Repozytorium Uniwersytetu Jagiellońskiego

LOFAR, VLA, and Chandra observations of the Toothbrush galaxy cluster

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van Weeren, R. J.

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Brunetti, G.

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Brüggen, M.

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Andrade-Santos, F.

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Ogrean, G. A.

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Williams, W. L.

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Röttgering, H. J. A.

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Dawson, W. A.

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Forman, W. R.

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de Gasperin, F.

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Hardcastle, M. J.

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Jones, C.

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Miley, G. K.

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Rafferty, D. A.

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Rudnick, L.

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Sabater, J.

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Sarazin, C. L.

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Shimwell, T. W.

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Bonafede, A.

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Best, P. N.

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Bîrzan, L.

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Cassano, R.

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Chyży, Krzysztof T. [SAP11011785]

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Croston, J. H.

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Dijkema, T. J.

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Enßlin, T.

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Ferrari, C.

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Heald, G.

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Hoeft, M.

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Horellou, C.

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Jarvis, M. J.

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Kraft, R. P.

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Mevius, M.

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Intema, H. T.

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Murray, S. S.

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Orrú, E.

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Pizzo, R.

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Sridhar, S. S.

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Simionescu, A.

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Stroe, A.

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van der Tol, S.

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White, G. J.

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dc.date.accessioned

2016-06-29T11:58:52Z

dc.date.available

2016-06-29T11:58:52Z

dc.date.issued

2016

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dc.identifier.issn

0004-637X

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dc.identifier.uri

http://ruj.uj.edu.pl/xmlui/handle/item/28467

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eng

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Dodaję tylko opis bibliograficzny

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dc.title

LOFAR, VLA, and Chandra observations of the Toothbrush galaxy cluster

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dc.type

JournalArticle

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dc.abstract.en

We present deep LOFAR observations between 120 and 181 MHz of the “Toothbrush” (RX J0603.3+4214), a cluster that contains one of the brightest radio relic sources known. Our LOFAR observations exploit a new and novel calibration scheme to probe 10 times deeper than any previous study in this relatively unexplored part of the spectrum. The LOFAR observations, when combined with VLA, GMRT, and Chandra X-ray data, provide new information about the nature of cluster merger shocks and their role in re-accelerating relativistic particles. We derive a spectral index of \alpha = -0.8 \pm 0.1 at the northern edge of the main radio relic, steepening toward the south to \alpha \approx -2. The spectral index of the radio halo is remarkably uniform (\alpha = -1.16, with an intrinsic scatter of \leqslant 0.04). The observed radio relic spectral index gives a Mach number of M = 2.8\frac{+0,5}{-0,3}, assuming diffusive shock acceleration. However, the gas density jump at the northern edge of the large radio relic implies a much weaker shock (M \approx 1.2, with an upper limit of M \approx 1.5). The discrepancy between the Mach numbers calculated from the radio and X-rays can be explained if either (i) the relic traces a complex shock surface along the line of sight, or (ii) if the radio relic emission is produced by a re-accelerated population of fossil particles from a radio galaxy. Our results highlight the need for additional theoretical work and numerical simulations of particle acceleration and reacceleration at cluster merger shocks

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dc.subject.en

galaxies: clusters: individual: RX J0603.3+4214

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galaxies: clusters: intracluster medium

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large-scale structure of Universe

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radiation mechanisms: non-thermal

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X-rays: galaxies: clusters

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dc.description.volume

818

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dc.description.number

2

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dc.identifier.doi

10.3847/0004-637X/818/2/204

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dc.identifier.eissn

1538-4357

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dc.title.journal

The Astrophysical Journal

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dc.language.container

eng

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dc.affiliation

Wydział Fizyki, Astronomii i Informatyki Stosowanej : Instytut – Obserwatorium Astronomiczne

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dc.subtype

Article

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dc.identifier.articleid

204

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dc.rights.original

CC-BY; inne; ostateczna wersja wydawcy; po opublikowaniu; 12;

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.pointsMNiSW

[2016 A]: 40



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