论文标题
丝状重子和在哪里找到它们：在当地宇宙网络中合并和积聚冲击的同步辐射的预测
Filamentary Baryons and Where to Find Them: A forecast of synchrotron radiation from merger and accretion shocks in the local Cosmic Web
论文作者
论文摘要
我们为北方一半的一半的低红移（$ z <0.2 $）cosmic网络产生概率预测。 In particular, we predict the contribution to the specific intensity function at $ν_\mathrm{obs} = 150\ \mathrm{MHz}$ from merger shocks in clusters and accretion shocks in filaments, both of which arise during large-scale structure formation.我们假设一种原始的磁化情况，但是我们的方法足以允许探索替代磁化场景，甚至替代辐射机制和光谱窗口。将来，通过比较不同的预测，可以从同步宇宙网络检测中推断出最合理的物理模型。我们的方法结合了贝叶斯大规模结构重建，MHD宇宙学模拟的快照，高斯随机场和射线追踪方法。结果有助于选择对深度观测的目标，并且可以在实际检测实验中使用。我们重点介绍了大力神集群，昏迷群，Abell 2199，Abell 2255，Lockman Hole和Ursa Major Supercluster的预测。在学位尺度分辨率下，中位强度达到$ m_ {i_ν} \ sim 10^{ - 1} \ξ_e\ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ deg^{ - 2}} $，其中$ξ_e$是电子加速效率。
We generate probabilistic predictions of the low-redshift ($z < 0.2$) synchrotron Cosmic Web for half of the Northern Sky. In particular, we predict the contribution to the specific intensity function at $ν_\mathrm{obs} = 150\ \mathrm{MHz}$ from merger shocks in clusters and accretion shocks in filaments, both of which arise during large-scale structure formation. We assume a primordial magnetogenesis scenario, but our method is general enough to allow for an exploration of alternative magnetogenesis scenarios - and even alternative radiation mechanisms and spectral windows. In the future, by comparing different predictions, one could infer the most plausible physical model from a synchrotron Cosmic Web detection. Our method combines Bayesian large-scale structure reconstructions, snapshots of an MHD cosmological simulation, a Gaussian random field, and a ray tracing approach. The results help to select targets for deep observations and can be used in actual detection experiments. We highlight predictions for the Hercules Cluster, the Coma Cluster, Abell 2199, Abell 2255, the Lockman Hole and the Ursa Major Supercluster. At degree-scale resolution, the median specific intensity reaches $m_{I_ν} \sim 10^{-1}\ ξ_e\ \mathrm{Jy\ deg^{-2}}$, where $ξ_e$ is the electron acceleration efficiency.
