How do galaxies build up their spin in the cosmic web?
  Using the Horizon-AGN simulation we find a mass dependent spin orientation
trend 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 tend
to possess a spin perpendicular to these filaments. We explore the physical
mechanisms driving galactic spin swings and quantify how much mergers and
smooth accretion re-orient them relative to their host filaments and impact
their shape. In particular, we analyze the effect of dispersion and morphology
of galaxies and discuss potential tracers for prospective surveys.
