Galaxy properties in the cosmic web of EAGLE simulation

2020/08/19 by Wenxiao Xu, Qi Guo, Haonan Zheng +9 · 21 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #COSMIC cancer database #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Halo #Luminosity #Physics #Redshift #Star formation #Stellar mass #astro-ph.GA

paper · pdf · doi:10.1093/mnras/staa2497

published in Monthly Notices of the Royal Astronomical Society 498(2), 1839-1851 (Oxford University Press) · 14 pages, 14 figures, 1 table. Accepted for publication in MNRAS

openalex publication_date 2020/08/19 · arxiv created 2020/09/16 · arxiv updated 2020/09/25 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

ABSTRACT We investigate the dependence of the galaxy properties on cosmic web environments using the most up-to-date hydrodynamic simulation: Evolution and Assembly of Galaxies and their Environments (EAGLE). The baryon fractions in haloes and the amplitudes of the galaxy luminosity function decrease going from knots to filaments to sheets to voids. Interestingly, the value of L* varies dramatically in different cosmic web environments. At z = 0, we find a characteristic halo mass of 10¹² \rm h^-1\rm M_\odot , below which the stellar-to-halo mass ratio is higher in knots, while above which it reverses. This particular halo mass corresponds to a characteristic stellar mass of 1.8× 10¹⁰ \rm h^-1\rm M_\odot . Below the characteristic stellar mass, central galaxies have redder colours, lower sSFRs, and higher metallicities in knots than those in filaments, sheets and voids, while above this characteristic stellar mass, the cosmic web environmental dependences either reverse or vanish. Such dependences can be attributed to the fact that the active galaxy fraction decreases along voids, sheets, filaments, and knots. The cosmic web dependences get weaker towards higher redshifts for most of the explored galaxy properties and scaling relations, except for the gas metallicity versus stellar mass relation.

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