  We present the first quantitative detection of large-scale filamentary
structure at $z \simeq 0.7$ in the large cosmological volume probed by the
VIMOS Public Extragalactic Redshift Survey (VIPERS). We use simulations to show
the capability of VIPERS to recover robust topological features in the galaxy
distribution, in particular the filamentary network. We then investigate how
galaxies with different stellar masses and stellar activities are distributed
around the filaments and find a significant segregation, with the most massive
or quiescent galaxies being closer to the filament axis than less massive or
active galaxies. The signal persists even after down-weighting the contribution
of peak regions. Our results suggest that massive and quiescent galaxies
assemble their stellar mass through successive mergers during their migration
along filaments towards the nodes of the cosmic web. On the other hand,
low-mass star-forming galaxies prefer the outer edge of filaments, a vorticity
rich region dominated by smooth accretion, as predicted by the recent spin
alignment theory. This emphasizes the role of large scale cosmic flows in
shaping galaxy properties.
