Galaxy 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.

A radio ridge connecting two galaxy clusters in a filament of the cosmic web

Govoni F.;Bonafede A.;Paladino R.;Vazza F.
Membro del Collaboration Group
;
Vacca V.;Giovannini G.;Feretti L.;Loi F.;GHELLER, CLAUDIO;BRUGGEN, MARCUS;Hoeft M.;Wise M.
2019

Abstract

Galaxy 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.
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.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11585/703722
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