A comparison of radio and X-ray morphologies of four clusters of galaxies containing radio halos

By F. Govoni, Torsten A. Ensslin, L. Feretti, G. Giovannini. 2001

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Clusters of galaxies may contain cluster-wide, centrally located, diuse radio sources, called halos. They have been found to show morphologies similar to those of the X-ray emission. To quantify this qualitative statement we performed a point-to-point comparison of the radio and the X-ray emission for four clusters of galaxies containing radio halos: Coma, Abell 2255, Abell 2319, Abell 2744. Our study leads to a linear relation between the radio and the X-ray surface brightness in two clusters, namely Abell 2255 and Abell 2744. In Coma and A2319 the radio and the X-ray brightnesses seem to be related with a sub-linear power law. Implications of these ndings within simple radio halo formation models are briefly discussed.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/396a2d92ea71fc05b8490e4fca2e45c34316f15d

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Citations in the corpus

Acceleration of primary and secondary particles in galaxy clusters by compressible MHD turbulence: from radio haloes to gamma-rays (2010, background): “…(i) is motivated by the fact that, similarly to other giant halos, the Coma radio halo has a very broad synchrotron–brightness distribution (Govoni et al 2001; see also discussion in Cassano et al 2007 and Donnert et al 2010a) implying a very broad spatial distribution of relativistic…”
Diffuse Optical Light in Galaxy Clusters. II. Correlations with Cluster Properties (2007, background): “The presence of a large radio halo and radio relic are yet more evidence for dynamical activity in this cluster (Govoni et al. 2001).”
ON THE CONNECTION BETWEEN GIANT RADIO HALOS AND CLUSTER MERGERS (2010, background): “Indeed, studies showed a point-to-point correlation between the radio and X-ray brightness (e.g., Govoni et al. 2001) and between the RH properties and cluster properties (mass, velocity dispersion) calculated within the halo region (Cassano et al. 2007).”
Radio signature of cosmological structure formation shocks (2006, background): “We analysed the relics in A115, A 2256, and A3667 and found that the shocks have Mach numbers in the range of 3 to 5.”
Constraining the population of cosmic ray protons in cooling flow clusters with γ-ray and radio observations: Are radio mini-halos of hadronic origin? (2003, unknown): “Pursuing an approach of averaging only along the line of sight could attenuate the bias (Govoni et al. 2001).”
Radio and X-ray diffuse emission in six clusters of galaxies (2001, methodology): “As already noted in Govoni et al. (2001), in A2744 we found a perfect similarity of the two profiles.”
A Textbook Example of a Bow Shock in the Merging Galaxy Cluster 1E 0657–56 (2001, background): “A spatial correlation between the halo brightness and the local gas temperature (in addition to the general similarity to the X-ray brightness, e.g., LHBA; Govoni et al. 2001) was noticed by MV in two other merging clusters and supports the merger shock origin for the relativistic halo electrons(e.g”
Simulating cosmic rays in clusters of galaxies – II. A unified scheme for radio haloes and relics with predictions of the γ-ray emission (2007, background): “Our correlations are strikingly similarto the ones found in observed radio halos (cf. Govoni et al. 2001).”
Cosmic ray transport in galaxy clusters: implications for radio halos, gamma-ray signatures, and cool core heating (2010, background): “(However, Govoni et al. 2001a, find that the naively expected radio halo profile does not seem to fit the observed asymptotic in case of weak magnetic fields (B < 3 μG).)”
Four Extreme Relic Radio Sources in Clusters of Galaxies (2001, background): “In the clusters Coma (Enßlin et al. 1998), A1300 (Reid et al. 1999), A2255 (Feretti et al. 1997), A2744 (Govoni et al. 2001) and possibly in the cluster 1E 0657−56 (Liang et al. 2000), both a halo and a relic have been found.”
Foreground simulations for the LOFAR-epoch of reionization experiment (2008, background): “The distribution of the radio haloes seems to follow closely the large-scale distribution of the free–free driven X-ray emission of clusters (Govoni et al. 2001).”
On the Origin of Radio Halos in Galaxy Clusters (2001, background): “First, Govoni et al. (2001) have compared the point-to-point spatial distribution of the radio and X-ray emission in four clusters and have found a linear relationship in two cases and a nearly linear relationship in the other two.”
On the formation of cluster radio relics (2001, background): “Cluster radio haloes have steep radio spectra (spectral index a < 1–1:5Þ; they are unpolarized, and their diffuse morphologies are often similar to those of the thermal X-ray emission of the cluster gas (Govoni et al. 2001).”
Diffuse Radio Emission from Galaxy Clusters (2019, background): “…al. (2014) SPT-CL J0245-5302 0.300 cdRS Zheng et al. (2018) Abell 2552 0.305 cH Kale et al. (2015) Abell 2744 0.308 H, mRS Giovannini et al. (1999); Govoni et al. (2001b) Bacchi et al. (2003); Orrú et al. (2007) Venturi et al. (2013); Pearce et al. (2017) George et al. (2017); Duchesne et al.…”