The dynamical status of the cluster of galaxies 1E0657-56

Barrena, R.; Biviano, A.; Ramella, M.; Falco, E.; Seitz, S.

doi:10.1051/0004-6361:20020244

Cited by 102 publications

(153 citation statements)

References 57 publications

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“…This non detection might be the result of a less favourable merger geometry, with a larger angle separating the A2163 collision axis from the sky plane. As discussed in Paper I, the galaxy velocity distribution in the main cluster indeed shows a strong velocity gradient of ∼1250 km s −1 along a NE/SW axis, which is much higher than the velocity offset of ∼600 km s −1 separating the two galaxy components of 1E 0657-56 (Barrena et al 2002).…”

Section: Discussionmentioning

confidence: 69%

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A2163: Merger events in the hottest Abell galaxy cluster

Bourdin

Arnaud

Mazzotta

et al. 2011

A&A

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Located at z = 0.203, A2163 is a rich galaxy cluster with an intra-cluster medium (ICM) that exhibits extraordinary properties, including an exceptionally high X-ray luminosity, average temperature, and a powerful and extended radio halo. The irregular and complex morphology of its gas and galaxy structure suggests that this cluster has recently undergone major merger events that involve two or more cluster components. In this paper, we study the gas structure and dynamics by means of spectral-imaging analysis of X-ray data obtained from XMM-Newton and Chandra observations. From the evidence of a cold front, we infer the westward motion of a cool core across the E-W elongated atmosphere of the main cluster A2163-A. Located close to a galaxy over-density, this gas "bullet" appears to have been spatially separated from its galaxy (and presumably dark matter component) as a result of high-velocity accretion. From gas brightness and temperature profile analysis performed in two opposite regions of the main cluster, we show that the ICM has been adiabatically compressed behind the crossing "bullet" possibly because of shock heating, leading to a strong departure of the ICM from hydrostatic equilibrium in this region. Assuming that the mass estimated from the Y X proxy best indicates the overall mass of the system and that the western cluster sector is in approximate hydrostatic equilibrium before subcluster accretion, we infer a merger scenario between two subunits of mass ratio 1:4, leading to a present total system mass of M 500 1.9 × 10 15 M . Additional analysis of the spatially-separated northern subcluster A2163-B does not show any evidence of strong interaction with the main cluster A2163-A, leading us to infer that the physical distance separating the northern subcluster and the main component is longer than the projected separation of these components. The exceptional properties of A2163 present various similarities with those of 1E0657-56, the so-called "bullet-cluster". These similarities are likely to be related to a comparable merger scenario.

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Section: Discussionmentioning

confidence: 69%

“…Comparing to the current estimates of the mass will allow us to assess which solutions are acceptable (Barrena et al 2002). We have taken R p = 1.25 Mpc and V r = 200 km s −1 (from Paper I), and set t to 10 Gyr (the age of the universe at z = 0.2).…”

Section: Discussionmentioning

confidence: 99%

A2163: Merger events in the hottest Abell galaxy cluster

Bourdin

Arnaud

Mazzotta

et al. 2011

A&A

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“…The KMM algorithm uses the maximum-likelihood ratio test to estimate how likely the two-system solution is to be a significant improvement over the single-system solution (e.g. Barrena, Biviano & Ramella 2002).…”

Section: Subclusteringmentioning

confidence: 99%

Dynamical analysis of the cluster pair: A3407 + A3408

Nascimento

Ribeiro

Trevisan

et al. 2016

Mon. Not. R. Astron. Soc.

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We carried out a dynamical study of the galaxy cluster pair A3407 & A3408 based on a spectroscopic survey obtained with the 4 meter Blanco telescope at the CTIO, plus 6dF data, and ROSAT All-Sky-Survey. The sample consists of 122 member galaxies brighter than m R = 20. Our main goal is to probe the galaxy dynamics in this field and verify if the sample constitutes a single galaxy system or corresponds to an ongoing merging process. Statistical tests were applied to clusters members showing that both the composite system A3407 + A3408 as well as each individual cluster have Gaussian velocity distribution. A velocity gradient of ∼ 847 ± 114 km s −1 was identified around the principal axis of the projected distribution of galaxies, indicating that the global field may be rotating. Applying the KMM algorithm to the distribution of galaxies we found that the solution with two clusters is better than the single unit solution at the 99% c.l. This is consistent with the X-ray distribution around this field, which shows no common X-ray halo involving A3407 and A3408. We also estimated virial masses and applied a two-body model to probe the dynamics of the pair. The more likely scenario is that in which the pair is gravitationally bound and probably experiences a collapse phase, with the cluster cores crossing in less than ∼1 h −1 Gyr, a pre-merger scenario. The complex X-ray morphology, the gas temperature, and some signs of galaxy evolution in A3408 suggests a post-merger scenario, with cores having crossed each other ∼ 1.65h −1 Gyr ago, as an alternative solution.

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“…This property has recently boosted an entire research field of cluster surveys with the SZ effect (Carlstrom et al 2002). In fact, "flux-limited" SZ cluster surveys are almost mass-limited cluster surveys (Bartlett 2006). This property is extremely relevant, because the mass of clusters is a sensible cosmological probe, as we explain below.…”

Section: Clusters As Probes For Cosmologymentioning

confidence: 94%

“…The cluster 1ES 0657-55.8, dubbed "the bullet cluster" (Markevitch et al 2002;Barrena et al 2002), is a spectacular example of a merging cluster at intermediate redshift (z = 0.296). At low redshifts, there are many other examples of merging clusters or galaxy groups falling onto clusters along filamentary structure.…”

Section: Substructure Mass Accretion and Non-thermal Phenomenamentioning

confidence: 99%

Clusters of Galaxies: Setting the Stage

2008

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Clusters of galaxies are self-gravitating systems of mass ∼ 10 14 -10 15 h −1 M and size ∼ 1-3h −1 Mpc. Their mass budget consists of dark matter (∼ 80%, on average), hot diffuse intracluster plasma ( 20%) and a small fraction of stars, dust, and cold gas, mostly locked in galaxies. In most clusters, scaling relations between their properties, like mass, galaxy velocity dispersion, X-ray luminosity and temperature, testify that the cluster components are in approximate dynamical equilibrium within the cluster gravitational potential well. However, spatially inhomogeneous thermal and non-thermal emission of the intracluster medium (ICM), observed in some clusters in the X-ray and radio bands, and the kinematic and morphological segregation of galaxies are a signature of non-gravitational processes, ongoing cluster merging and interactions. Both the fraction of clusters with these features, and the correlation between the dynamical and morphological properties of irregular clusters and the surrounding large-scale structure increase with redshift.In the current bottom-up scenario for the formation of cosmic structure, where tiny fluctuations of the otherwise homogeneous primordial density field are amplified by gravity, clusters are the most massive nodes of the filamentary large-scale structure of the cosmic web and form by anisotropic and episodic accretion of mass, in agreement with most of the observational evidence. In this model of the universe dominated by cold dark matter, at the present time most baryons are expected to be in a diffuse component rather than in stars and A. Diaferio ( ) Dipartimento

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The dynamical status of the cluster of galaxies 1E0657-56

Cited by 102 publications

References 57 publications

A2163: Merger events in the hottest Abell galaxy cluster

A2163: Merger events in the hottest Abell galaxy cluster

Dynamical analysis of the cluster pair: A3407 + A3408

Clusters of Galaxies: Setting the Stage

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