A CFH12k lensing survey of X-ray luminous galaxy clusters

Bardeau, S.; Soucail, G.; Kneib, Jean-Paul; Czoske, O.; Ebeling, H.; Hudelot, P.; Smail, Ian; Smith, Graham P.

doi:10.1051/0004-6361:20077443

Cited by 82 publications

(152 citation statements)

References 105 publications

(169 reference statements)

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“…Previous studies tend to find a slope in the M − L relation that is slightly larger than one (Lin et al 2004;Popesso et al 2005;Bardeau et al 2007;Reyes et al 2008). This tendency is predicted by some of the semi-analytical models of galaxy formation, at least for massive clusters (Marinoni & Hudson 2002) in which the star formation efficiency can be inhibited by the long cooling times of hot gas on high-mass scales.…”

Section: Optical Scaling Lawsmentioning

confidence: 85%

“…To correct for the PSF smearing, we use the Im2shape software (Bridle et al 2002), which has already demonstrated its potential to recover the intrinsic shape of the galaxies (Cypriano et al 2004;Bardeau et al 2005Bardeau et al , 2007Limousin et al 2007a,b). Starting with a given model for the shape of each object, the code convolves it with the local estimate of the PSF.…”

Section: Object Selectionmentioning

confidence: 99%

“…Mass estimators are usually derived from X-ray data (Markevitch 1998;Arnaud et al 2002;Reiprich & Böhringer 2002;Popesso et al 2005;Morandi et al 2007;Pratt et al 2009;Vikhlinin et al 2009). Several attempts to use weak lensing masses have also been proposed more recently (Hoekstra 2007;Bardeau et al 2007;Rykoff et al 2008;Leauthaud et al 2010;Okabe et al 2010b). Most these studies converge towards a power law that differs from the relation expected in the hierarchical scenario of structure formation where the X-ray luminosity scales with the mass as F −1 z L X ∝ (F z M tot ) 4/3 .…”

Section: X-ray Scaling Lawsmentioning

confidence: 99%

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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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Section: Optical Scaling Lawsmentioning

confidence: 85%

Section: Object Selectionmentioning

confidence: 99%

Section: X-ray Scaling Lawsmentioning

confidence: 99%

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The dark matter distribution inz ~ 0.5 clusters of galaxies

Foëx¹,

Soucail²,

Pointecouteau³

et al. 2012

A&A

Self Cite

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“…This software performs an analytical deconvolution of the galaxy images, approximated by a single elliptical Gaussian, and returns the intrinsic shape parameters with their uncertainties, estimated by a Bayesian analysis of the image residuals. It has been successfully applied on a sample of clusters of galaxies by Bardeau et al (2007), who developed a methodology for the shear analysis that we follow fairly closely. To test the validity of the analysis chain, we checked that the result of the deconvolution process applied to the stellar field itself shrinks the size of the deconvolved stars to less than 0.1 , with a flat distribution of their orientation (Fig.…”

Section: Psf Correction and Galaxy Shape Measurementsmentioning

confidence: 99%

Dark matter distribution in the merging cluster Abell 2163

Soucail¹

2012

A&A

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Context. The cluster Abell 2163 is a merging system of several subclusters with complex dynamics. It presents exceptional X-rays properties (high temperature and luminosity), suggesting that it is a very massive cluster. Recent 2D analysis of the gas distribution has revealed a complex and multiphase structure. Aims. This paper presents a wide-field weak lensing study of the dark matter distribution in the cluster in order to provide an alternative vision of the merging status of the cluster. The 2D mass distribution was built and compared to the galaxies and gas distributions. Methods. A Bayesian method, implemented in the Im2shape software, was used to fit the shape parameters of the faint background galaxies and to correct for PSF smearing. A careful color selection on the background galaxies was applied to retrieve the weak lensing signal. Shear signal was measured out to more than 2 Mpc ( 12 from the center). The radial shear profile was fit with different parametric mass profiles. The 2D mass map was built from the shear distribution and used to identify the different mass components. Results. The 2D mass map agrees with the galaxy distribution, while the total mass inferred from weak lensing shows a strong discrepancy to the X-ray deduced mass. Regardless of the method used, the virial mass M 200 falls in the range 8 to 14 × 10 14 h −1 70 M inside the virial radius (∼2.0 h −1 70 Mpc), a value that is two times less than the mass deduced from X-rays. The central mass clump appears bimodal in the dark matter distribution, with a mass ratio ∼3:1 between the two components. The infalling clump A2163-B is detected in weak lensing as an independent entity. All these results are interpreted in the context of a multiple merger seen less than 1 Gyr after the main crossover.

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“…The methodology used in this work follows Bardeau et al (2007), also applied by Limousin et al (2009) on the first SL2S group sample. A full description of the procedure can be found in Foëx et al (2012), and of its applications in the last SL2S sample in Foëx et al (2013).…”

Section: Weak Lensing Methodsmentioning

confidence: 99%

Characterizing SL2S galaxy groups using the Einstein radius

Verdugo¹,

Motta²,

Foëx³

et al. 2014

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Aims. We aim to study the reliability of R A (the distance from the arcs to the center of the lens) as a measure of the Einstein radius in galaxy groups. In addition, we want to analyze the possibility of using R A as a proxy to characterize some properties of galaxy groups, such as luminosity (L) and richness (N). Methods. We analyzed the Einstein radius, θ E , in our sample of Strong Lensing Legacy Survey (SL2S) galaxy groups, and compared it with R A , using three different approaches: 1) the velocity dispersion obtained from weak lensing assuming a singular isothermal sphere profile (θ E,I ); 2) a strong lensing analytical method (θ E,II ) combined with a velocity dispersion-concentration relation derived from numerical simulations designed to mimic our group sample; and 3) strong lensing modeling (θ E,III ) of eleven groups (with four new models presented in this work) using Hubble Space Telescope (HST) and Canada-France-Hawaii Telescope (CFHT) images. Finally, R A was analyzed as a function of redshift z to investigate possible correlations with L, N, and the richness-to-luminosity ratio (N/L). Results. We found a correlation between θ E and R A , but with large scatter. We estimate θ E,I = (2.2 ± 0.9) + (0.7 ± 0.2)R A , θ E,II = (0.4 ± 1.5) + (1.1 ± 0.4)R A , and θ E,III = (0.4 ± 1.5) + (0.9 ± 0.3)R A for each method respectively. We found weak evidence of anticorrelation between R A and z, with Log R A = (0.58 ± 0.06) − (0.04 ± 0.1)z, suggesting a possible evolution of the Einstein radius with z, as reported previously by other authors. Our results also show that R A is correlated with L and N (more luminous and richer groups have greater R A ), and a possible correlation between R A and the N/L ratio. Conclusions. Our analysis indicates that R A is correlated with θ E in our sample, making R A useful for characterizing properties like L and N (and possibly N/L) in galaxy groups. Additionally, we present evidence suggesting that the Einstein radius evolves with z.

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A CFH12k lensing survey of X-ray luminous galaxy clusters

Cited by 82 publications

References 105 publications

The dark matter distribution inz ~ 0.5 clusters of galaxies

The dark matter distribution inz ~ 0.5 clusters of galaxies

Dark matter distribution in the merging cluster Abell 2163

Characterizing SL2S galaxy groups using the Einstein radius

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