Projected axis ratios of galaxy clusters in the Horizon-AGN simulation: Impact of baryon physics and comparison with observations

Suto, Daichi; Peirani, Sébastien; Dubois, Yohan; Kitayama, Tetsu; Nishimichi, Takahiro; Sasaki, Shin; Suto, Yasushi

doi:10.1093/pasj/psw118

Cited by 30 publications

(43 citation statements)

References 48 publications

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“…More recently, it was shown by Suto et al (2017) that baryonic physics operating in the cluster central region, such as cooling and feedback effects, can have a substantial impact on the non-sphericity of cluster halos up to half the virial radius, even though these baryonic effects have little impact on the spherically averaged DM density profile. They found that the DM distribution becomes more spherical, depending on the distance from the cluster center, when the effects of baryons are included.…”

Section: Comparison With λCdm Predictionsmentioning

confidence: 99%

The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters*

Umetsu

Sereno

Tam

et al. 2018

ApJ

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We reconstruct the two-dimensional (2D) matter distributions in 20 high-mass galaxy clusters selected from the CLASH survey by using the new approach of performing a joint weak gravitational lensing analysis of 2D shear and azimuthally averaged magnification measurements. This combination allows for a complete analysis of the field, effectively breaking the mass-sheet degeneracy. In a Bayesian framework, we simultaneously constrain the mass profile and morphology of each individual cluster, assuming an elliptical Navarro-Frenk-White halo characterized by the mass, concentration, projected axis ratio, and position angle (PA) of the projected major axis. We find that spherical mass estimates of the clusters from azimuthally averaged weak-lensing measurements in previous work are in excellent agreement with our results from a full 2D analysis. Combining all 20 clusters in our sample, we detect the elliptical shape of weak-lensing halos at the 5σ significance level within a scale of 2 h Mpc 1 -. The median projected axis ratio is 0.67±0.07 at a virial mass of M M 15.2 2.8 10 vir 14 = ´ ( ) , which is in agreement with theoretical predictions from recent numerical simulations of the standard collisionless cold dark matter model. We also study misalignment statistics of the brightest cluster galaxy, X-ray, thermal Sunyaev-Zel'dovich effect, and strong-lensing morphologies with respect to the weak-lensing signal. Among the three baryonic tracers studied here, we find that the X-ray morphology is best aligned with the weak-lensing mass distribution, with a median misalignment angle of PA 21We also conduct a stacked quadrupole shear analysis of the 20 clusters assuming that the X-ray major axis is aligned with that of the projected mass distribution. This yields a consistent axis ratio of 0.67±0.10, suggesting again a tight alignment between the intracluster gas and dark matter.

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Section: Comparison With λCdm Predictionsmentioning

confidence: 99%

The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters*

Umetsu

Sereno

Tam

et al. 2018

ApJ

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“…Cosmological effects related, for instance, to the growth rate and dark energy, may have an effect on the relative amplitude of moments. One could extend those measurements to cosmological hydrodynamical simulations in which baryonic physics, such as gas cooling and feedback from active galaxy nuclei, will substantially change the shape of the total mass distribution on small scales (Teyssier et al 2011;Suto et al 2017). These scales may be more efficiently probed by strong lensing observables (following, e.g.…”

Section: Redshift Mass Binmentioning

confidence: 99%

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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“…For example, the shape of dark matter distributions in galaxy clusters are affected by implemented baryon physics (e.g. Bett et al 2010;Schaller et al 2015;Bryan et al 2013;Suto et al 2017), which would be much rounder in all scales up to ∼ 1 Mpc without the feedback effect from the active galactic nucleus (AGN) (e.g. Suto et al 2017).…”

Section: Introductionmentioning

confidence: 99%

“…Bett et al 2010;Schaller et al 2015;Bryan et al 2013;Suto et al 2017), which would be much rounder in all scales up to ∼ 1 Mpc without the feedback effect from the active galactic nucleus (AGN) (e.g. Suto et al 2017). Self interacting dark matter models predict more spherical distributions in the inner region of galaxy clusters than collisionless dark matter (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…There are previous studies to estimate the ellipticities and alignments of different components using the Horizon-AGN simulation. Suto et al (2017) measured ellipticities of projected distributions but they did not study the alignments among different components. Chisari et al (2017) investigated the alignment between galaxies and their host dark matter haloes.…”

Section: Introductionmentioning

confidence: 99%

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Projected alignment of non-sphericities of stellar, gas, and dark matter distributions in galaxy clusters: analysis of the Horizon-AGN simulation

Okabe

Nishimichi

Oguri

et al. 2018

Monthly Notices of the Royal Astronomical Society

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While various observations measured ellipticities of galaxy clusters and alignments between orientations of the brightest cluster galaxies and their host clusters, there are only a handful of numerical simulations that implement realistic baryon physics to allow direct comparisons with those observations. Here we investigate ellipticities of galaxy clusters and alignments between various components of them and the central galaxies in the state-of-the-art cosmological hydrodynamical simulation Horizon-AGN, which contains dark matter, stellar, and gas components in a large simulation box of (100h −1 Mpc) 3 with high spatial resolution (∼ 1 kpc). We estimate ellipticities of total matter, dark matter, stellar, gas surface mass density distributions, X-ray surface brightness, and the Compton y-parameter of the Sunyaev-Zel'dovich effect, as well as alignments between these components and the central galaxies for 120 projected images of galaxy clusters with masses M 200 > 5 × 10 13 M . Our results indicate that the distributions of these components are well aligned with the major-axes of the central galaxies, with the root mean square value of differences of their position angles of ∼ 20 • , which vary little from inner to the outer regions. We also estimate alignments of these various components with total matter distributions, and find tighter alignments than those for central galaxies with the root mean square value of ∼ 15 • . We compare our results with previous observations of ellipticities and position angle alignments and find reasonable agreements. The comprehensive analysis presented in this paper provides useful prior information for analyzing stacked lensing signals as well as designing future observations to study ellipticities and alignments of galaxy clusters.

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Projected axis ratios of galaxy clusters in the Horizon-AGN simulation: Impact of baryon physics and comparison with observations

Cited by 30 publications

References 48 publications

The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters*

The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters*

Multipolar moments of weak lensing signal around clusters

Projected alignment of non-sphericities of stellar, gas, and dark matter distributions in galaxy clusters: analysis of the Horizon-AGN simulation

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