On the accretion history of galaxy clusters: temporal and spatial distribution

Vallés-Pérez, David; Planelles, S.; Quilis, Vicent

doi:10.1093/mnras/staa3035

Cited by 30 publications

(30 citation statements)

References 62 publications

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“…As presented in Schneider & Bartelmann (1997) show that the dominant azimuthal order is the quadrupole m = 2 (see also Vallés-Pérez et al 2020) and the second most significant azimuthal symmetric orders are m = 1, 3, 4 with contributions higher than 10% (see also Gouin et al 2020). In details, the azimuthal matter distribution inside galaxy clusters (up to R 200 ) is almost quadrupolar, whereas the matter distribution in cluster infalling regions (from R 200 to 4 × R 200 ) is mainly traced by the harmonic orders m = 1, 2, 3, 4.…”

Section: Appendix A: Multipolar Expansion Of Dm Distributionmentioning

confidence: 90%

“…with |Q m | the modulus of the aperture multipole moment at the order m. By decomposing surface mass density in harmonic expansion terms, Schneider & Weiss (1991) have shown that |Qm| |Q0| −→ 1/2 for a matter distribution Σ(θ) ∝ cos(2θm). Therefore, the value of multipolar ratio β m varies between 0 and 1/2, such that β m = 0 for a circular matter distribution and β m = 1/2 for a matter distribution describing the azimuthal symmetry at the order m (see also Vallés-Pérez et al 2020, for a similar definition).…”

Section: Formalism Of Multipole Moments Q Mmentioning

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: Appendix A: Multipolar Expansion Of Dm Distributionmentioning

confidence: 90%

Section: Formalism Of Multipole Moments Q Mmentioning

confidence: 99%

Gas distribution from clusters to filaments in IllustrisTNG

Gouin,

Gallo,

Aghanim

2022

Preprint

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“…The simulation analysed in this paper has been carried out with the cosmological code MASCLET [42], and has been already employed in a series of previous works [43,44,45]. Here we shall introduce the main details of the simulation, while some topics which are not intimately connected to the analyses in this paper can be found in more detail in the aforementioned references.…”

Section: Simulation Detailsmentioning

confidence: 99%

“…This same object has been analysed in great detail in[44] (focusing on its observational properties) and[45] (exploring its accretion history).…”

mentioning

confidence: 99%

Unravelling cosmic velocity flows: a Helmholtz-Hodge decomposition algorithm for cosmological simulations

Vallés-Pérez,

Planelles,

Quilis

2021

Preprint

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In the context of intra-cluster medium turbulence, it is essential to be able to split the turbulent velocity field in a compressive and a solenoidal component. We describe and implement a new method for this aim, i.e., performing a Helmholtz-Hodge decomposition, in multi-grid, multi-resolution descriptions, focusing on (but not being restricted to) the outputs of AMR cosmological simulations. The method is based on solving elliptic equations for a scalar and a vector potential, from which the compressive and the solenoidal velocity fields, respectively, are derived through differentiation. These equations are addressed using a combination of Fourier (for the base grid) and iterative (for the refinement grids) methods. We present several idealised tests for our implementation, reporting typical median errors in the order of 1‰-1%, and with 95-percentile errors below a few percents. Additionally, we also apply the code to the outcomes of a cosmological simulation, achieving similar accuracy at all resolutions, even in the case of highly non-linear velocity fields. We finally take a closer look to the decomposition of the velocity field around a massive galaxy cluster.

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“…The inner slope of the mass distribution might deviate from the NFW model because of several processes such as dynamical friction, central condensation of cooled gas, and active galactic nucleus (AGN) feedback (e.g., Blumenthal et al 1986;Martizzi et al 2012;Schaller et al 2015;Laporte & White 2015;Peirani et al 2017;He et al 2020). The external slope of the mass distribution in individual clusters might deviate from the NFW model depending on the mass accretion rate in the cluster outskirts (e.g., Diemer & Kravtsov 2014;More et al 2015;Vallés-Pérez et al 2020). The shape of the cluster mass profile also depends on the properties of the dark matter (DM) component.…”

Section: Introductionmentioning

confidence: 99%

The GOGREEN survey: the internal dynamics of clusters of galaxies at redshift 0.9-1.4

Biviano,

van der Burg,

Balogh

et al. 2021

Preprint

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Context. The study of galaxy cluster mass profiles (M(r)) provides constraints on the nature of dark matter and on physical processes affecting the mass distribution. The study of galaxy cluster velocity anisotropy profiles (β(r)) informs the orbits of galaxies in clusters, which are related to their evolution. The combination of mass profiles and velocity anisotropy profiles allows us to determine the pseudo phase-space density profiles (Q(r)); numerical simulations predict that these profiles follow a simple power law in cluster-centric distance. Aims. We determine the mass, velocity anisotropy, and pseudo phase-space density profiles of clusters of galaxies at the highest redshifts investigated in detail to date. Methods. We exploited the combination of the GOGREEN and GCLASS spectroscopic data-sets for 14 clusters with mass M 200 ≥ 10 14 M ⊙ at redshifts 0.9 ≤ z ≤ 1.4. We constructed an ensemble cluster by stacking 581 spectroscopically identified cluster members with stellar mass M ⋆ ≥ 10 9.5 M ⊙ . We used the MAMPOSSt method to constrain several M(r) and β(r) models, and we then inverted the Jeans equation to determine the ensemble cluster β(r) in a non-parametric way. Finally, we combined the results of the M(r) and β(r) analysis to determine Q(r) for the ensemble cluster. Results. The concentration c 200 of the ensemble cluster mass profile is in excellent agreement with predictions from Lambda cold dark matter (ΛCDM) cosmological numerical simulations, and with previous determinations for clusters of similar mass and at similar redshifts, obtained from gravitational lensing and X-ray data. We see no significant difference between the total mass density and either the galaxy number density distributions or the stellar mass distribution. Star-forming galaxies are spatially significantly less concentrated than quiescent galaxies. The orbits of cluster galaxies are isotropic near the center and more radial outside. Star-forming galaxies and galaxies of low stellar mass tend to move on more radially elongated orbits than quiescent galaxies and galaxies of high stellar mass. The profile Q(r), determined using either the total mass or the number density profile, is very close to the power-law behavior predicted by numerical simulations. Conclusions. The internal dynamics of clusters at the highest redshift probed in detail to date are very similar to those of lower-redshift clusters, and in excellent agreement with predictions of numerical simulations. The clusters in our sample have already reached a high degree of dynamical relaxation.

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On the accretion history of galaxy clusters: temporal and spatial distribution

Cited by 30 publications

References 62 publications

Gas distribution from clusters to filaments in IllustrisTNG

Gas distribution from clusters to filaments in IllustrisTNG

Unravelling cosmic velocity flows: a Helmholtz-Hodge decomposition algorithm for cosmological simulations

The GOGREEN survey: the internal dynamics of clusters of galaxies at redshift 0.9-1.4

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