Giant Ringlike Radio Structures Around Galaxy Cluster Abell 3376

Bagchi, J.; Durret, F.; Neto, G. B. Lima; Paul, Surajit

doi:10.1126/science.1131189

Cited by 173 publications

(225 citation statements)

References 27 publications

(20 reference statements)

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“…They reveal many new details in the relic and show that the relic has a significant amount of filamentary structure on scales down to ∼30kpc. Small-scale filamentary structures have also been seen for other relics, such as the Toothbrush cluster (van Weeren et al , 2016a, A3667 (Röttgering et al 1997), A3376 (Bagchi et al 2006), and in particular for Abell2256 (Clarke & Enßlin 2006;van Weeren et al 2009a;Owen et al 2014).…”

Section: Continuum Imagesmentioning

confidence: 84%

Chandra and JVLA Observations of HST Frontier Fields Cluster MACS J0717.5+3745

Weeren

Ogrean

Jones

et al. 2017

ApJ

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To investigate the relationship between thermal and non-thermal components in merger galaxy clusters, we present deep JVLA and Chandraobservations of the HST Frontier Fields cluster MACSJ0717.5+3745. The Chandraimage shows a complex merger event, with at least four components belonging to different merging subclusters. Northwestof the cluster, ∼0.7 Mpc from the center, there is a ram-pressure-stripped core that appears to have traversed the densest parts of the cluster after entering the intracluster medium (ICM) from the direction of a galaxy filament to the southeast. We detect a density discontinuity north-northeastof this core, which we speculate is associated with a cold front. Our radio images reveal new details for the complex radio relic and radio halo in this cluster. In addition, we discover several new filamentary radio sources with sizes of 100-300kpc. A few of these seem to be connected to the main radio relic, while others are either embedded within the radio halo or projected onto it. A narrow-angled-tailed (NAT) radio galaxy, a cluster member, is located at the center of the radio relic. The steep spectrum tails of this active galactic nucleuslead into the large radio relic where the radio spectrum flattens again. This morphological connection between the NAT radio galaxy and relic provides evidence for reacceleration (revival) of fossil electrons. The presence of hot 20 keV ICM gas detected by Chandranear the relic location provides additional support for this re-acceleration scenario.

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Section: Continuum Imagesmentioning

confidence: 84%

Chandra and JVLA Observations of HST Frontier Fields Cluster MACS J0717.5+3745

Weeren

Ogrean

Jones

et al. 2017

ApJ

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“…8 E.g. A3667 and A3376: Schilizzi & McAdam (1975); Goss et al (1982); Jones & McAdam (1992); Röttgering et al (1997); Bagchi et al (2006). 9 Radio gischt in the taxonomy of Kempner et al (2004Roettiger et al (1999a); Kassim et al (2001); Miniati et al (2001a); Bagchi et al (2002); Berrington & Dermer (2003); Hoeft et al (2004Hoeft et al ( , 2008Siemieniec-Ozieblo (2004); Keshet et al (2004); Hoeft & Brüggen (2007); Giacintucci et al (2008); Battaglia et al (2009).…”

Section: Observational Propertiesmentioning

confidence: 99%

Cosmic ray transport in galaxy clusters: implications for radio halos, gamma-ray signatures, and cool core heating

Enßlin

Pfrommer

Miniati

et al. 2011

A&A

199

294

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We investigate the interplay of cosmic ray (CR) propagation and advection in galaxy clusters. Propagation in form of CR diffusion and streaming tends to drive the CR radial profiles towards being flat, with equal CR number density everywhere. Advection of CR by the turbulent gas motions tends to produce centrally enhanced profiles. We assume that the CR streaming velocity is of the order of the sound velocity. This is motivated by plasma physical arguments. The CR streaming is then usually larger than typical advection velocities and becomes comparable or lower than this only for periods with trans-and super-sonic cluster turbulence. As a consequence a bimodality of the CR spatial distribution results. Strongly turbulent, merging clusters should have a more centrally concentrated CR energy density profile with respect to relaxed ones with very subsonic turbulence. This translates into a bimodality of the expected diffuse radio and gamma-ray emission of clusters, since more centrally concentrated CR will find higher target densities for hadronic CR proton interactions, higher plasma wave energy densities for CR electron and proton re-acceleration, and stronger magnetic fields. Thus, the observed bimodality of cluster radio halos appears to be a natural consequence of the interplay of CR transport processes, independent of the model of radio halo formation, be it hadronic interactions of CR protons or re-acceleration of low-energy CR electrons. Energy dependence of the CR propagation should lead to spectral steepening of dying radio halos. Furthermore, we show that the interplay of CR diffusion with advection implies first order CR re-acceleration in the pressure-stratified atmospheres of galaxy clusters. Finally, we argue that CR streaming could be important in turbulent cool cores of galaxy clusters since it heats preferentially the central gas with highest cooling rate.

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“…Particularly interesting are the so-called double-relics, where two relics are diametrically located on both sides of the cluster center (e.g., Bonafede et al 2009;van Weeren et al 2009;Bagchi et al 2006;van Weeren et al 2010;Brown et al 2011;van Weeren et al 2011). These relics are thought to trace outward moving shock waves from a binary cluster merger event, which develop after core passage of the two subclusters.…”

Section: Introductionmentioning

confidence: 99%

Relics as Probes of Galaxy Cluster Mergers

et al. 2011

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Abstract. Galaxy clusters grow by mergers with other clusters and galaxy groups. These mergers create shocks within the intracluster medium (ICM). It is proposed that within the shocks particles can be accelerated to extreme energies. In the presence of a magnetic field these particles should then form large regions emitting synchrotron radiation, creating so-called radio relics. An example of a cluster with relics is CIZA J2242.8+5301. Here we present hydrodynamical simulations of idealized binary cluster collisions with the aim of constraining the merger scenario for this cluster. We conclude that by using the location, size and width of double radio relics we can set constraints on the mass ratios, impact parameters, timescales, and viewing geometries of binary cluster merger events.

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Giant Ringlike Radio Structures Around Galaxy Cluster Abell 3376

Cited by 173 publications

References 27 publications

Chandra and JVLA Observations of HST Frontier Fields Cluster MACS J0717.5+3745

Chandra and JVLA Observations of HST Frontier Fields Cluster MACS J0717.5+3745

Cosmic ray transport in galaxy clusters: implications for radio halos, gamma-ray signatures, and cool core heating

Relics as Probes of Galaxy Cluster Mergers

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