The Coma Cluster at LOFAR Frequencies. II. The Halo, Relic, and a New Accretion Relic

Bonafede, A.; Brunetti, G.; Rudnick, Lawrence; Vazza, Franco; Bourdin, H.; Giovannini, G.; Shimwell, T. W.; Zhang, Xiaoyuan; Mazzotta, P.; Simionescu, A.; Biava, N.; Bonnassieux, E.; Brienza, M.; Brüggen, M.; Rajpurohit, K.; Riseley, C. J.; Stuardi, C.; Feretti, L.; Tasse, C.; Botteon, A.; Carretti, E.; Cassano, R.; Cuciti, V.; Gasperin, F. de; Gastaldello, F.; Rossetti, M.; Röttgering, H. J. A.; Venturi, T.; Weeren, R. J. van

doi:10.3847/1538-4357/ac721d

Cited by 48 publications

(55 citation statements)

References 97 publications

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“…While not of high significance, the excess is seen for both the RPS and extended radio source samples. large extent ≈ ¢ 32 × ¢ 10 (;1.08× 0.34 Mpc 2 ), which is broadly consistent with Giovannini et al (1991) (see also Bonafede et al 2021Bonafede et al , 2022, Figures 1 and 4, respectively). The sharpness of the surface brightness contours suggests that the relic consists of a high-surface-brightness southwestern part and a fainter, diffuse low-surface-brightness northwestern part.…”

Section: X-ray Propertiessupporting

confidence: 90%

“…The radio relic, B1253+275, plausibly associated with a runaway merger shock (see also Zhang et al 2019) has a large extent ≈ ¢ 32 × ¢ 10 (;1.08 × 0.34 Mpc 2 ) and the low-frequency flux density S 400 MHz = 0.98 ± 0.06 Jy. This extended radio relic shows diffuse emission with a central ridge, a bridge of emission connected with the narrow-angle-tailed galaxy NGC 4789, which suggests that this tailed radio galaxy could be the source of the seed particles feeding the radio relic, 1253+275 (see also Giovannini et al 1991;Bonafede et al 2021Bonafede et al , 2022. 12.…”

Section: Discussionmentioning

confidence: 93%

“…The tailed radio source to the southwest of the relic is associated with NGC 4789, seen clearly in our high-resolution images (Figure 3 and see also Figure 11). The extended radio relic shows diffuse emission with a central ridge, a bridge of emission connected to the narrow-angle tailed galaxy NGC 4789 (see Figure 12), which suggests that this tailed radio galaxy could be the source of the seed particles feeding the radio relic, 1253+275, providing a direct connection between a radio relic source and the radio galaxy, NGC 4789 (Giovannini et al 1991;van Weeren et al 2017;Bonafede et al 2021Bonafede et al , 2022.…”

Section: X-ray Propertiesmentioning

confidence: 99%

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High-resolution, High-sensitivity, Low-frequency uGMRT View of Coma Cluster of Galaxies

Lal

Lyskova

Zhang

et al. 2022

ApJ

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We present high-resolution, high-sensitivity upgraded Giant Metrewave Radio Telescope observations of the Coma cluster (A1656) at 250–500 MHz and 550–850 MHz. At 250–500 MHz, 135 sources have extensions >0.′45 (with peak-to-local-noise ratio >4). Of these, 24 sources are associated with Coma-member galaxies. In addition, we supplement this sample of 24 galaxies with 20 ram pressure stripped (RPS) galaxies from (Chen et al. 2020, eight are included in the original extended radio source sample) and an additional five are detected and extended. We present radio morphologies, radio spectra, spectral index maps, and equipartition properties for these two samples. In general, we find the equipartition properties lie within a narrow range (e.g., P min = 1–3 × 10− 13 dynes cm−2). Only NGC 4874, one of the two brightest central Coma cluster galaxies, has a central energy density and pressure about five times higher and a radio source age about 50% lower than that of the other Coma galaxies. We find a diffuse tail of radio emission trailing the dominant galaxy of the merging NGC 4839 group that coincides with the slingshot tail seen in X-rays. The southwestern radio relic, B1253+275, has a large extent ≈32′ × 10′ (≃1.08 × 0.34 Mpc2). For NGC 4789, whose long radio tails merge into the relic and may be a source of its relativistic seed electrons, we find a transverse radio spectral gradient, a steepening from southwest to northeast across the width of the radio source. Finally, radio morphologies of the extended and RPS samples suggest that these galaxies are on their first infall into Coma on (predominantly) radial orbits.

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Section: X-ray Propertiessupporting

confidence: 90%

Section: Discussionmentioning

confidence: 93%

Section: X-ray Propertiesmentioning

confidence: 99%

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High-resolution, High-sensitivity, Low-frequency uGMRT View of Coma Cluster of Galaxies

Lal

Lyskova

Zhang

et al. 2022

ApJ

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“…Although we used a finer grid resolution (~115 kpc versus ~185 kpc) than Botteon et al (2020b) for A399-401, this might indicate that the two radio bridges are produced by similar processes. When we compare the slopes from these two radio bridges with mini and giant radio halos in the literature or with those from A399 and A401, we conclude that slopes from radio bridges are overall flatter (Govoni et al 2001;Feretti et al 2001;Giacintucci et al 2005;Rajpurohit et al 2018Rajpurohit et al , 2021Botteon et al 2018bBotteon et al , 2020bIgnesti et al 2020;Biava et al 2021;Bonafede et al 2021Bonafede et al , 2022. This might be an indication that the physical connections between the ICM and radio bridges and the ICM and radio halos are different from each other.…”

Section: Origin Of the Radio Bridgementioning

confidence: 79%

Deep study of A399-401: Application of a wide-field facet calibration

Jong

Weeren

Botteon

et al. 2022

A&A

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Context. Diffuse synchrotron emission pervades numerous galaxy clusters, indicating the existence of cosmic rays and magnetic fields throughout the intra-cluster medium. It is general consensus that this emission is generated by shocks and turbulence that are activated during cluster merger events and cause a (re-)acceleration of particles to highly relativistic energies. Similar emission has recently been detected in megaparsec-scale filaments connecting pairs of premerging clusters. These instances are the first in which diffuse emission has been found outside of the main cluster regions. Aims. We aim to examine the particle acceleration mechanism in the megaparsec-scale bridge between Abell 399 and Abell 401 and assess in particular whether the synchrotron emission originates from first-or second-order Fermi reacceleration. We also consider the possible influence of active galactic nuclei (AGNs). Methods. To examine the diffuse emission and the AGNs in Abell 399 and Abell 401, we used deep (~40 hours) LOw-Frequency ARray (LOFAR) observations with an improved direction-dependent calibration to produce radio images at 144 MHz with a sensitivity of σ = 79 µJy beam −1 at a 5.9 ′′ × 10.5 ′′ resolution. Using a point-to-point analysis, we searched for a correlation between the radio and X-ray brightness from which we would be able to constrain the particle reacceleration mechanism. Results. Our radio images show the radio bridge between the radio halos at high significance. We find a trend between the radio and X-ray emission in the bridge. We also measured the correlation between the radio and X-ray emission in the radio halos and find a strong correlation for Abell 401 and a weaker correlation for Abell 399. On the other hand, we measure a strong correlation for the radio halo extension from A399 in the northwest direction. With our deep images, we also find evidence for AGN particle injection and reenergized fossil plasma in the radio bridge and halos. Conclusions. We argue that second-order Fermi reacceleration is currently the most favored process to explain the radio bridge. In addition, we find indications for a scenario in which past AGN particle injection might introduce significant scatter in the relation between the radio and X-ray emission in the bridge, but may also supply the fossil plasma needed for in situ reacceleration. The results for Abell 401 are also clearly consistent with a second-order Fermi reacceleration model. The relation between the thermal and nonthermal components in the radio halo in Abell 399 is affected by a recent merger. However, a strong correlation toward its northwest extension and the steep spectrum in the radio halo support an origin of the radio emission in a second-order Fermi reacceleration model as well. The evidence that we find for reenergized fossil plasma near Abell 399 and in the radio bridge supports the reacceleration of the fossil plasma scenario.

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“…Upper limits were found with different approaches: cross-correlating large radio maps with the large-scale galaxy distribution (Vernstrom et al 2017;Brown et al 2017); analysing RMs of giant radio galaxies (O'Sullivan et al 2019;Stuardi et al 2020); cross-correlating RMs with the galaxy distribution (Amaral et al 2021); simulations constrained by observations or non-detections (Vacca et al 2018;Locatelli et al 2021). Intracluster bridges of radio emission were detected in a few galaxy clusters 1 (e.g., Kim et al 1989;Brown & Rudnick 2011;Bonafede et al 2022;de Gasperin et al 2022). A detection of the synchrotron emission from an intercluster bridge connecting close pairs of merging clusters was obtained by Govoni et al (2019) (see also Botteon et al 2020), establishing the presence of magnetic fields in the IGM beyond cluster outskirts.…”

Section: Introductionmentioning

confidence: 99%

Magnetic field evolution in cosmic filaments with LOFAR data

Carretti,

O'Sullivan,

Vacca

et al. 2022

Preprint

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Measuring the magnetic field in cosmic filaments reveals how the Universe is magnetised and the process that magnetised it. Using the Rotation Measures (RM) at 144-MHz from the LoTSS DR2 data, we analyse the rms of the RM extragalactic component as a function of redshift to investigate the evolution with redshift of the magnetic field in filaments. From previous results, we find that the extragalactic term of the RM rms at 144-MHz is dominated by the contribution from filaments (more than 90 percent). Including an error term to account for the minor contribution local to the sources, we fit the data with a model of the physical filament magnetic field, evolving as 𝐵 𝑓 = 𝐵 𝑓 ,0 (1 + 𝑧) 𝛼 and with a density drawn from cosmological simulations of five magnetogenesis scenarios. We find that the best-fit slope is in the range 𝛼 = [−0.2, 0.1] with uncertainty of 𝜎 𝛼 = 0.4-0.5, which is consistent with no evolution. The comoving field decreases with redshift with a slope of 𝛾 = 𝛼 − 2 = [−2.2, −1.9]. The mean field strength at 𝑧 = 0 is in the range 𝐵 𝑓 ,0 = 39-84 nG. For a typical filament gas overdensity of 𝛿 𝑔 = 10 the filament field strength at 𝑧 = 0 is in the range 𝐵 10 𝑓 ,0 = 8-26 nG. A primordial stochastic magnetic field model with initial comoving field of 𝐵 Mpc = 0.04-0.11 nG is favoured. The primordial uniform field model is rejected.

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The Coma Cluster at LOFAR Frequencies. II. The Halo, Relic, and a New Accretion Relic

Cited by 48 publications

References 97 publications

High-resolution, High-sensitivity, Low-frequency uGMRT View of Coma Cluster of Galaxies

High-resolution, High-sensitivity, Low-frequency uGMRT View of Coma Cluster of Galaxies

Deep study of A399-401: Application of a wide-field facet calibration

Magnetic field evolution in cosmic filaments with LOFAR data

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