A radio ridge connecting two galaxy clusters in a filament of the cosmic web. (arXiv:1906.07584v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Govoni_F/0/1/0/all/0/1">F. Govoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orru_E/0/1/0/all/0/1">E. Orr&#xf9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonafede_A/0/1/0/all/0/1">A. Bonafede</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iacobelli_M/0/1/0/all/0/1">M. Iacobelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paladino_R/0/1/0/all/0/1">R. Paladino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vazza_F/0/1/0/all/0/1">F. Vazza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murgia_M/0/1/0/all/0/1">M. Murgia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vacca_V/0/1/0/all/0/1">V. Vacca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giovannini_G/0/1/0/all/0/1">G. Giovannini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feretti_L/0/1/0/all/0/1">L. Feretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loi_F/0/1/0/all/0/1">F. Loi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardi_G/0/1/0/all/0/1">G. Bernardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrari_C/0/1/0/all/0/1">C. Ferrari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pizzo_R/0/1/0/all/0/1">R.F. Pizzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gheller_C/0/1/0/all/0/1">C. Gheller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manti_S/0/1/0/all/0/1">S. Manti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruggen_M/0/1/0/all/0/1">M. Br&#xfc;ggen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brunetti_G/0/1/0/all/0/1">G. Brunetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassano_R/0/1/0/all/0/1">R. Cassano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gasperin_F/0/1/0/all/0/1">F. de Gasperin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ensslin_T/0/1/0/all/0/1">T.A. En&#xdf;lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoeft_M/0/1/0/all/0/1">M. Hoeft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Horellou_C/0/1/0/all/0/1">C. Horellou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Junklewitz_H/0/1/0/all/0/1">H. Junklewitz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rottgering_H/0/1/0/all/0/1">H.J.A. R&#xf6;ttgering</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scaife_A/0/1/0/all/0/1">A.M.M. Scaife</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shimwell_T/0/1/0/all/0/1">T.W. Shimwell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weeren_R/0/1/0/all/0/1">R.J. van Weeren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wise_M/0/1/0/all/0/1">M. Wise</a>

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 intra-cluster gas. We observed a ridge of
radio emission connecting the merging galaxy clusters Abell 0399 and Abell 0401
with the Low Frequency Array (LOFAR) at 140 MHz. 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 re-accelerate a pre-existing
population of relativistic particles, producing emission at radio wavelengths
that illuminates the magnetic ridge.

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 intra-cluster gas. We observed a ridge of
radio emission connecting the merging galaxy clusters Abell 0399 and Abell 0401
with the Low Frequency Array (LOFAR) at 140 MHz. 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 re-accelerate a pre-existing
population of relativistic particles, producing emission at radio wavelengths
that illuminates the magnetic ridge.

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