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Using the Horizon-AGN simulation we find a mass dependent spin orientationtrend for galaxies: the spin of low-mass, rotation-dominated, blue,star-forming galaxies are preferentially aligned with their closest filament,whereas high-mass, velocity dispersion- supported, red quiescent galaxies tendto possess a spin perpendicular to these filaments. We explore the physicalmechanisms driving galactic spin swings and quantify how much mergers andsmooth accretion re-orient them relative to their host filaments and impacttheir shape. In particular, we analyze the effect of dispersion and morphologyof galaxies and discuss potential tracers for prospective surveys.

How do galaxies build up their spin in the cosmic web?