1.6 The thesis: aims and methods
1.6.1 Previous studies on the analyzed clusters
The two clusters studies through this work have been already known since the cata- logues of Abell (((1958); (1965); (1989)) and are both part of their southern exten- sions. As very massive clusters, their properties have been already partly investigated in the past, although always limited to the cluster central regions (the inner Mpc). Our results extend and complete the available knowledge to larger distances. For comparison in the following chapters, here the main past results will be summarised for RXCJ0014.3-3022 and RXCJ2308.3-0211.
1.6.1.1 RXCJ0014.3-3022
This cluster (A 2744 or AC118) has been subject of several optical studies, being a BO cluster. In an early study of four such clusters, including RXCJ0014.3-3022, Poggianti et al. ((1996)) analysed spectral lines and broad-band colours by means of an evolutionary synthesis model. They concluded that a substantial fraction of cluster galaxies is undergoing short but vigorous starburst episodes, which affect a substantial galactic mass fractions, typically 30% or more. Later on, HST-WFPC2 observations at 0.3′′-spatial resolution and ground-based multi-object spectroscopy (MOS) in a central square region of about 1 Mpc on the side (Couch et al. (1998)) revealed a link between starburst activity and galaxy-galaxy interactions in three “Butcher-Oemler” clusters at z ∼ 0.3, including RXCJ0014.3-3022. These authors concluded that the evolution of the overall cluster galaxy population is driven by several different physical processes. Colour-magnitude relation and luminosity func- tion in the optical and near-infrared were successively determined by Busarello et al. ((2002)), Andreon ((2002)), and Merluzzi et al. ((2003)).
The latter studies targeted an almost four time wider region, which allowed the first evidence of substructure in the galaxy distribution in the central region of RXCJ0014.3-3022 to be covered. X-ray observations withChandra led to the discov- ery of a shock discontinuity due to a major merger occurring at Mach number of∼
1.2 (Kempner & David (2004)). These authors suggested that the ongoing merging could be pumping energy into the central radio halo of the cluster (Giovannini et
al. (1999); Govoni et al. (2001)). In a recent analysis of the central radio halo and peripheral radio relic of RXCJ0014.3-3022, conducted with the VLA at 350 MHz and 1.4 GHz, Orr´u et al. ((2007)) discovered that the flat spectrum regions of the radio halo are correlated with higher temperature in X-rays. This result supports the idea that a fraction of the gravitational energy, which is dissipated during mergers in heating the thermal plasma, is converted into re-acceleration of relativistic particles and amplification of the magnetic field. Indeed, the dynamical analysis of Boschin et al. ((2006)) confirmed the presence of substructure in the cluster central region, where two subcomponents with a mass ratio of 3:1 approach each other at a velocity along the line of sight in excess of 3000 km s−1.
Recently we have extended the knowledge on the substructure and galaxy popula- tions of the cluster beyond the cluster virial radius, which measures about 2.5 Mpc (Zhang et al. (2006)). In particular, deep XMM-Newton observations allowed to produce 2D maps of the entropy of the X-ray emitting gas at high signal-to-noise ra- tio (S/N), which revealed not only the shock region discovered byChandra but also the presence of a low-entropy channel pointing outwards from the cluster core to- wards the South (B¨ohringer et al. (2006)). Finally, B¨ohringer et al. ((2006)) showed that the merging nature of the cluster induces a displacement of the distributions of galaxies and ICM for both subcomponents (similar to the famous “Bullet Cluster” in Clowe et al. (2006)).
1.6.1.2 RXCJ2308.3-0211
Fewer studies have been performed on this cluster (A 2537). This can be due to its position close to the galactic plane, where absorption is very large. Moreover, although it is a massive cluster, it is dimmer than RXCJ0014.3-3022.
Dahle et al. ((2002)) performed lensing analysis over a sample of clusters, including RXCJ2308.3-0211. The results of their shear analysis show that the cluster has a mass distribution partly different from the galaxy distribution, being elongated on the N– S axis, but the peaks of the two are well in accord. They also derive a mass value slightly below 1015M⊙. Similarly,Chandraobservations by Schmidt & Allen ((2007)) show an x-ray derived mass of about 8×1014M⊙, although with very large upper
errorbars, suggesting an even larger mass. Both values are in agreement with the X-ray determination of Znahg et al. ((2006)), where a mass of (7.4±1.8)×1014M⊙ is found within R500. Venturi et al. ((2007)) covered this cluster with GMT radio
observations, not finding any clue of extended radio features. Only the cD shows a short radio tail.
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