The ellipticity of galaxy cluster haloes from satellite galaxies and weak lensing

Shin, T.; Clampitt, Joseph; Jain, Bhuvnesh; Bernstein, G. M.; Neil, Andrew R.; Rozo, Eduardo; Rykoff, E. S.

doi:10.1093/mnras/stx3366

Cited by 56 publications

(67 citation statements)

References 58 publications

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“…(17) The ICL ellipticity increases with radius and reaches = 0.4 − 0.5 at a circular radius of r ≈ 200 kpc. That is consistent with the ellipticity of cluster Dark Matter halos (Shin et al 2018).…”

Section: Discussionsupporting

confidence: 86%

“…We have selected a subset of 50 clusters from our dataset with the most reliable cluster PA and cluster center measurements. We use the satellite galaxies as test particles for the underlying Dark Matter distribution (e.g., Shin et al 2018).…”

Section: Discussionmentioning

confidence: 99%

“…The average ellipticity of Dark Matter halos can be measured by using satellite galaxies as test particles or using stacked weak lensing measurements. Both methods have been applied by Shin et al (2018) for 10 428 SDSS clusters. They found an average axis ratio (b/a) DM = 0.573 ± 0.002(stat)±0.039(sys) using the satellite galaxy method or (b/a) DM = 0.56 ± 0.09(stat)±0.03(sys) using the stacked weak lensing method.…”

Section: Discussionmentioning

confidence: 99%

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Structure of Brightest Cluster Galaxies and Intracluster Light

Kluge

Neureiter

Riffeser

et al. 2020

ApJS

120

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Observations of 170 local (z 0.08) galaxy clusters in the northern hemisphere have been obtained with the Wendelstein Telescope Wide Field Imager (WWFI). We correct for systematic effects such as PSF broadening, foreground stars contamination, relative bias offsets and charge persistence. Scattered light induced background inhomogeneities are reduced down to ∆SB > 31 g' mag arcsec −2 by large dithering and subtraction of night-sky flats. Residual background inhomogeneities brighter than SB σ < 27.6 g' mag arcsec −2 caused by galactic cirrus are detected in front of 23% of the clusters. However, the large field of view allows to discriminate between accretion signatures and galactic cirrus. We detect accretion signatures in form of tidal streams in 22%, shells in 9.4%, multiple nuclei in 47% and two Brightest Cluster Galaxies (BCGs) in 7% of the clusters / BCGs.We measure semi-major axis surface brightness profiles of the BCGs and their surrounding Intracluster Light (ICL) down to a limiting surface brightness of SB = 30 g' mag arcsec −2 . The spatial resolution in the inner regions is increased by combining the WWFI light profiles with those that we measured from archival Hubble Space Telescope images or deconvolved WWFI images. We find that 71% of the BCG+ICL systems have SB profiles that are well described by a single Sérsic (SS) function whereas 29% require a double Sérsic (DS) function to obtain a good fit. SS BCGs, having more symmetric isophotal shapes and fewer detected accretion signatures than DS BCGs, appear to have slightly more relaxed morphology than their DS counterparts. Members of the latter type encompass S2 = 52 ± 21% of their total light in the outer Sérsic component. There is a wide scatter in transition radii r × between the two Sérsic components and surface brightnesses at the transition radii SB(r × ). The integrated brightnesses of the BCG+ICL systems correlate only weakly with S2, r × and SB(r × ). That indicates that the outer Sérsic component is unlikely to trace the dynamically hot ICL since BCG+ICL systems grow at present epoch predominantly in their outskirts.We find that BCGs have scaling relations that differ markedly from those of normal ellipticals, likely due to their indistinguishable embedding in the ICL. The most extended BCG+ICL systems have luminosities and radii comparable to whole clusters. We use different plausible estimates for the ICL component (based on an integrated brightness threshold, SB thresholds and profile decompositions) and find that they do not affect our conclusions about the properties of the ICL. On average, the ICL seems to be better aligned than the BCG with the host cluster in terms of position angle and centering. That makes it a potential Dark Matter tracer. We find positive correlations between BCG+ICL brightness and cluster mass, cluster radius, cluster richness and integrated satellite brightness, confirming that BCG/ICL growth is indeed coupled with cluster growth.

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Section: Discussionsupporting

confidence: 86%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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Structure of Brightest Cluster Galaxies and Intracluster Light

Kluge

Neureiter

Riffeser

et al. 2020

ApJS

120

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“…More recently, Shin et al (2018) studied the stacked halo ellipticity for a sample of ∼10 4 SDSS redMaPPer clusters. Stacking the quadrupole shear signal along the major axis of the cluster member distribution, they found a mean axis ratio of 0.558±0.086±0.026 (statistical followed by systematic uncertainty).…”

Section: Weak-lensing Quadrupole Shear Measurementmentioning

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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“…The ellipsoidal shape of clusters has been estimated via different observables such as, galaxy distribution (e.g. Paz et al 2006;Shin et al 2018), X-ray surface brightness (e.g. Kawahara 2010;Lovisari et al 2017), gravitational lensing (Evans & Bridle 2009;Oguri et al 2010;van Uitert et al 2017), and Sunyaev Zel'dovich (SZ) effect (e.g.…”

Section: Introductionmentioning

confidence: 99%

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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The ellipticity of galaxy cluster haloes from satellite galaxies and weak lensing

Cited by 56 publications

References 58 publications

Structure of Brightest Cluster Galaxies and Intracluster Light

Structure of Brightest Cluster Galaxies and Intracluster Light

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

Probing the azimuthal environment of galaxies around clusters

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