The large-scale environment from cosmological simulations I: The baryonic cosmic web

Abstract

Using a series of cosmological simulations that includes one dark-matter-only (DM-only) run, one gas cooling-star formation-supernovae feedback (CSF) run and one that additionally includes feedback from active galactic nuclei (AGNs), we classify the large-scale structures with both a velocity-shear-tensor code (Vweb) and a tidal-tensor code (Pweb). We find that the baryonic processes have almost no impact on large-scale structures -- at least not when classified using aforementioned techniques. More importantly, our results confirm that the gas component alone can be used to infer the filamentary structure of the Universe practically un-biased, which could be applied to cosmology constrains. In addition, the gas filaments are classified with its velocity (Vweb) and density (Pweb) fields, which can theoretically connect to the radio observations, such as HI surveys. This will help us to bias-freely link the radio observations with DM distributions at large scale.

13 pages, 8 figures, matched to the MNRAS accepted version (V2). Matched to the the version after the Erratum. No conclusion is changed (V3). Corrections for the references papers (V4)

References in corpus (16)

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Cited by in corpus (25)

• \textsc{The Three Hundred} project: The \textsc{Gizmo-Simba} run
• Properties of gas phases around cosmic filaments at z=0 in the Illustris-TNG simulation
• The Abell 3391/95 galaxy cluster system: A 15 Mpc intergalactic medium emission filament, a warm gas bridge, infalling matter clumps, and (re-) accelerated plasma discovered by combining SRG/eROSITA data with ASKAP/EMU and DECam data
• An EAGLE view of the missing baryons
• Mapping and characterisation of cosmic filaments in galaxy cluster outskirts: strategies and forecasts for observations from simulations
• An inventory of galaxies in cosmic filaments feeding galaxy clusters: galaxy groups, backsplash galaxies, and pristine galaxies
• The ThreeHundred: the structure and properties of cosmic filaments in the outskirts of galaxy clusters
• Relative distribution of dark matter, gas, and stars around cosmic filaments in the IllustrisTNG simulation
• Do model emission line galaxies live in filaments at z~1?
• The eROSITA view of the Abell 3391/95 field: a case study from the Magneticum cosmological simulation
• Simulating MOS science on the ELT: Ly$\alpha$ forest tomography
• The large-scale environment from cosmological simulations II: The redshift evolution and distributions of baryons
• Simultaneous Dependence of Matter Clustering on Scale and Environment
• A semi-analytical perspective on massive galaxies at $z\sim 0.55$
• Cosmic metal invaders: Intergalactic OVII as a tracer of the warm-hot intergalactic medium within cosmic filaments in the EAGLE simulation
• The Three Hundred project: Estimating the dependence of gas filaments on the mass of galaxy clusters
• How do baryonic effects on the cosmic matter distribution vary with scale and local density environment?
• A theoretical view of the T-web statistical description of the cosmic web
• Relation between the local width and linear halo mass density of cosmic filaments
• The Three Hundred: Gas Properties Outside of Galaxy Cluster with the WHIM Contribution and Detection
• Mock catalogues of emission line galaxies based on the local mass density in dark-matter only simulations
• A universal and physically motivated threshold for Hessian-based cosmic web identification: V-Web case
• Impact of the large-scale cosmic web on the X-ray emitting circumgalactic medium
• A semi-analytical perspective on massive red galaxies: I. Assembly history, environment & redshift evolution
• Profiles of cosmic filaments since z=4.0 in cosmological hydrodynamical simulation