Properties of gas phases around cosmic filaments at<i>z</i>= 0 in the IllustrisTNG simulation

Galárraga-Espinosa, Daniela; Aghanim, N.; Langer, M.; Tanimura, Hidehiko

doi:10.1051/0004-6361/202039781

Cited by 42 publications

(42 citation statements)

References 99 publications

(231 reference statements)

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“…As we can see, the number of cosmic filaments that are connected to clusters and the departure from spherical symmetry are significantly correlated for both the DM and the WHIM gasphase. In agreement with Galárraga-Espinosa et al (2021a) who found that WHIM gas phase is strongly dominant in cosmic filaments, we conclude that azimuthal distribution of WHIM tends to follow DM by tracing cosmic filamentary structures connected to clusters at their peripheries.…”

Section: Mass and Connectivity Dependencysupporting

confidence: 92%

“…At larger distances from cluster center (> 3R 200 ), the distribution of the gas in temperature-density diagrams appears distributed in the different phases: cold diffuse (IGM), cold dense (halo gas), warm diffuse (WHIM), warm dense (WCGM) and hot gas. This temperature-density distribution is quite similar to the expected distribution of overall cosmic gas in the universe at z = 0 (see figure 2 of Galárraga-Espinosa et al 2021a, which considered all gas cells in the simulation box). Therefore, it suggests that beyond radial distances larger that 3R 200 the influence of cluster environments is no more significant.…”

Section: The Gas Phasessupporting

confidence: 75%

“…We consider all the gas cells contained around our 415 halo samples up to 5×R 200 (labeled as PartType0 in IllustrisTNG). We focus here on two thermodynamical properties: the temperature T (computed under the assumption of perfect monoatomic gas, as in Galárraga-Espinosa et al 2021a) and the n H hydrogen number density which is a direct tracer of the total gas density (directly pre-computed in IllustrisTNG). We refer to, Martizzi et al (2019) for an accurate description of gas properties in the different cosmic web environments (voids, walls, filaments, and nodes), and Galárraga-Espinosa et al (2021a) for a complete study of gas thermodynamics inside cosmic filaments; two studies of cosmic gas using the IllustrisTNG simulation.…”

Section: Radial Gas Distribution In Cluster Environmentsmentioning

confidence: 99%

“…We now probe the detail radial profile of the different gas phases as a function of cluster-centric distance. Similarly to Galárraga-Espinosa et al (2021a), we defined the mass fraction of a given gas phase such as:…”

Section: The Gas Phasesmentioning

confidence: 99%

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Gas distribution from clusters to filaments in IllustrisTNG

Gouin,

Gallo,

Aghanim

2022

Preprint

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Matter distribution in the environment of galaxy clusters, from their cores to their connected cosmic filaments, must be in principle related to the underlying cluster physics and it evolutionary state. We aim to investigate how radial and azimuthal distribution of gas is affected by cluster environments, and how it can be related to cluster mass assembly history. Radial physical properties of gas (velocity, temperature, and density) is first analysed around 415 galaxy cluster environments from IllustrisTNG simulation at z = 0. Whereas hot plasma is virialised inside clusters (< R200), the dynamics of warm hot inter-galactic medium (WHIM) can be separated in two regimes: accumulating and slowly infalling gas at cluster peripheries (∼ R200) and fast infalling motions outside clusters (> 1.5R200). The azimuthal distribution of dark matter (DM), hot and warm gas phases is secondly statistically probed by decomposing their 2-D distribution in harmonic space. Inside clusters, the azimuthal symmetries of DM and hot gas are well tracing cluster structural properties, such as their center offsets, substructure fractions and elliptical shapes. Beyond cluster virialised regions, we found that WHIM gas follows the azimuthal distribution of DM by tracing cosmic filament patterns. Azimuthal symmetries of hot and warm gas distribution is finally shown to be imprints of cluster mass assembly history, by strongly correlating with the formation time, mass accretion rate, and dynamical state of clusters. Azimuthal mode decomposition of 2-D gas distribution is a promising probe to assess the 3-D physical and dynamical cluster properties up to their connected cosmic filaments.

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Section: Mass and Connectivity Dependencysupporting

confidence: 92%

Section: The Gas Phasessupporting

confidence: 75%

Section: Radial Gas Distribution In Cluster Environmentsmentioning

confidence: 99%

Section: The Gas Phasesmentioning

confidence: 99%

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Gas distribution from clusters to filaments in IllustrisTNG

Gouin,

Gallo,

Aghanim

2022

Preprint

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“…Malavasi et al 2021;Kotecha et al 2021, however see also Liao & Gao 2019;Song et al 2021), and the intergalactic medium (e.g. Klar & Mücket 2012;Galárraga-Espinosa et al 2021).…”

Section: Discussionmentioning

confidence: 99%

COWS: A filament finder for Hessian cosmic web identifiers

Pfeifer,

Libeskind,

Hoffman

et al. 2022

Preprint

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The large scale galaxy and matter distribution is often described by means of the cosmic web made up of voids, sheets, filaments and knots. Many different recipes exist for identifying this cosmic web. Here we focus on a sub-class of cosmic web identifiers, based on the analysis of the Hessian matrix, and proposed a method, called COsmic Web Skeleton (COWS), of separating a set of filaments cells into an ensemble of individual discreet filaments. Specifically, a thinning algorithm is applied to velocity shear tensor based cosmic web (V-web) to identify the spine of the filaments. This results in a set of filaments with well defined end-point and length. It is confirmed that these sit at local density ridges and align with the appropriate direction defined by the underlying velocity field. The radial density profile of these curved cylindrical filaments, as well as the distribution of their lengths is also examined. The robustness of all results is checked against resolution and the V-web threshold. The code for the COWS method has been made publicly available.

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Shape and connectivity of groups and clusters: Effect of the dynamical state and accretion history

Gouin

Bonnaire

Aghanim

2021

A&A

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Matter distribution around clusters is highly anisotropic because clusters are the nodes of the cosmic web. The shape of the clusters and the number of filaments to which they are connected, that is, their connectivity, is thought to reflect their level of anisotropic matter distribution and must in principle be related to their physical properties. We investigate the effect of the dynamical state and the formation history on both the morphology and local connectivity of about 2400 groups and clusters of galaxies from the large hydrodynamical simulation IllustrisTNG at z = 0. We find that the mass of groups and clusters mainly affects the geometry of the matter distribution: Massive halos are significantly more elliptical and are more strongly connected to the cosmic web than low-mass halos. Beyond the mass-driven effect, ellipticity and connectivity are correlated and are imprints of the growth rate of groups and clusters. Both anisotropy measures appear to trace different dynamical states, such that unrelaxed groups and clusters are more elliptical and more connected than relaxed ones. This relation between matter anisotropies and dynamical state is the sign of different accretion histories. Relaxed groups and clusters have mostly been formed a long time ago and are slowly accreting matter at the present time. They are highly spherical and weakly connected to their environment, mostly because they had enough time to relax and thus lost the connection with their preferential directions of accretion and merging. In contrast, late-formed unrelaxed objects are highly anisotropic with strong connectivities and ellipticities. These groups and clusters are in their formation phase and must be strongly affected by the infalling of materials from filaments.

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Properties of gas phases around cosmic filaments atz= 0 in the IllustrisTNG simulation

Cited by 42 publications

References 99 publications

Gas distribution from clusters to filaments in IllustrisTNG

Gas distribution from clusters to filaments in IllustrisTNG

COWS: A filament finder for Hessian cosmic web identifiers

Shape and connectivity of groups and clusters: Effect of the dynamical state and accretion history

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