Properties of the diffuse gas component in filaments detected in the Dianoga cosmological simulations

Abstract

Hydrodynamical cosmological simulations are ideal laboratories where the evolution of the cosmic web can be studied. This allows for easier insight into the nature of the filaments. We investigate how the intrinsic properties of filaments are evolving in areas extracted from a larger cosmological simulation. We aim to identify significant trends in the properties of Warm-Hot Intergalactic Medium (WHIM) and suggest possible explanations. To study the filaments and their contents, we select a subset of regions from the Dianoga simulation. We analysed these regions that were simulated with different baryon physics, namely with and without the AGN feedback. We construct the cosmic web using the Sub-space Constrained Mean Shift (SCMS) algorithm and the Sequential Chain Algorithm for Resolving Filaments (SCARF). We examined the basic physical properties of filaments (length, shape, mass, radius) and analysed different gas phases (hot, WHIM and colder gas components) within those structures. The evolution of the global filament properties and the properties of the gas phases were studied in the redshift range $0<z<1.48$. Within our simulations, the detected filaments have, on average, lengths below $9$ Mpc. The filaments' shape correlates with their length; the longer they are, the more likely they are curved. We find that the scaling relation between mass $M$ and length $L$ of the filaments is well described by the power law $M\propto L^{1.7}$. The radial density profile is widening with redshift, meaning that the radius of the filaments is getting larger over time. The fraction of gas mass in the WHIM phase does not depend on the model and is rising towards lower redshifts. However, the included baryon physics has a strong impact on the metallicity of gas in filaments, indicating that the AGN feedback impacts the metal content already at redshifts of $z\sim 2$.

16 pages, 13 figures

References in corpus (18)

• The effect of photo-ionization on the cooling rates of enriched, astrophysical plasmas
• Chemical enrichment of galaxy clusters from hydrodynamical simulations
• A refined sub-grid model for black hole accretion and AGN feedback in large cosmological simulations
• Detection of hot gas in the filament connecting the clusters of galaxies Abell 222 and Abell 223
• The VIMOS Public Extragalactic Redshift Survey (VIPERS): Galaxy segregation inside filaments at $z\simeq 0.7$
• Pressure of the hot gas in simulations of galaxy clusters
• The SAMI Galaxy Survey: First detection of a transition in spin orientation with respect to cosmic filaments in the stellar kinematics of galaxies
• Gas and galaxies in filament between clusters of galaxies: The study of A399-A401
• 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
• First detection of stacked X-ray emission from cosmic web filaments
• The ThreeHundred: the structure and properties of cosmic filaments in the outskirts of galaxy clusters
• Like a spider in its web: a study of the Large Scale Structure around the Coma cluster
• Warm-Hot Intergalactic Medium Associated with the Coma Cluster
• Cosmic filaments in galaxy cluster outskirts: quantifying finding filaments in redshift space
• Large Scale Structure in CHILES
• Suzaku Observations of the Outskirts of the Galaxy Cluster Abell 3395 including a Filament toward Abell 3391
• A detailed study of the bridge of excess X-ray emission between the galaxy clusters Abell 2029 and Abell 2033
• Prospects of detecting soft X-ray emission from typical WHIM filaments around massive clusters and the Coma cluster soft excess