Environmental history of filament galaxies: stellar mass assembly and star-formation of filament galaxies

Abstract

Galaxy properties correlate with their position within the cosmic web. While galaxies are observed in an environment today, they may have experienced different environments in the past. The environmental history, linked to pre-processing, leaves an imprint on the properties of galaxies. We use the GAEA semi-analytic model and IllustrisTNG to reconstruct the environmental histories of galaxies between $z=0$ and $z=4$ that today reside in filaments. Our goal is to understand how galaxy properties are related to their past environments, and the role of the cosmic web in shaping their properties. We find that filament galaxies at $z=0$ are a heterogeneous mix of populations with distinct environmental histories. The vast majority of them have experienced group processing, with only $\sim$20\% remaining centrals throughout their life. For $9<{\log }_{10}({\mathrm{M}}_{\mathrm{star}}/{\mathrm{M}}_{\mathrm{sun}})<10$ galaxies, models confirm that the environmental effects are primarily driven by group processing: satellites stop growing stellar mass and exhibit elevated quenched fractions, whereas filament galaxies remain centrals have properties that are similar to field galaxies. Massive galaxies (${\log }_{10}({\mathrm{M}}_{\mathrm{star}}/{\mathrm{M}}_{\mathrm{sun}})>10$) that have never been satellites and 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, even at fixed mass. The most massive $\log (({\mathrm{M}}_{\mathrm{star}}/{\mathrm{M}}_{\mathrm{sun}})>11$) galaxies accreted onto filaments over 9 Gyr ago, highlighting the role of filaments in building up the high-mass end of the galaxy population. Filaments regulate galaxy evolution in a mass-dependent way: group environments regulate low-mass galaxies, while filaments favour the growth of massive galaxies.

arXiv commentSubmitted to A&A, comments welcome

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Cited by in corpus (1)

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