Galaxies in the Universe are not distributed uniformly, but rather in a web-like structure char- acterised by dense clusters, elongated filaments, sheetlike walls, and under-dense regions in between, called voids. Galaxies in voids are on average bluer, less massive, have later morphological types, and have higher star formation rates than galaxies in denser environments. Simulations show that different gas accretion modes dominate in each environment and the halo-to-stellar mass ratio is higher in void galaxies compared to galaxies in denser environments. This suggests that galaxies in voids evolve slower. Here I present results related to the molecular gas mass and star formation histories of galaxies in the voids, filaments, walls and clusters, trying to unveil the effect of the large-scale environment on galaxy evolution.