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Using data from four deep fields (COSMOS, AEGIS, ECDFS, and CDFN), we studythe correlation between the position of galaxies in the star formation rate(SFR) versus stellar mass plane and local environment at $z<1.1$. To accuratelyestimate the galaxy SFR, we use the deepest available Spitzer/MIPS 24 andHerschel/PACS datasets. We distinguish group environments ($M_{halo}\sim$10$^{12.5-14.2}$$M_{\odot}$) based on the available deep X-raydata and lower halo mass environments based on the local galaxy density. Weconfirm that the Main Sequence (MS) of star forming galaxies is not a linearrelation and there is a flattening towards higher stellar masses ($M_*>10^{10.4-10.6}$ $M_{\odot}$), across all environments. At high redshift ($0.5<z<1.1$ ), the MS varies little with environment. At low redshift ($0.15<z<0.5$ ), group galaxies tend to deviate from the mean MS towards theregion of quiescence with respect to isolated galaxies and less-denseenvironments. We find that the flattening of the MS toward low SFR is due to anincreased fraction of bulge dominated galaxies at high masses. Instead, thedeviation of group galaxies from the MS at low redshift is caused by a largefraction of red disk dominated galaxies which are not present in the lowerdensity environments. Our results suggest that above a mass threshold ($\sim10^{10.4}-10^{10.6}$$M_{\odot}$ ) stellar mass, morphology and environmentact together in driving the evolution of the SF activity towards lower level.The presence of a dominating bulge and the associated quenching processes arealready in place beyond $z\sim$1. The environmental effects appear, instead, atlower redshifts and have a long time-scale.

Non-linearity and environmental dependence of the star forming galaxies Main Sequence