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Galaxy properties in the cosmic web of EAGLE simulation.

Xu, Wenxiao and Guo, Qi and Zheng, Haonan and Gao, Liang and Lacey, Cedric and Gu, Qing and Liao, Shihong and Shao, Shi and Mao, Tianxiang and Zhang, Tianchi and Chen, Xuelei (2020) 'Galaxy properties in the cosmic web of EAGLE simulation.', Monthly notices of the Royal Astronomical Society., 498 (2). pp. 1839-1851.


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 1012h−1M⊙⁠, 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 1.8×1010h−1M⊙⁠. Below the characteristic stellar mass central galaxies have redder colors, 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 vs. stellar mass relation.

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Publisher statement:This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. ©: 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:11 August 2020
Date deposited:18 September 2020
Date of first online publication:20 August 2020
Date first made open access:18 September 2020

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