence derived from our
color-color and sSFR-selected star forming galaxy population, including the
turnover at high stellar mass, does not exhibit an environmental dependence at
any redshift from 0 < z < 3.5. We investigate the role of morphology in the
high mass end of the SFMS to determine whether bulge growth is driving the high
mass turnover. We find that star-forming galaxies experience this turnover
independent of bulge-to-total ratio, strengthening the case that the turnover
is due to the disk component's specific star formation rate evolving with
stellar mass rather than bulge growth.
