Lensing measurements of the ellipticity of luminous red galaxies dark matter haloes

Clampitt, Joseph; Jain, Bhuvnesh

doi:10.1093/mnras/stw254

Cited by 50 publications

(104 citation statements)

References 48 publications

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“…On group/cluster scales, several authors have constrained the halo ellipticity from stacked weak-lensing measurements ( (Clampitt & Jain 2016), broadly consistent with ΛCDM predictions. We note that, in their approach, one probes halo quadrupoles with respect to the major axis of the light distribution (e.g., BCGs) chosen as a reference orientation.…”

Section: Comparison With Other Observational Studiesmentioning

confidence: 61%

“…To this end, we employ the Cartesian estimators of Clampitt & Jain (2016) that null the purely tangential, monopole shear contribution. Specifically, we measure the stacked quadrupole shear signal with respect to a coordinate system with the xaxis aligned with the X-ray major axis of each cluster.…”

Section: Weak-lensing Quadrupole Shear Measurementmentioning

confidence: 99%

“…Specifically, we measure the stacked quadrupole shear signal with respect to a coordinate system with the xaxis aligned with the X-ray major axis of each cluster. We adopt the same sign convention for the Cartesian g 1 and g 2 components as defined in Clampitt & Jain (2016;see their Figure 1) and use θ to denote the azimuthal angle relative to the x-axis. Following Clampitt & Jain (2016), we group together the first and second shear components of background galaxies in the regions where cos 4θ and sin 4θ have the same sign (Figure 7), respectively, and define the following estimator:…”

Section: Weak-lensing Quadrupole Shear Measurementmentioning

confidence: 99%

“…the source-averaged critical surface density for a given cluster (Section 2.1), w (k) is the statistical weight for the kth background galaxy (Section 3.3.1), and k runs over all background galaxies that fall in the specified bin, different for each shear component α and sign s (Clampitt & Jain 2016): α=1, s=−, −π/8θ j <π/8; α=1, s=+, π/8θ j <3π/8; α=2, s=−, 0θ j <π/4; α=2, s=+, π/4θ j <π/2. For each case, the summation in Equation (31) also includes background galaxies lying in symmetrical regions shifted by π/2, π, and 3π/2, as illustrated in Figure 7.…”

Section: Weak-lensing Quadrupole Shear Measurementmentioning

confidence: 99%

“…The resulting stacked quadrupole profiles for our cluster sample are shown in Figure 8. Clampitt & Jain (2016) modeled the quadrupole shear signal using a multipole expansion of the surface mass density of elliptical halos (Adhikari et al 2015). However, this method can only be applied to the case with a small halo ellipticity, so that the higher-order terms can be safely ignored.…”

Section: Weak-lensing Quadrupole Shear Measurementmentioning

confidence: 99%

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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 Other Observational Studiesmentioning

confidence: 61%

Section: Weak-lensing Quadrupole Shear Measurementmentioning

confidence: 99%

Section: Weak-lensing Quadrupole Shear Measurementmentioning

confidence: 99%

Section: Weak-lensing Quadrupole Shear Measurementmentioning

confidence: 99%

Section: Weak-lensing Quadrupole Shear Measurementmentioning

confidence: 99%

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

Umetsu

Sereno

Tam

et al. 2018

ApJ

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Cluster–galaxy weak lensing

Umetsu

2020

Astron Astrophys Rev

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Weak gravitational lensing of background galaxies provides a direct probe of the projected matter distribution in and around galaxy clusters. Here, we present a self-contained pedagogical review of cluster–galaxy weak lensing, covering a range of topics relevant to its cosmological and astrophysical applications. We begin by reviewing the theoretical foundations of gravitational lensing from first principles, with a special attention to the basics and advanced techniques of weak gravitational lensing. We summarize and discuss key findings from recent cluster–galaxy weak-lensing studies on both observational and theoretical grounds, with a focus on cluster mass profiles, the concentration–mass relation, the splashback radius, and implications from extensive mass-calibration efforts for cluster cosmology.

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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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Lensing measurements of the ellipticity of luminous red galaxies dark matter haloes

Cited by 50 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*

Cluster–galaxy weak lensing

Multipolar moments of weak lensing signal around clusters

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