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We study the impact of local density and stellar mass on the morphology of~500 quiescent (Q) and SFGs from the VIS3COS survey. We perform B/Ddecomposition of the SBPs and find ~41% of 10^10 Msun galaxies to be bestfitted with 2 components. We complement our analysis with non-parametricmeasurements and qualitative visual classifications. We find that galaxymorphology depends on stellar mass and environment for our sample as a whole.We only find an impact of the environment on galaxy sizes for galaxies moremassive than 10^11 Msun. We find higher n and B/T in high-density regions whencompared to low-density counterparts at similar stellar masses. We also findthat higher stellar mass galaxies have steeper light profiles compared to thelower ones. Using visual classifications, we find a morphology-density relationat z~0.84 for galaxies more massive than 10^10 Msun, with elliptical galaxiesbeing dominant at high-density regions and disks more common in low-densityregions. However, when splitting the sample into colour-colour selected SF andQ sub-populations, there are no statistically significant differences betweenlow- and high-density regions. We find that Q galaxies are smaller, have highern, and higher B/T when compared to SF counterparts. We confirm these trendswith non-parametric quantities, finding Q galaxies to be smoother and havingmost of their light over smaller areas than SFGs. Overall, we find that thedependence of morphology on stellar mass is stronger than with local densityand these relations are strongly correlated with the quenching fraction. Thechange in average morphology corresponds to a change in the relative fractionsof blue disk-like galaxies and red elliptical galaxies with stellar mass andenvironment. We hypothesize that the processes responsible for the quenching ofSF must also affect the galaxy morphology on similar timescales.

VIS3COS: II. Nature and nurture in galaxy structure and morphology