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The growth-rate and the internal dynamics of galaxy-sized dark-matter haloesdepend on their location within the cosmic web. Haloes that sit at the nodesgrow in mass till the present time and are dominated by radial orbits.Conversely, haloes embedded in prominent filaments do not change much in sizeand are dominated by tangential orbits. Using zoom hydrodynamical simulationsincluding star formation and feedback, we study how gas accretes onto thesedifferent classes of objects that, for simplicity, we dub 'accreting' and'stalled' haloes. We find that all haloes get a fresh supply of newly accretedgas in their inner regions, although this slowly decreases with time, inparticular for the stalled haloes. The inflow of new gas is always higher than(but comparable with) that of recycled material. Overall, the cold-gas fractionincreases (decreases) with time for the accreting (stalled) haloes. In allcases, a stellar disc and a bulge form at the centre of the simulated haloes.The total stellar mass is in excellent agreement with expectations based on theabundance-matching technique. Many properties of the central galaxies do notseem to correlate with the large-scale environment in which the haloes reside.However, there are two notable exceptions that characterise stalled haloes withrespect to their accreting counterparts: i) the galaxy disc contains much olderstellar populations; ii) its vertical scale-height is larger by a factor of twoor more. This thickening is likely due to the heating of the long-lived discsby mergers and close flybys.

ZOMG II: Does the halo assembly history influence central galaxies and gas accretion?