Abell 2142 at large scales: An extreme case for sloshing?

Rossetti, M.; Eckert, D.; Grandi, S. De; Gastaldello, F.; Ghizzardi, S.; Röediger, E.; Molendi, S.

doi:10.1051/0004-6361/201321319

Cited by 102 publications

(116 citation statements)

References 46 publications

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“…Could these lower mass concentrations found by methods based upon internal kinematics be a sign that A2142 is out of dynamical equilibrium? The substructures found by Owers et al (2011) and the results by Rossetti et al (2013) on the importance of the mergers undergone by A2142 suggest that full relaxation is to be excluded. On the other hand, the agreement on the virial radius amongst the different methods and with the results from X-ray and lensing (the latter does not require equilibrium) suggests that A2142 is not far from dynamical equilibrium.…”

Section: Discussionmentioning

confidence: 85%

“…The merging scenario is also supported by the presence of substructures of galaxies lying along the direction of the cluster elongation, as found in the SZ maps by Umetsu et al (2009), lensing analysis by Okabe & Umetsu (2008), and analysis of the distribution of LOS velocities of Owers et al (2011). However, after analysing XMMNewton images to investigate the cold fronts of A2142, Rossetti et al (2013) argue that the mergers have intermediate mass ratios rather than major ones.…”

Section: Introductionmentioning

confidence: 77%

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Mass, velocity anisotropy, and pseudo phase-space density profiles of Abell 2142

Munari

Biviano

Mamon

2014

A&A

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Aims. We aim to compute the mass and velocity anisotropy profiles of Abell 2142 and, from there, the pseudo phase-space density profile Q(r) and the density slope − velocity anisotropy β − γ relation, and then to compare them with theoretical expectations. Methods. The mass profiles were obtained by using three techniques based on member galaxy kinematics, namely the caustic method, the method of dispersion-kurtosis, and MAMPOSSt. Through the inversion of the Jeans equation, it was possible to compute the velocity anisotropy profiles. Results. The mass profiles, as well as the virial values of mass and radius, computed with the different techniques agree with one another and with the estimates coming from X-ray and weak lensing studies. A combined mass profile is obtained by averaging the lensing, X-ray, and kinematics determinations. The cluster mass profile is well fitted by an NFW profile with c = 4.0 ± 0.5. The population of red and blue galaxies appear to have a different velocity anisotropy configuration, since red galaxies are almost isotropic, while blue galaxies are radially anisotropic, with a weak dependence on radius. The Q(r) profile for the red galaxy population agrees with the theoretical results found in cosmological simulations, suggesting that any bias, relative to the dark matter particles, in velocity dispersion of the red component is independent of radius. The β − γ relation for red galaxies matches the theoretical relation only in the inner region. The deviations might be due to the use of galaxies as tracers of the gravitational potential, unlike the non-collisional tracer used in the theoretical relation.

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Section: Discussionmentioning

confidence: 85%

Section: Introductionmentioning

confidence: 77%

Mass, velocity anisotropy, and pseudo phase-space density profiles of Abell 2142

Munari

Biviano

Mamon

2014

A&A

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“…Rossetti et al (2013) describe A2142 as a unique cluster with giant radio halo where the sloshing occurs at much larger scales compared to simulations and to most clusters with sloshing cold fronts, up to about 1 h −1 Mpc. X-ray studies show a complex substructure in this cluster (Okabe & Umetsu 2008;Umetsu et al 2009).…”

Section: Abell Cluster A2142mentioning

confidence: 88%

“…X-ray studies show a complex substructure in this cluster (Okabe & Umetsu 2008;Umetsu et al 2009). Rossetti et al (2013) suggest that the cluster A2142 shows indication for a merger mainly along the line of sight, which could trigger the radio emission without significantly disturbing the X-ray morphology.…”

Section: Abell Cluster A2142mentioning

confidence: 94%

Unusual A2142 supercluster with a collapsing core: distribution of light and mass

Einasto

Gramann

Saar

et al. 2015

A&A

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Context. Superclusters of galaxies can be used to test cosmological models of the formation and evolution of the largest structures in the cosmic web, and of galaxy and cluster evolution in superclusters. Aims. We study the distribution, masses, and dynamical properties of galaxy groups in the A2142 supercluster. Methods. We analyse the global luminosity density distribution in the supercluster and divide the supercluster into the high-density core and the low-density outskirts regions. We find galaxy groups and filaments in these regions, calculate their masses and mass-tolight ratios and analyse their dynamical state with 1D and 3D statistics. We use the spherical collapse model to study the dynamical state of the supercluster. Results. In the A2142 supercluster rich groups and clusters lie along an almost straight line forming the 50 h −1 Mpc long main body of the supercluster. The A2142 supercluster has a very high density core surrounded by lower-density outskirts. The total estimated mass of the supercluster is M est = 6.2 × 10 15 M . More than a half of groups with at least ten member galaxies in the supercluster lie in the high-density core of the supercluster, centred at the X-ray cluster A2142. Most of the groups in the core region are multimodal. In the outskirts of the supercluster, the number of groups is larger than in the core, and groups are poorer. The orientation of the axis of the cluster A2142 follows the orientations of its X-ray substructures and radio halo, and is aligned along the supercluster axis. The high-density core of the supercluster with the global density D8 ≥ 17 and perhaps with D8 ≥ 13 may have started to collapse. Conclusions. A2142 supercluster with collapsing core and straight body, is an unusual object among superclusters. In the course of the future evolution, the supercluster may split into several systems.

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“…Ghizzardi et al 2010), although with a few notable exceptions (e.g. A2142, Markevitch et al 2000;Rossetti et al 2013). Simulations of off-axis mergers in non-cool-core clusters (i.e.…”

Section: Discussionmentioning

confidence: 99%

Radio emission at the centre of the galaxy cluster Abell 3560: evidence for core sloshing?

Venturi

Rossetti

Bardelli

et al. 2013

A&A

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Context. We study the interplay between the radio emission associated with the dominant galaxy in clusters and the properties of the surrounding intracluster medium on the basis of its X-ray emission. Aims. Previous radio observations of the galaxy cluster A 3560, located in the Shapley Concentration core, revealed complex radio emission associated with the brightest cluster member. To understand the origin of this radio emission we performed a detailed multiwavelength study with high-quality proprietary data in the radio and X-ray bands and by means of optical data available in the literature. Methods. We observed the cluster with the Giant Metrewave Radio Telescope, the Very Large Array, and the Australia Telescope Compact array at 240 and 610 MHz, 1.28, 1.4, 2.3, 4.8, and 8.4 GHz, and performed a detailed morphological and spectral study of the radio emission associated with the brightest cluster galaxy (BCG). Furthermore, we observed the cluster with the XMM-Newton and Chandra observatories to derive the properties of the intracluster gas. Finally, we made use of literature data to obtain the bidimensional distribution of the galaxies in the cluster. Results. The radio emission, associated with the north-eastern nucleus of the dumb-bell BCG, is the result of two components: an active radio galaxy, with jets and lobes, plus aged diffuse emission, which is not refurbished with new electrons at present. Our Chandra data show that the radio active nucleus of the BCG has extended X-ray emission, which we classify as a low-luminosity corona. A residual image of the XMM-Newton brightness distribution shows a spiral-like feature, which we interpret as the signature of gas sloshing. A sub-group is clearly visible in the surface brightness residual map, and this is also supported by the XMM-Newton temperature analysis. The optical bidimensional analysis shows substructure in A 3560. A galaxy clump was detected at the location of the X-ray sub-group, and another group is present south of the cluster core, in the region where the spiral-like feature was detected. The aged part of the radio emission closely follows the spiral pattern of the X-ray residual brightness distribution, while the two active radio lobes are bent in a completely different direction. We conclude that the complex radio emission associated with the cluster BCG is the result of a minor merger event in A 3560. The aged diffuse emission is strongly affected by the sloshing motion in the intracluster gas and most likely bears information on the trajectory of the cluster BCG during the dynamical evolution of the cluster. On the other hand, the bent jets and lobes of the current radio AGN activity may reflect a complex gas velocity field in the innermost cluster regions and/or sloshing-induced oscillations in the motion of the cD galaxy.

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Abell 2142 at large scales: An extreme case for sloshing?

Cited by 102 publications

References 46 publications

Mass, velocity anisotropy, and pseudo phase-space density profiles of Abell 2142

Mass, velocity anisotropy, and pseudo phase-space density profiles of Abell 2142

Unusual A2142 supercluster with a collapsing core: distribution of light and mass

Radio emission at the centre of the galaxy cluster Abell 3560: evidence for core sloshing?

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