Govoni, F.Orru, E.Bonafede, A.Iacobelli, M.Paladino, R.Vazza, F.Murgia, M.Vacca, V.Giovannini, G.Feretti, L.Loi, F.Bernardi, G.Ferrari, C.Pizzo, R. F.Gheller, C.Manti, S.Bruggen, M.Brunetti, G.Cassano, R.de Gasperin, F.Ensslin, T. A.Hoeft, M.Horellou, C.Junklewitz, H.Rottgering, H. J. A.Scaife, A. M. M.Shimwell, T. W.van Weeren, R. J.Wise, M.2019-06-242019-06-242019-06-242019-06-0710.1126/science.aat7500https://infoscience.epfl.ch/handle/20.500.14299/158458WOS:000471079600005Galaxy clusters are the most massive gravitationally bound structures in the Universe. They grow by accreting smaller structures in a merging process that produces shocks and turbulence in the intracluster gas. We observed a ridge of radio emission connecting the merging galaxy clusters Abell 0399 and Abell 0401 with the Low-Frequency Array (LOFAR) telescope network at 140 megahertz. This emission requires a population of relativistic electrons and a magnetic field located in a filament between the two galaxy clusters. We performed simulations to show that a volume-filling distribution of weak shocks may reaccelerate a preexisting population of relativistic particles, producing emission at radio wavelengths that illuminates the magnetic ridge.Multidisciplinary SciencesScience & Technology - Other Topicsshock accelerationbinary clustercd clustersemissiondynamicsrelicsnearbytext::journal::journal article::research article