Study of galaxies on large-scale filaments in simulations
  We use data from the Evolution and Assembly of GaLaxies in their Environment
(EAGLE) cosmological simulation to study properties of galaxies in the cosmic
web. Galaxies become more redder and form stars at a lower rate relative to
their counterparts further away from the cylindrical axis of the large-scale
filaments. These trends are particularly strong for galaxies with
$M_*/M_{\odot}\lesssim10^{10}$. We also find that at distances $<0.5$ Mpc from
the spine of the filaments, the median gas and stellar mass fraction in
filament galaxies rises sharply with decreasing distance from the spine of the
filament. These results, together with matching trends in the SFR/$M_*$ and the
$g-r$ colour of filament galaxies suggest that (i) the intrafilamentary gas
condenses into the filament galaxies thus fuelling star formation in them, and
(ii) increased number density of galaxies closer to the central axis of the
filament enhances the rate of gravitational interactions among filament
galaxies closer to the spine.
