SC 1327–312 &amp; SC 1329–313: Two galaxy groups in-between a major merging event observed with Beppo–SAX

Bardelli, S.; Grandi, S. De; Ettori, S.; Molendi, S.; Zucca, E.; Colafrancesco, S.

doi:10.1051/0004-6361:20011665

Cited by 14 publications

(22 citation statements)

References 35 publications

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“…Note that the SC 1329 group has a bimodal velocity distribution: the optical clumps associated to the two velocity peaks are named T520 and T496 (Bardelli et al 1998a). a Bardelli et al (1998b), b Bardelli et al (1998a), c Bardelli et al (2002), d Ettori et al (2000). resembles the results of the numerical simulations carried out by Roettiger et al (1997) for the case of a collision of two clusters.…”

Section: The Cluster Merger In A3558-csupporting

confidence: 55%

AGN and starburst radio activity in the A3558 cluster complex

Giacintucci

Venturi

Bardelli

et al. 2004

A&A

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Abstract. We present Very Large Array (VLA) 1.4 GHz (21 cm) observations of the region between the centres of A3558 and A3562, in the major cluster merger complex of the Shapley Concentration. Our final catalogue includes a total of 174 radio sources above the flux density limit of 0.25 mJy b −1 . By cross-correlation with optical and spectroscopic catalogues we found 33 optical counterparts belonging to the Shapley Concentration. We investigated the effects of cluster merger on the radio emission properties of the galaxy population by means of the radio source counts and the radio luminosity functions (RLF). We found that the radio source counts are consistent with the field source counts. The RLF of elliptical and S0 galaxies in the region surveyed, is consistent with the "universal" RLF for early-type galaxies. This result suggests that the deficit in radio galaxies found in our previous work over the whole A3558 chain is entirely due to the cluster A3558. A population of faint radio galaxies (log P 1.4 GHz (W Hz −1 ) < ∼ 22) is also found. Half of these objects are also blue, suggesting that starburst is the main mechanism driving the radio emission. Finally, we detected 14 spiral radio galaxies, whose ratio between radio and optical emission is similar to those found in galaxies located in rich and dynamically evolved clusters. Our results are briefly discussed in the light of the age and stage of the merger in the A3558 cluster complex.

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Section: The Cluster Merger In A3558-csupporting

confidence: 55%

AGN and starburst radio activity in the A3558 cluster complex

Giacintucci

Venturi

Bardelli

et al. 2004

A&A

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“…The size of the relic in our image is ∼ 350 kpc, which is small but not unusual. Its radio power is low (P 325 MHz = 3 × 10 23 W Hz −1 ), and it is at least qualitatively consistent with the scaling relation between the radio power of relics and the mass of the host cluster (see de Gasperin et al [18]), considering that the mass estimated for SC 1329-313 from Beppo-SAX observations is approximately ∼ 3.5 × 10 14 M Sun (Bardelli et al [47]). The relic is overlaid on the XMM-Newton X-ray image in Figure 4, which clearly shows the location between the two SC groups.…”

Section: The Relicsupporting

confidence: 67%

Extended Radio Emission in the Perhipheral Regions of the Shapley Concentration Core

et al. 2017

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Abstract:The Shapley Concentration (SC) is a galaxy supercluster (few tens of degrees) in the Local Universe (∼0.048) which is currently undergoing cluster mergers and group accretion. It is a diversified environment, with cluster complexes in advanced evolutionary stage, groups of clusters in the very early stages of merger, fairly massive clusters with ongoing accretion activity, and smaller groups located in filaments. These features make the SC an ideal place to observe the signatures of the formation of large-scale structures in the Universe. As a matter of fact, the SC has been observed over a broad range of frequencies with the most important observatories, allowing for a unique multiband study. In this paper, we will present new results from an ongoing study of the Shapley Concentration Core, which is being carried out with the Giant Metrewave Radio Telescope (GMRT). Our work confirms the role played by radio observations in disentangling the details of the accretion and merging processes, and delivers a wealth of information in regions well outside the cluster cores. In particular, we will report on the discovery of a relic in the region between the two clusters A 3558 and A 3562, and of the radio properties of the brightest galaxy in the peripheral cluster A 3556.Keywords: Galaxy clusters; Shapley Concentration; radio sources Cluster Mergers and Diffuse Radio EmissionAccording to the hierarchical scenario, cluster mergers-the most energetic events in the Universe, with a total energy output of the order of 10 63 -10 64 erg-are the natural way to account for mass assembly: galaxy clusters form as a consequence of merger trees, to reach and exceed masses on the order of 10 15 M Sun . Cluster mergers deeply affect the dynamics of the galaxies, as well as the properties of the thermal intracluster medium and those of relativistic particles and magnetic field.The close connection between the properties of the radio emission in galaxy clusters and their dynamical state is now an established result. Giant radio halos and relics-Mpc-scale steep spectrum synchrotron radio sources (see Feretti et al. [1] for a recent observational overview)-are thought to be the result of particle re-acceleration due to turbulence and shocks, respectively, induced in the cluster volume during mergers and accretion processes (see Brunetti and Jones [2] for a recent theoretical review). While the details of the microphysics of these processes are still a matter of

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“…The presence of a radio halo in this cluster (Giacintucci et al 2005) indicates a merger activity, since radio halos have only been found in interacting systems. Evidence of interaction also comes from Beppo-SAX data (Bardelli et al 2002). Using XMM-Newton data, Finoguenov et al (2004) suggest that the SC 1329-313 group southwest of A3562 has passed to the north of A3562, and the cluster core is likely oscillating in response to the passage of the group.…”

Section: Merger Cold Frontsmentioning

confidence: 99%

Cold fronts in galaxy clusters

Ghizzardi¹,

Rossetti²,

Molendi³

2010

A&A

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127

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Context. Cold fronts have been observed in several galaxy clusters. Understanding their nature and origin is extremely important for investigating the internal dynamics of clusters. Aims. To gain insight into the nature of these features, we carry out a statistical investigation of their occurrence in a sample of galaxy clusters observed with XMM-Newton and correlate this occurrence with different cluster properties. Methods. We selected a sample of 45 clusters starting from the B55 flux limited sample (Edge et al. 1990, MNRAS, 245, 559) and performed a systematic search for cold fronts. Results. We find that a large fraction of clusters host at least one cold front. Cold fronts are easily detected in all systems that are manifestly undergoing a merger event in the plane of the sky, while the presence of these features in the remaining clusters is related to a steep entropy gradient, in agreement with theoretical expectations. Assuming that cold fronts in cool core clusters are triggered by minor merger events, we estimate a minimum of 1/3 merging events per halo per Gyr.

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SC 1327–312 & SC 1329–313: Two galaxy groups in-between a major merging event observed with Beppo–SAX

Cited by 14 publications

References 35 publications

AGN and starburst radio activity in the A3558 cluster complex

AGN and starburst radio activity in the A3558 cluster complex

Extended Radio Emission in the Perhipheral Regions of the Shapley Concentration Core

Cold fronts in galaxy clusters

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