Galaxy properties, such as stellar mass and star formation rate, correlate with their position within the cosmic web. Although galaxy properties can be correlated with a specific environment at a certain cosmic epoch, they may have experienced different environments at previous times. This `environmental history', which is closely linked to pre-processing, is bound to leave an imprint on the observable and physical properties of galaxies. In this work, we use the Galaxy Evolution and Assembly (GAEA) semi-analytic model and the magneto-hydrodynamic IllustrisTNG simulation to reconstruct the environmental histories of galaxies that today reside in filaments between z=0 and z=4. Our goal is to understand how galaxy properties are related to their past environments and to uncover the role of the cosmic web in shaping their present-day properties. This approach enables us to determine whether and when filamentary structures influence galaxy evolution. We find that filament galaxies at z=0 are a heterogeneous mix of populations with distinct environmental histories, and a clear dependency on the infall times into filaments. The vast majority of filament galaxies at z=0 have experienced group processing at some stage of their evolution, with only ∼20% of galaxies remaining centrals throughout their life. For low-mass filament galaxies (̊m 9 10) are affected by the filament environment, regardless of being centrals or satellites. Massive galaxies that have never been satellites and that entered filaments more than 9 Gyr ago show accelerated stellar mass assembly and higher quenched fractions relative to the field, due to a higher frequency of merger events inside filaments. Moreover, the most massive ̊m łog ( (M_ star / M_ sun) > 11) galaxies typically accreted onto filaments over 9 Gyr ago and have never become satellites within a larger halo, highlighting the role of filaments in building up the high-mass end of the galaxy population.
Zakharova et al. (Tue,) studied this question.