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The strikingly anisotropic large-scale distribution of matter made of anextended network of voids delimited by sheets, themselves segmented byfilaments, within which matter flows towards compact nodes where theyintersect, imprints its geometry on the dynamics of cosmic flows, ultimatelyshaping the distribution of galaxies and the redshift evolution of theirproperties. The (filament-type) saddle points of this cosmic web provide alocal frame in which to quantify the induced physical and morphologicalevolution of galaxies on large scales. The properties of virtual galaxieswithin the Horizon-AGN simulation are stacked in such a frame. The iso-contoursof the galactic number density, mass, specific star formation rate (sSFR),kinematics and age are clearly aligned with the filament axis with steepgradients perpendicular to the filaments. A comparison to a simulation withoutfeedback from active galactic nuclei (AGN) illustrates its impact on quenchingstar formation of centrals away from the saddles. The redshift evolution of theproperties of galaxies and their age distribution are consistent with thegeometry of the bulk flow within that frame. They compare well withexpectations from constrained Gaussian random fields and the scaling with themass of non-linearity, modulo the redshift dependent impact of feedbackprocesses. Physical properties such as sSFR and kinematics seem not to dependonly on mean halo mass and density: the residuals trace the geometry of thesaddle, which could point to other environment-sensitive physical processes,such as spin advection, and AGN feedback at high mass.

Galaxies flowing in the oriented saddle frame of the cosmic web