A Powerful Radio Halo in the Hottest Known Cluster of Galaxies 1E 0657–56

By Haida Liang, R. Hunstead, M. Birkinshaw, P. Andreani. 2000

170 citations recorded by the source corpus.

We report the detection of a diffuse radio halo source in the hottest known cluster of galaxies 1E 0657-56 (RX J0658-5557). The radio halo has a morphology similar to the X-ray emission from the hot intracluster medium. The presence of a luminous radio halo in such a hot cluster is further evidence for a steep correlation between the radio halo power and the X-ray temperature. We favor models for the origin of radio halo sources involving a direct connection between the X-ray emitting thermal particles and the radio emitting relativistic particles.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/70bec6aa726366bf3bf4e88fde81c6ea0cb24bb3

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Citations in the corpus

A Textbook Example of a Bow Shock in the Merging Galaxy Cluster 1E 0657–56 (2001, background): “FromASCA data, Tucker et al. (1998, hereafter T98) derived a temperature around 17 keV, making this system one of the hottest known (see also Yaqoob 1999; Liang et al. 2000, hereafter LHBA).”
Cluster Mergers and Non-Thermal Phenomena: A Statistical Magneto-Turbulent Model (2004, background): “In addition correlations between the radio power of radio haloes at 1.4 GHz and the bolometric X-ray luminosity, temperature and mass of the parent clusters have been found (Colafrancesco 1999; Liang et al. 2000; Govoni et al. 2001; Giovannini & Feretti 2002).”
On the Origin of Radio Halos in Galaxy Clusters (2001, background): “However, it has been argued (e.g., Giovannini & Feretti 2000; Liang et al. 2000; Feretti 2000) that merging cannot be solely responsible for the formation of radio halos because at least 50% of clusters show evidence for X-ray substructure (Jones & Forman 1999) whereas only ∼ 10% 1 2 possess radio…”
NuSTAR OBSERVATIONS OF THE BULLET CLUSTER: CONSTRAINTS ON INVERSE COMPTON EMISSION (2014, methodology): “The average temperature of the global spectrum is 14.2±0.3 keV, in good agreement with estimates from ROSAT+ASCA (14.5 keV, Liang et al. 2000) and Chandra (14.8 keV, Markevitch et al. 2002), but somewhat higher than independent estimates from XMM-Newton and RXTE (∼ 12 keV, Petrosian et al. 2006).”
Cosmic-Ray Electrons in Groups and Clusters of Galaxies: Primary and Secondary Populations from a Numerical Cosmological Simulation (2001, background): “With this in mind, we note that in all the presented cases the mean predicted total power at 1.4 GHz is consistent with the observed values for a conservative estimate of of 10~2 to 10~3.”
Diffuse Radio Emission from Galaxy Clusters (2019, background): “3+4220 0.292 H Wilber et al. (2018a) Bullet clusterl 0.296 H, RS Liang et al. (2000); Shimwell et al. (2014, 2015) Abell 781 0.298 cRS/cF non-confirmed H Venturi et al. (2008); Rudnick & Lemmerman (2009) Govoni et al. (2011); Venturi et al. (2011, 2013) Botteon et al. (2018b) PSZ1 G096.”
A comparison of radio and X-ray morphologies of four clusters of galaxies containing radio halos (2001, methodology): “So far, the similarity of the radio halo and the X-ray morphology of the clusters has been pointed out in the literature (Deiss et al. 1997, Feretti 1999, Liang et al. 2000) but it has never been used to constrain theoretical models.”
Cosmic ray transport in galaxy clusters: implications for radio halos, gamma-ray signatures, and cool core heating (2010, background): “The radio luminosity of giant halos seems to be strongly correlated with the X-ray emissivity of the cluster (Liang et al. 2000; Brunetti et al. 2009, and see Fig.”
Cluster Magnetic Fields (2001, background): “…a natural explanation for the observed correlation between cluster radio halos and substructure in cluster atmospheres (Govoni et al. 2001a), and between cluster radio luminosity and cluster atmosphere temperature, assuming that the gas temperature increases during a merger (Liang et al. 2000).”
GMRT radio halo survey in galaxy clusters at z = 0.2–0.4 - II. The eBCS clusters and analysis of the complete sample (2008, methodology): “4 GHz – logLX correlation shown in a number of papers (e.g. Liang et al. 2000; CBS06) and scaled assuming α1.”
Radio and X-ray diffuse emission in six clusters of galaxies (2001, background): “…Markevitch et al. 1998) and the cluster mass (e.g., Reiprich & Böhringer 1999) are related to the X-ray luminosity, a relation is expected also between the monochromatic radio power and the cluster temperature (Liang et al. 2000) and between the monochromatic radio power and the cluster mass.”
Determining the Cosmic Distance Scale from Interferometric Measurements of the Sunyaev-Zeldovich Effect (2002, background): “Shocks from cluster mergers may be the acceleration mechanism though there are numerous theories (e.g., Jaffe 1977, 1980; Dennison 1980; Roland 1981; Schlickeiser et al. 1987; Ensslin et al. 1998; Blasi & Colafrancesco 1999; Dolag & Ensslin 2000; Liang et al. 2000).”
Bow Shock and Radio Halo in the Merging Cluster A520 (2004, background): “Both A520 and 1E 0657 56 have radio halos (Govoni et al. 2001; Liang et al. 2000).”
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.”
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): “Prominent examples for “radio hal” emission can be obtained from Giovannini et al. (1999) and include the Coma cluster (Kim et al. 1989; Deiss et al. 1997) and the galaxy cluster 1E 0657-56 (Liang et al. 2000).”