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Using multi-wavelength data, from UV-optical-near-mid IR, for $\sim$6000galaxies in the local Universe, we study the dependence of star formation onthe morphological T-types for massive galaxies ($\log M_*/M_\odot \geq 10$). Wefind that, early-type spirals (Sa-Sbc) and S0s predominate in the green valley,which is a transition zone between the star forming and quenched regions.Within the early-type spirals, as we move from Sa to Sbc spirals the fractionof green valley and quenched galaxies decreases, indicating the important roleof the bulge in the quenching of galaxies. The fraction of early-type spiralsdecreases as we enter the green valley from the blue cloud, which coincideswith the increase in the fraction of S0s. This points towards the morphologicaltransformation of early-type spiral galaxies into S0s which can happen due toenvironmental effects such as ram-pressure stripping, galaxy harassment, ortidal interactions. We also find a second population of S0s which are activelystar-forming and are present in all environments. Since morphological T-type,specific star formation rate (sSFR), and environmental density are allcorrelated with each other, we compute the partial correlation coefficient foreach pair of parameters while keeping the third parameter as a controlvariable. We find that morphology most strongly correlates with sSFR,independent of the environment, while the other two correlations(morphology-density and sSFR-environment) are weaker. Thus, we conclude that,for massive galaxies in the local Universe, the physical processes that shapetheir morphology are also the ones that determine their star-forming state.

On the interdependence of galaxy morphology, star formation, and environment in massive galaxies in the nearby Universe