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Although extensively investigated, the role of the environment in galaxyformation is still not well understood. In this context, the Galaxy StellarMass Function (GSMF) is a powerful tool to understand how environment relatesto galaxy mass assembly and the quenching of star-formation. In this work, wemake use of the high-precision photometric redshifts of the UltraVISTA Surveyto study the GSMF in different environments up to $z \sim 3$, on physicalscales from 0.3 to 2 Mpc, down to masses of $M \sim 10^{10} M_{\odot}$. Wewitness the appearance of environmental signatures for both quiescent andstar-forming galaxies. We find that the shape of the GSMF of quiescent galaxiesis different in high- and low-density environments up to $z \sim 2$ with thehigh-mass end ($M \gtrsim 10^{11} M_{\odot}$) being enhanced in high-densityenvironments. On the contrary, for star-forming galaxies a difference betweenthe GSMF in high- and low density environments is present for masses $M\lesssim 10^{11} M_{\odot}$. Star-forming galaxies in this mass range appear tobe more frequent in low-density environments up to $z < 1.5$. Differences inthe shape of the GSMF are not visible anymore at $z > 2$. Our results, in termsof general trends in the shape of the GSMF, are in agreement with a scenario inwhich galaxies are quenched when they enter hot gas-dominated massive haloeswhich are preferentially in high-density environments.

Reconstructing the galaxy density field with photometric redshifts: II. Environment-dependent galaxy evolution since $z \simeq 3$