In this talk, we would like to discuss how large-scale filaments affect the evolution of galaxies. By analyzing the HORIZON-AGN simulation data at a fixed redshift of z~2, we found that the dependency of galaxy properties on large-scale environment is mostly inherited from the (large-scale) environmental dependency of their host halo mass. When adopting a residual analysis that removes the host halo mass effect, we detected a direct and non-negligible influence of cosmic filaments. Proximity to filaments enhances the build-up of stellar mass. However, our multi-scale analysis also reveals that, at the edge of filaments, star formation is suppressed. We suggest that gas transfer from the outside to the inside of the haloes (where galaxies reside) becomes less efficient closer to filaments, due to high angular momentum supply at the vorticity-rich edge of filaments. To understand the underlying causality of such impacts of filaments on galaxy properties more directly, it is needed to track individual galaxies in time. Along that direction, we first tracked galaxy-hosting halos using a dark matter-only simulation. We examined the settling process of halos into the filament potential well in a phase space and their mass evolution along with it. Halos’ orbital trajectories and mass evolution are determined quite much by the initial condition of halos (i.e., initial position and formation time), which are also affected by the density of filaments. We found the mass segregation around filaments as with observations, which can be explained with massive halos being those that arrived filaments earlier.