The Seeding of Cosmic Ray Electrons by Cluster Radio Galaxies: A Review

Vazza, Franco; Botteon, Andrea

doi:10.3390/galaxies12020019

Galaxies

2024

DOI: 10.3390/galaxies12020019

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The Seeding of Cosmic Ray Electrons by Cluster Radio Galaxies: A Review

Franco Vazza,

Andrea Botteon

Abstract: Radio galaxies in clusters of galaxies are a prominent reservoir of magnetic fields and of non-thermal particles, which become mixed with the intracluster medium. We review the observational and theoretical knowledge of the role of these crucial ingredients for the formation of diffuse radio emission in clusters (radio halos, relics, mini halos) and outline the open questions in this field.

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Cited by 5 publications

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Ageing and dynamics of the tailed radio galaxies in Abell 2142

Bruno,

Venturi,

Dallacasa

et al. 2024

A&A

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Context. Tailed radio galaxies are shaped by ram pressure that is due to the high-velocity motion of their host through the intracluster medium (ICM). Recent works have reported on the increasing complexity of the phenomenology of tailed galaxies, with departures from theoretical ageing models and novel evidence of re-energising mechanisms that are nonetheless unclear. Aims. The nearby (z = 0.0894) galaxy cluster Abell 2142 hosts two tailed galaxies, namely T1 and T2, which exhibit peculiar morphological features. We aim to investigate the properties of T1 and T2 and constrain their spectral evolution, dynamics, and interactions with the ICM. Methods. We combined data from LOw Frequency Array (LOFAR), upgraded Giant Metrewave Radio Telescope (uGMRT), Very Large Array (VLA), and MeerKAT (from 30 MHz to 6.5 GHz) to carry out a detailed spectral analysis of T1 and T2. We analysed the surface brightness profiles, measured integrated and spatially resolved spectral indices. We performed a comparison with single injection ageing models. The Chandra X-ray data were used to search for discontinuities in the ICM properties in the direction of the targets. Results. The spectral properties of T1 at low frequencies can be predicted by ageing models and provide constraints on the 3D dynamics of the host by assuming a constant velocity. However, a more complex scenario is suggested by the sharp transitions along sub-regions of the tail, local surface brightness enhancements, and a spectral shape at high frequencies that is not predicted by any of the models. This scenario may plausibly involve hydrodynamical instabilities and particle mixing. T2 exhibits unusual morphological and surface brightness features, and its spectral behaviour is not predicted by standard models. The effects of two active galactic nucleus (AGN) outburst events during the infall of T2 towards the cluster centre could potentially explain its characteristic properties.

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Ageing and dynamics of the tailed radio galaxies in Abell 2142

Bruno,

Venturi,

Dallacasa

et al. 2024

A&A

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LOFAR high-band antenna observations of the Perseus cluster

van Weeren,

Timmerman,

Vaidya

et al. 2024

A&A

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The Perseus cluster is the brightest X-ray cluster in the sky and is known as a cool-core galaxy cluster. Being a very nearby cluster, it has been extensively studied. This has provided a comprehensive view of the physical processes that operate in the intracluster medium (ICM), including feedback from the active galactic nucleus (AGN) 3C\,84 and measurements of ICM turbulence. Additionally, the Perseus cluster contains a central radio mini-halo. This diffuse radio source traces cosmic-ray electrons (re-)accelerated in situ in the ICM. Here, we report on LOFAR high-band antenna 120--168\,MHz observations of the Perseus cluster that probe a range of four orders of magnitude in angular scales. In our 0.3 (0.11\,kpc) resolution image, we find that the northern extension of the 3C\,84 lobe consists of several narrow 1.5--3\,kpc parallel strands of emission. In addition, we detect steep-spectrum filaments associated with a previous outburst of the central AGN radio emission filling two known X-ray ``ghost'' cavities. At 7 resolution (2.6\,kpc), our images show a complex structured radio mini-halo, with several edges and filaments. At resolutions of 26 (10\,kpc) and 80 (29\,kpc), we discover diffuse radio emission with a 1.1\,Mpc extent. We classify this emission as a giant radio halo, and its properties are distinct from the inner mini-halo. We also detect two diffuse sources at projected cluster centric radii of 0.7 and 1.0\,Mpc. Finally, we observe a 0.9\,Mpc trail of radio emission from the cluster member galaxy IC\,310 that connects it to the giant radio halo. Together with other recent studies of relaxed clusters, our LOFAR observations indicate that cluster-wide radio emission could be (more) common in cool-core clusters. In the case of the Perseus cluster, a past off-axis merger event that preserved the cool core might have generated enough turbulence to produce an extended radio halo observable at low frequencies.

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ASKAP reveals the radio tail structure of the Corkscrew Galaxy shaped by its passage through the Abell 3627 cluster

Koribalski,

Duchesne,

Lenc

et al. 2024

Monthly Notices of the Royal Astronomical Society

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Among the bent tail radio galaxies common in galaxy clusters are some with long, collimated tails (so-called head-tail galaxies) shaped by their interactions with the intracluster medium (ICM). Here we report the discovery of intricate filamentary structure in and beyond the ∼28′ (570 kpc) long, helical radio tail of the Corkscrew Galaxy (1610–60.5, ESO 137-G007), which resides in the X-ray bright cluster Abell 3627 (D = 70 Mpc). Deep radio continuum data were obtained with wide-field Phased Array Feeds on the Australian Square Kilometer Array Pathfinder (ASKAP) at 944 MHz and 1.4 GHz. While the bright (young) part of the Corkscrew Galaxy tail is highly collimated, the faint (old) part shows increasing oscillation amplitudes, break-ups, and filaments. We find a stunning set of arc-shaped radio filaments beyond and mostly orthogonal to the collimated Corkscrew tail end, forming a partial bubble. This may be the first detection of a ”proto-lobe” previously seen in 3D MHD simulations, formed by the face-on impact of the Corkscrew Galaxy with a shock front in the cluster outskirts. Interactions of the radio galaxy tail with the ICM are likely responsible for the tail collimation and shear forces within the ICM for its increasingly filamentary structure. We also report the discovery of small (∼20–30 kpc) ram-pressure stripped radio tails in four Abell 3627 cluster galaxies, located between the Corkscrew Galaxy and its prominent neighbour, the wide-angle tail (WAT) radio galaxy 1610–60.8 (ESO 137-G006).

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The Seeding of Cosmic Ray Electrons by Cluster Radio Galaxies: A Review

Cited by 5 publications

References 139 publications

Ageing and dynamics of the tailed radio galaxies in Abell 2142

Ageing and dynamics of the tailed radio galaxies in Abell 2142

LOFAR high-band antenna observations of the Perseus cluster

ASKAP reveals the radio tail structure of the Corkscrew Galaxy shaped by its passage through the Abell 3627 cluster

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