Impact of cosmic filaments on the gas accretion rate of dark matter halos

Weishan Zhu; Fupeng Zhang; Long-Long Feng

doi:10.3847/1538-4357/ac37b9

paper

Impact of cosmic filaments on the gas accretion rate of dark matter halos

arXiv:2111.04400 · doi:10.3847/1538-4357/ac37b9

Abstract

We investigate the impact of cosmic filaments on the gas accretion rate, $M ˙_{gas}$ , of dark matter halos in filaments, based on cosmological hydrodynamic simulation. We find that for halos less massive than $1 0^{12.0} M_{⊙}$ , $M ˙_{gas}$ of halos residing in prominent filaments (with width $D_{fil} > 3 Mpc /h$ ) is lower than halos residing in tenuous filaments ( $D_{fil} < 3 Mpc /h$ ) by $20 - 30%$ at $z = 0.5$ , and by a factor of 2-3 at $z = 0$ . However, $M ˙_{gas}$ depends weakly on the physical distance between halo center and the spine of filaments from high redshift to $z = 0$ , only shows clear difference between the inner and outer regions in prominent filaments at $z = 0$ . We further probe the thermal properties of gas in prominent and tenuous filaments, which appear in relatively highly and intermediate overdense regions, respectively. The gas in prominent filaments is hotter. Around $26%$ , $38%$ and $45%$ of gases in prominent filaments are hotter than $1 0^{6}$ K at $z = 1.0, 0.5$ and $z = 0.0$ respectively. The corresponding fractions in tenuous filaments are merely $\sim 6%, 9%$ and $11%$ . The suppressed gas accretion rate for low-mass halos in prominent filaments at $z ≲ 0.5$ may result from the hotter ambient gas, which could provide a physical processing mechanism to cut down the supply of gas to halos before they enter clusters. This process meets partially the need of the preheating mechanism implemented in some semi-analytical models of galaxy formation, but works only for $\sim 20%$ of halos at $z < 1$ .

arXiv comment16 pages, 12 figures. published version in The Astrophysical Journal

Impact of cosmic filaments on the gas accretion rate of dark matter halos

Abstract

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