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

Abstract

We investigate the impact of cosmic filaments on the gas accretion rate, ${\dot{M}}_{\mathrm{gas}}$, of dark matter halos in filaments, based on cosmological hydrodynamic simulation. We find that for halos less massive than $10^{12.0}{\mathrm{M}}_{\odot }$, ${\dot{M}}_{\mathrm{gas}}$ of halos residing in prominent filaments (with width $D_{\mathrm{fil}}>3\mathrm{Mpc}/h$) is lower than halos residing in tenuous filaments ($D_{\mathrm{fil}}<3\mathrm{Mpc}/h$) by $20-30\%$ at $z=0.5$, and by a factor of 2-3 at $z=0$. However, ${\dot{M}}_{\mathrm{gas}}$ 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 $10^6$ 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 $z\lesssim 0.5$ 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 $z<1$.

16 pages, 12 figures. published version in The Astrophysical Journal

References in corpus (30)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe
• Mass and environment as drivers of galaxy evolution in SDSS and zCOSMOS and the origin of the Schechter function
• Cold streams in early massive hot haloes as the main mode of galaxy formation
• Strangulation as the primary mechanism for shutting down star formation in galaxies
• Properties of Dark Matter Haloes in Clusters, Filaments, Sheets and Voids
• Moving mesh cosmology: tracing cosmological gas accretion
• Bimodal gas accretion in the Horizon-MareNostrum galaxy formation simulation
• The DEEP2 Galaxy Redshift Survey: The Role of Galaxy Environment in the Cosmic Star-Formation History
• Effect of local environment and stellar mass on galaxy quenching and morphology at $0.5<z<2.0$
• The relation between star formation, morphology and local density in high redshift clusters and groups
• The effects of environment on morphological evolution between 0<z<1.2 in the COSMOS Survey
• From voids to filaments: environmental transformations of galaxies in the SDSS
• Cosmic Web of Galaxies in the COSMOS Field: Public Catalog and Different Quenching for Centrals and Satellites
• The environmental dependence of gas accretion onto galaxies: quenching satellites through starvation
• Properties of gas phases around cosmic filaments at z=0 in the Illustris-TNG simulation
• The GOGREEN survey: The environmental dependence of the star-forming galaxy main sequence at $1.0<z<1.5$
• Large Scale Structures in the CANDELS Fields: The Role of the Environment in Star Formation Activity
• Evidence for HI replenishment in massive galaxies through gas accretion from the cosmic web
• The ThreeHundred: the structure and properties of cosmic filaments in the outskirts of galaxy clusters
• Caught in the cosmic web: Environmental effect on halo concentrations, shape, and spin
• The Effect of Ram-Pressure Stripping on Dwarf Galaxies
• Beyond halo mass: quenching galaxy mass assembly at the edge of filaments
• CANDELS Sheds Light on the Environmental Quenching of Low-mass Galaxies
• Study of galaxies on large-scale filaments in simulations
• The dispersion measure and scattering of FRBs: Contributions from the intergalactic medium, foreground halos, and hosts
• Properties of Galaxies in Cosmic Filaments around the Virgo Cluster
• The Accretion and Cooling of Preheated Gas in Dark Matter Halos
• Galaxy properties in the cosmic web of EAGLE simulation
• Evolution of galaxies in groups in the Coma Supercluster

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