On the projected mass distribution around galaxy clusters

Codis, Sandrine; Gavazzi, R.; Gouin, C.

doi:10.1051/0004-6361/201630091

Cited by 9 publications

(12 citation statements)

References 54 publications

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“…Equation (A.8) simply quantifies the boost imposed by the peak condition in the initial conditionsδ c,i . This is consistent with the perturbative approach of Codis et al (2017) who showed that gravitational evolution induces a non-linear bias at all multipoles proportional to the peak height ν, the amplitude of fluctuations σ 0 ∝ D(a) and the rescaled three-point function ξ (3) . The agreement between both approaches follows from the D(a)δ c,i ↔ σ 0 ν correspondence.…”

Section: A1 the Weakly Non-linear Regimesupporting

confidence: 91%

“…To first order, the non-linear evolution of mass shells sinking towards the centre of clusters induces a boost of power at all angular scales due to the contraction of the Lagrangian patch initially encompassing the mass fluctuations. When the density field is nearly Gaussian, only m ≤ 2 moments are affected by the peak constraint, as demonstrated in Codis et al (2017), while in the quasi-linear regime this paper also predicts, perturbatively, the achromatic boost. In the highly non-linear regime, a simple model based on the spherical collapse model was presented, and is found to be in good agreement with measurements on massive haloes extracted from the PLUS Dark Matter cosmological simulation.…”

Section: Redshift Mass Binmentioning

confidence: 53%

“…From Eq. (A.8) and Codis et al (2017), it appears that the excess amplitude of harmonics scales like D(a) at first order. However, these predictions are only valid in the weakly non-linear regime.…”

Section: A1 the Weakly Non-linear Regimementioning

confidence: 89%

“…The formalism must be updated to deal with a particular flavour of three-point statistics that accounts for the presence of a maximum with a specific height ν p of the density field at the origin of the coordinate system. In brief, the companion paper (Codis et al 2017) has shown that the effect of the peak constraint is to -significantly boost the monopole (we are near a peak); -significantly remove power from the dipole (we are now well centred on the peak); -slightly suppress the power of the quadrupole; -leave all other m ≥ 3 multipoles unchanged.…”

Section: The Statistics Of Q M Under Peak Constraintmentioning

confidence: 92%

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Multipolar moments of weak lensing signal around clusters

Gouin

Gavazzi

Codis

et al. 2017

A&A

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Context. Upcoming weak lensing surveys such as Euclid will provide an unprecedented opportunity to quantify the geometry and topology of the cosmic web, in particular in the vicinity of lensing clusters. Aims. Understanding the connectivity of the cosmic web with unbiased mass tracers, such as weak lensing, is of prime importance to probe the underlying cosmology, seek dynamical signatures of dark matter, and quantify environmental effects on galaxy formation. Methods. Mock catalogues of galaxy clusters are extracted from the N-body PLUS simulation. For each cluster, the aperture multipolar moments of the convergence are calculated in two annuli (inside and outside the virial radius). By stacking their modulus, a statistical estimator is built to characterise the angular mass distribution around clusters. The moments are compared to predictions from perturbation theory and spherical collapse. Results. The main weakly chromatic excess of multipolar power on large scales is understood as arising from the contraction of the primordial cosmic web driven by the growing potential well of the cluster. Besides this boost, the quadrupole prevails in the cluster (ellipsoidal) core, while at the outskirts, harmonic distortions are spread on small angular modes, and trace the non-linear sharpening of the filamentary structures. Predictions for the signal amplitude as a function of the cluster-centric distance, mass, and redshift are presented. The prospects of measuring this signal are estimated for current and future lensing data sets.Conclusions. The Euclid mission should provide all the necessary information for studying the cosmic evolution of the connectivity of the cosmic web around lensing clusters using multipolar moments and probing unique signatures of, for example, baryons and warm dark matter.

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Section: A1 the Weakly Non-linear Regimesupporting

confidence: 91%

Section: Redshift Mass Binmentioning

confidence: 53%

Section: A1 the Weakly Non-linear Regimementioning

confidence: 89%

Section: The Statistics Of Q M Under Peak Constraintmentioning

confidence: 92%

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Multipolar moments of weak lensing signal around clusters

Gouin

Gavazzi

Codis

et al. 2017

A&A

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show abstract

“…Using the multipolar expansion of 2-D matter distribution around galaxy clusters, this technique succeeded in highlighting both the elliptical shape of clusters (see e.g Clampitt & Jain 2016;Shin et al 2018),. and filamentary patterns at cluster outskirts(Dietrich et al 2005;Mead et al 2010;Gouin et al 2017;Codis et al 2017) from 2-D projected DM distribution.…”

mentioning

confidence: 99%

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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Probing the azimuthal environment of galaxies around clusters

Gouin

Aghanim

Bonjean

et al. 2020

A&A

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Galaxy clusters are connected at their peripheries to the large scale structures by cosmic filaments that funnel accreting material. These filamentary structures are studied to investigate both environment-driven galaxy evolution and structure formation and evolution. In the present work, we probe in a statistical manner the azimuthal distribution of galaxies around clusters as a function of the cluster-centric distance, the cluster richness, and the galaxy activity (star-forming or passive). We perform a harmonic decomposition in large photometric galaxy catalogue around 6400 SDSS clusters with masses M > 10 14 solar masses, in the redshift range of 0.1 < z < 0.3. The same analysis is performed on the mock galaxy catalogue from the light-cone of Magneticum hydrodynamical simulation. We use the multipole analysis to quantify asymmetries in the 2-D galaxy distribution. In the inner cluster regions at R < 2R500, we confirm that the galaxy distribution traces an ellipsoidal shape, which is more pronounced for richest clusters. In the clusters' outskirts (R = [2 − 8]R500), filamentary patterns are detected in harmonic space with a mean angular scale mmean = 4.2 ± 0.1. Massive clusters seem to have a larger number of connected filaments than low massive ones. We also find that passive galaxies appear to better trace the filamentary structures around clusters, even if the contribution of SF ones tend to increase with the cluster-centric distance, suggesting a gradient of galaxy activity in filaments around clusters.

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On the projected mass distribution around galaxy clusters

Cited by 9 publications

References 54 publications

Multipolar moments of weak lensing signal around clusters

Multipolar moments of weak lensing signal around clusters

Gas distribution from clusters to filaments in IllustrisTNG

Probing the azimuthal environment of galaxies around clusters

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