Diffuse filaments connect galaxy clusters to form the cosmic web. Detecting these filaments could yield information on the magnetic field strength, cosmic ray population, and temperature of intercluster gas; yet, the faint and large-scale nature of these bridges makes direct detections very challenging. Using multiple independent all-sky radio and X-ray maps we stack pairs of luminous red galaxies as tracers for cluster pairs. For the first time, we detect an average surface brightness between the clusters from synchrotron (radio) and thermal (X-ray) emission with ≳5σ significance, on physical scales larger than observed to date (${\ge}3$ Mpc). We obtain a synchrotron spectral index of α ≃ −1.0 and estimates of the average magnetic field strength of $30\,\mathrm{ nG} \le B \le 60 $ nG, derived from both equipartition and inverse-Compton arguments, implying a 5–15 per cent degree of field regularity when compared with Faraday rotation measure estimates. While the X-ray detection is inline with predictions, the average radio signal comes out higher than predicted by cosmological simulations and dark matter annihilation and decay models. This discovery demonstrates that there are connective structures between mass concentrations that are significantly magnetized, and the presence of sufficient cosmic rays to produce detectable synchrotron radiation.

中文翻译：

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通过无线电和 X 射线发射发现沿堆叠的宇宙细丝的磁场

漫射细丝连接星系团以形成宇宙网。探测这些细丝可以得到关于磁场强度、宇宙射线数量和星团间气体温度的信息；然而，这些桥梁的微弱和大型性质使得直接检测非常具有挑战性。使用多个独立的全天无线电和 X 射线图，我们将成对的发光红色星系堆叠起来作为星团对的示踪剂。我们第一次检测到来自同步加速器（无线电）和热（X 射线）发射的星团之间的平均表面亮度，显着性为 ≳5σ，物理尺度大于迄今为止观察到的 (${\ge}3$ Mpc) . 我们获得了 α ≃ -1.0 的同步加速器光谱指数和 $30\,\mathrm{ nG} \le B \le 60 $ nG 的平均磁场强度估计值，来自均分和逆康普顿参数，与法拉第旋转测量估计值相比，这意味着场规则度为 5-15%。虽然 X 射线探测与预测一致，但平均无线电信号的输出高于宇宙学模拟和暗物质湮灭和衰变模型的预测。这一发现表明，在显着磁化的质量浓度与存在足够的宇宙射线以产生可检测的同步辐射之间存在连接结构。