Galaxy evolution in the metric of the Cosmic Web
  The role of the cosmic web in shaping galaxy properties is investigated in
the 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 formation
rate (sSFR) of galaxies are analysed as a function of their distances to the 3D
cosmic web features, such as nodes, filaments and walls, as reconstructed by
DisPerSE. Significant mass and type/colour gradients are found for the whole
population, with more massive and/or passive galaxies being located closer to
the filament and wall than their less massive and/or star-forming counterparts.
Mass segregation persists among the star-forming population alone. The red
fraction of galaxies increases when closing in on nodes, and on filaments
regardless of the distance to nodes. Similarly, the star-forming population
reddens (or lowers its sSFR) at fixed mass when closing in on filament,
implying that some quenching takes place. Comparable trends are also found in
the state-of-the-art hydrodynamical simulation Horizon-AGN. These results
suggest that on top of stellar mass and large-scale density, the traceless
component of the tides from the anisotropic large-scale environment also shapes
galactic properties. An extension of excursion theory accounting for
filamentary tides provides a qualitative explanation in terms of anisotropic
assembly bias: at a given mass, the accretion rate varies with the orientation
and distance to filaments. It also explains the absence of type/colour
gradients in the data on smaller, non-linear scales.
