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The origin of the quenching in galaxies is still highly debated. Differentscenarios and processes are proposed. We use multi-band (400-1600 nm)bulge-disc decompositions of massive galaxies in the redshift range 0<z<2 toexplore the distribution and the evolution of galaxies in the log SFR-logM*plane as a function of the stellar mass-weighted bulge-to-total ratio (BTM) andalso for internal galaxy components (bulge/disc) separately. We find evidenceof a clear link between the presence of a bulge and the flattening of the MainSequence in the high-mass end. All bulgeless galaxies (BTM<0.2) lie on themain-sequence, and there is little evidence of a quenching channel withoutbulge growth. Galaxies with a significant bulge component (BTM>0.2) are equallydistributed in number between star forming and passive regions. The vastmajority of bulges in the Main Sequence galaxies are quiescent, while starformation is localized in the disc component. Our current findings underline astrong correlation between the presence of the bulge and the star formationstate of the galaxy. A bulge, if present, is often quiescent, independently ofthe morphology or the star formation activity of the host galaxy. Additionally,if a galaxy is quiescent, with a large probability, is hosting a bulge.Conversely, if the galaxy has a disky shape is highly probable to be starforming.

Coincidence between morphology and star-formation activity through cosmic time: the impact of the bulge growth