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We examine how the mass assembly of central galaxies depends on theirlocation in the cosmic web. The HORIZON-AGN simulation is analysed at z~2 usingthe DISPERSE code to extract multi-scale cosmic filaments. We find that thedependency of galaxy properties on large-scale environment is mostly inheritedfrom the (large-scale) environmental dependency of their host halo mass. Whenadopting a residual analysis that removes the host halo mass effect, we detecta direct and non-negligible influence of cosmic filaments. Proximity tofilaments enhances the build-up of stellar mass, a result in agreement withprevious studies. However, our multi-scale analysis also reveals that, at theedge of filaments, star formation is suppressed. In addition, we find clues forcompaction of the stellar distribution at close proximity to filaments. Wesuggest that gas transfer from the outside to the inside of the haloes (wheregalaxies reside) becomes less efficient closer to filaments, due to highangular momentum supply at the vorticity-rich edge of filaments. This quenchingmechanism may partly explain the larger fraction of passive galaxies infilaments, as inferred from observations at lower redshifts.

Beyond halo mass: quenching galaxy mass assembly at the edge of filaments