The matter distribution in<i>z</i>~ 0.5 redshift clusters of galaxies

Soucail, G.; Foëx, G.; Pointecouteau, É.; Arnaud, M.; Limousin, M.

doi:10.1051/0004-6361/201322689

Cited by 14 publications

(25 citation statements)

References 120 publications

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“…A correlation between the two has been observed in several studies (e.g. Lambas et al 1988;Panko et al 2009;Niederste-Ostholt et al 2010;Soucail et al 2015) and can be interpreted as either a collimated infall of galaxies from filaments (e.g. Dubinski 1998) or due to tidal interactions (e.g.…”

Section: Optical Morphologymentioning

confidence: 73%

From the core to the outskirts: structure analysis of three massive galaxy clusters

Foëx

Chon

Böhringer

2017

A&A

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Aims. The hierarchical model of structure formation is a key prediction of the Λ cold dark matter model, which can be tested by studying the large-scale environment and the substructure content of massive galaxy clusters. We present here a detailed analysis of the clusters RXCJ0225.9-4154, RXCJ0528.9-3927, and RXCJ2308.3-0211, as part of a sample of massive X-ray luminous clusters located at intermediate redshifts.Methods. We used a multiwavelength analysis, combining WFI photometric observations, VIMOS spectroscopy, and the X-ray surface brightness maps. We investigated the optical morphology of the clusters, we looked for significant counterparts in the residual X-ray emission, and we ran several statistical tests to assess their dynamical state. We correlated the results to define various substructure features, to study their properties, and to quantify their influence on simple dynamical mass estimators. Results. RXCJ0225.9-4154 has a bi-modal core, and two massive galaxy groups are located in its immediate surroundings; they are aligned in an elongated structure that is also detected in X-rays at the 1σ level. RXCJ0528.9-3927 is located in a poor environment; an X-ray centroid shift and the presence of two central BCGs provide mild evidence for a recent and active dynamical history. RXCJ2308.3-0211 has complex central dynamics, and it is found at the core of a superstes-cluster. Conclusions. The complexity of the cluster's central dynamics reflects the richness of its large-scale environment: RXCJ0225 and RXCJ2308 present a mass fraction in substructures larger than the typical 5% − 15%, whereas the isolated cluster RXCJ0528 does not have any major substructures within its virial radius. The largest substructures are found in the cluster outskirts. The optical morphology of the clusters correlates with the orientation of their BCG, and with the position of the main axes of accretion.

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Section: Optical Morphologymentioning

confidence: 73%

From the core to the outskirts: structure analysis of three massive galaxy clusters

Foëx

Chon

Böhringer

2017

A&A

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“…While structures 5 and 6 might have an optical counterparts, structure 4 and 7 very likely correspond to fake peaks or to a small group at a different redshift for structure 4. Structures 4 and 6 are also detected in Soucail et al (2015). A larger structure is found at the southwest (8 at 5.5σ κ ), which is not at the cluster redshift, given that it is not detected through the galaxy density contours, but could also be due to a contamination from stars in its vicinity.…”

Section: Individual Clustersmentioning

confidence: 89%

“…It is highly substructured as already found in Guennou et al (2014) and confirmed here by the presence of three spatially separated components: dark matter, X-ray gas, and galaxies. No substructures are detected in the mass reconstruction of Soucail et al (2015), but they used a smoothing kernel more than twice as large as ours. The most important substructures are those noted 2 and 3, the first to the south with a 5σ κ significance and the second to the northeast with a 4.3σ κ significance.…”

Section: Macsj0454mentioning

confidence: 90%

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Weak lensing study of 16 DAFT/FADA clusters: Substructures and filaments

Martinet

Clowe

Durret

et al. 2016

A&A

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While our current cosmological model places galaxy clusters at the nodes of a filament network (the cosmic web), we still struggle to detect these filaments at high redshifts. We perform a weak lensing study for a sample of 16 massive, medium-high redshift (0.4 < z < 0.9) galaxy clusters from the DAFT/FADA survey, which are imaged in at least three optical bands with Subaru/SuprimeCam or CFHT/MegaCam. We estimate the cluster masses using an NFW fit to the shear profile measured in a KSB-like method, adding our contribution to the calibration of the observable-mass relation required for cluster abundance cosmological studies. We compute convergence maps and select structures within these maps, securing their detection with noise resampling techniques. Taking advantage of the large field of view of our data, we study cluster environment, adding information from galaxy density maps at the cluster redshift and from X-ray images when available. We find that clusters show a large variety of weak lensing maps at large scales and that they may all be embedded in filamentary structures at megaparsec scale. We classify these clusters in three categories according to the smoothness of their weak lensing contours and to the amount of substructures: relaxed (∼7%), past mergers (∼21.5%), and recent or present mergers (∼71.5%). The fraction of clusters undergoing merging events observationally supports the hierarchical scenario of cluster growth, and implies that massive clusters are strongly evolving at the studied redshifts. Finally, we report the detection of unusually elongated structures in CLJ0152, MACSJ0454, MACSJ0717, A851, BMW1226, MACSJ1621, and MS1621.

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“…The deflection of light leads to one important theoretical and observational tool in modern astronomy and cosmology: the gravitational lensing (GL). After the observation of the first GL in 1979 [5], many features, including luminous arcs [6,7], Einstein cross [8], Einstein rings [9], GL of CMB [10][11][12], and supernovas [13,14] and even composition features such as the SN Refsdal which combines the Einstein cross with the GL of supernova [15] have been observed. The GL were then used to study properties of the lens [16], coevolution of supermassive black holes (BHs) and galaxies [17], cosmological parameters such as large scale structure (for a review see [18]), properties of the supernova [19], dark matter substructure [20,21], and to discriminate alternative gravitational theories.…”

Section: Introductionmentioning

confidence: 99%

The perturbative approach for the weak deflection angle

Jia

2020

Eur. Phys. J. C

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Both null and timelike rays experience trajectory bending in a gravitational field. In this work, we systematically develop a perturbative method to compute the deflection angle of rays with general velocity v in arbitrary static and spherically symmetric spacetimes and in equatorial plane of arbitrary static and axisymmetric spacetimes. We show that the expansion in the large closest approach x0 limit depends on the asymptotic behavior of the metric functions only, and the generated integrand is always integrable, resulting in a deflection angle in a series form of either x0 or b, the impact parameter. Using this method, the deflection angles as series of both x0 and b are found in Schwarzschild, Reissner-Nordström and Kerr-Newman spacetimes to 17-th, 15-th and 6-th orders respectively, for both lightrays and particles with general velocity. The effects of the impact parameter, velocity and other parameters of the spacatimes are briefly analyzed. Moreover, we show that for spacetimes whose metric functions are only asymptotically known, the deflection angle in the weak field limit can also be calculated. Furthermore, it is shown that the deflection angle in general static and spherically symmetric spacetime and equatorial plane of static and axisymmetric spacetime to the lowest non-trivial order, depends only on the impact parameter, velocity of the particle, and the effective ADM mass of the spacetime but not on other parameters such as charge or angular momentum. These deflection angles are used in an exact gravitational lensing equation and the corresponding apparent angles of the images of the source are also solved perturbatively.

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The matter distribution inz~ 0.5 redshift clusters of galaxies

Cited by 14 publications

References 120 publications

From the core to the outskirts: structure analysis of three massive galaxy clusters

From the core to the outskirts: structure analysis of three massive galaxy clusters

Weak lensing study of 16 DAFT/FADA clusters: Substructures and filaments

The perturbative approach for the weak deflection angle

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