The Effect of the Cosmic Web on Cluster Weak Lensing Mass Estimates

Metzler, Christopher A.; White, Martin; Loken, C.

doi:10.1086/318406

Cited by 90 publications

(120 citation statements)

References 14 publications

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“…Then all the particles in the direct vicinity of these haloes are extracted and projected along a given direction. Hence, each extracted halo contains a cluster and its outer environment (Metzler et al 2001). The additional effect of the uncorrelated background and foreground matter distribution along the line of 2 http://www2.iap.fr/users/peirani/PLUS/plus.htm sight to distant gravitationally lensed galaxies will be treated as an additional Gaussian random field acting as a noise contribution (see e.g.…”

Section: Dark Matter Haloes In the Plus Cosmological Simulationmentioning

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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Section: Dark Matter Haloes In the Plus Cosmological Simulationmentioning

confidence: 99%

Multipolar moments of weak lensing signal around clusters

Gouin

Gavazzi

Codis

et al. 2017

A&A

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“…Figure 7 shows that almost the entire Planck cluster sample will be excellent targets for weaklensing surveys, having an extremely high S/N. Although line-of-sight projection can be a significant contaminant for weak-lensing studies of the general cluster population (Metzler, White, & Loken 2001;White, van Waerbeke, & Mackey 2002), it is less of a problem for the Planck sample, which consists primarily of the most massive systems. Our conclusions are thus in line with, although slightly stronger than, those of Bartelmann, who suggested that Planck clusters would form an excellent sample for weak-lensing followup.…”

Section: Follow-upmentioning

confidence: 99%

Studying Clusters withPlanck

White

2003

ApJ

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We use mock Sunyaev-Zeldovich effect maps to investigate how well the Planck mission might find and characterize clusters of galaxies. We discuss different combinations of frequency maps and different methods for identifying cluster candidates. For the simplest methods, the catalogs are not complete, even for relatively high mass thresholds, but the all-sky nature of the mission ensures a large sample of massive, high-z clusters that will be ideal for many studies. We make a preliminary attempt to identify the X-ray, optical, and weak-lensing properties of the Planck sample.

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“…It is also limited to intermediate-redshift clusters for which the distant background galaxies are far enough behind the cluster. Gravitational lensing masses are also subject to systematics such as the determination of the redshift distribution of the sources or projection effects of matter structures near the cluster or along the line-of-sight (Metzler et al 2001;Hoekstra 2003;Meneghetti et al 2010).…”

Section: Introductionmentioning

confidence: 99%

The dark matter distribution inz ~ 0.5 clusters of galaxies

Foëx¹,

Soucail²,

Pointecouteau³

et al. 2012

A&A

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The total mass of clusters of galaxies is a key parameter for studing massive halos. It relates to numerous gravitational and baryonic processes at play in the framework of large-scale structure formation, thus rendering its determination both important and challenging. From a sample of the 11 X-ray bright clusters selected from the EXCPRES sample, we investigate the optical and X-ray properties of clusters with respect to their total mass derived from weak gravitational lensing. From multicolor, wide-field imaging obtained with MegaCam at CFHT, we derive the shear profile of each individual cluster of galaxies. We carefully investigate all systematic sources related to the weak lensing mass determination. The weak lensing masses are then compared to the X-ray masses obtained from the analysis of XMM-Newton observations assuming hydrostatic equilibrium. We find good agreement between the two mass proxies although a few outliers with either perturbed morphology or poor quality data prevent deriving robust mass estimates. The weak lensing mass is also correlated with the optical richness and the total optical luminosity, as well as with the X-ray luminosity, to provide scaling relations within the redshift range 0.4 < z < 0.6. These relations are in good agreement with previous works at lower redshifts. For the L X − M relation we combine our sample with two other cluster and group samples from the literature, thus covering two decades in mass and X-ray luminosity, with a regular and coherent correlation between the two physical quantities.

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The Effect of the Cosmic Web on Cluster Weak Lensing Mass Estimates

Cited by 90 publications

References 14 publications

Multipolar moments of weak lensing signal around clusters

Multipolar moments of weak lensing signal around clusters

Studying Clusters withPlanck

The dark matter distribution inz ~ 0.5 clusters of galaxies

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