University of Hertfordshire

From the same journal

From the same journal

By the same authors

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

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  • R. J. Van Weeren
  • G. Brunetti
  • M. Brüggen
  • F. Andrade-Santos
  • G. A. Ogrean
  • W. L. Williams
  • H. J. A. Röttgering
  • W. A. Dawson
  • W.R. Forman
  • F. de Gasperin
  • C. Jones
  • G.K. Miley
  • D. A. Rafferty
  • L. Rudnick
  • J. Sabater
  • C.L. Sarazin
  • T. W. Shimwell
  • A. Bonafede
  • P. N. Best
  • L. Bîrzan
  • R. Cassano
  • K. T. Chyży
  • J. H. Croston
  • T. J. Dijkema
  • T. Ensslin
  • C. Ferrari
  • G. Heald
  • M. Hoeft
  • C. Horellou
  • M.J. Jarvis
  • R.P. Kraft
  • M. Mevius
  • H. T. Intema
  • S. S. Murray
  • E. Orrú
  • R. Pizzo
  • S. S. Sridhar
  • A. Simionescu
  • A. Stroe
  • S. van der Tol
  • G.J. White
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Original languageEnglish
JournalThe Astrophysical Journal
Publication statusPublished - 22 Feb 2016


We present deep LOFAR observations between 120-181 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 towards the south to $\alpha \approx - 2$. The spectral index of the radio halo is remarkably uniform ($\alpha = -1.16$, with an intrinsic scatter of $\leq 0.04$). The observed radio relic spectral index gives a Mach number of $\mathcal{M} = 2.8^{+0.5}_{-0.3}$, assuming diffusive shock acceleration (DSA). However, the gas density jump at the northern edge of the large radio relic implies a much weaker shock ($\mathcal{M} \approx 1.2$, with an upper limit of $\mathcal{M} \approx 1.5$). 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 re-acceleration at cluster merger shocks.


This document is the Accepted Manuscript version of an article accepted for publication in The Astrophysical Journal following peer review. The version of record [R. J. van Weeren, et al, LOFAR, VLA, AND CHANDRA OBSERVATIONS OF THE TOOTHBRUSH GALAXY CLUSTER, The Astrophysical Journal, Vol. 818 (2), published 22 February 2016] is available online at doi: © 2016. The American Astronomical Society. All rights reserved.

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