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The role of the cosmic web in shaping galaxy properties is investigated inthe GAMA spectroscopic survey in the redshift range $0.03 \leq z \leq 0.25$.The stellar mass, $u - r$ dust corrected colour and specific star formationrate (sSFR) of galaxies are analysed as a function of their distances to the 3Dcosmic web features, such as nodes, filaments and walls, as reconstructed byDisPerSE. Significant mass and type/colour gradients are found for the wholepopulation, with more massive and/or passive galaxies being located closer tothe filament and wall than their less massive and/or star-forming counterparts.Mass segregation persists among the star-forming population alone. The redfraction of galaxies increases when closing in on nodes, and on filamentsregardless of the distance to nodes. Similarly, the star-forming populationreddens (or lowers its sSFR) at fixed mass when closing in on filament,implying that some quenching takes place. Comparable trends are also found inthe state-of-the-art hydrodynamical simulation Horizon-AGN. These resultssuggest that on top of stellar mass and large-scale density, the tracelesscomponent of the tides from the anisotropic large-scale environment also shapesgalactic properties. An extension of excursion theory accounting forfilamentary tides provides a qualitative explanation in terms of anisotropicassembly bias: at a given mass, the accretion rate varies with the orientationand distance to filaments. It also explains the absence of type/colourgradients in the data on smaller, non-linear scales.

Galaxy evolution in the metric of the Cosmic Web