论文标题
宇宙丝中的磁场演变，带有lofar数据
Magnetic field evolution in cosmic filaments with LOFAR data
论文作者
论文摘要
测量宇宙丝中的磁场揭示了宇宙是如何磁性化的以及磁性磁性的过程。使用Lots DR2数据的旋转度量（RM）在144-MHz处使用，我们分析了REDSHIFT的RM RM RMS的RMS作为RedShift的函数，以在细丝中使用磁场的红移来研究演变。从先前的结果来看，我们发现RM RM在144 MHz时的外乳外项由细丝的贡献（超过90％）主导。包括一个错误的术语来说明源的次要贡献，我们使用物理丝磁场的模型拟合数据，以$ b_f = b_ {f，0} \，（1+z）^α$演变，并从五种磁化场景的宇宙学模拟中得出密度。我们发现，最佳拟合坡度在$α= [-0.2，0.1] $的范围内，不确定性为$σ_α= 0.4 $ - 0.5，这与没有进化是一致的。 Comoving场随红移而降低，斜率为$γ=α-2 = [-2.2，-1.9] $。 $ z = 0 $的平均场强度在范围内$ b_ {f，0} = 39 $ - 84〜ng。对于典型的丝状气体过度密度为$δ_g= 10 $ $ z = 0 $的细丝场强度在范围内$ b_ {f，0}^{10} = 8 $ - 26〜ng。 $ b _ {\ rm mpc} = 0.04 $ - 0.11〜ng的原始随机磁场模型受到$ b _ {\ rm mpc}的初始磁场模型。原始统一场模型被拒绝。
Measuring the magnetic field in cosmic filaments reveals how the Universe is magnetised and the process that magnetised it. Using the Rotation Measures (RM) at 144-MHz from the LoTSS DR2 data, we analyse the rms of the RM extragalactic component as a function of redshift to investigate the evolution with redshift of the magnetic field in filaments. From previous results, we find that the extragalactic term of the RM rms at 144-MHz is dominated by the contribution from filaments (more than 90 percent). Including an error term to account for the minor contribution local to the sources, we fit the data with a model of the physical filament magnetic field, evolving as $B_f = B_{f,0}\,(1+z)^α$ and with a density drawn from cosmological simulations of five magnetogenesis scenarios. We find that the best-fit slope is in the range $α= [-0.2, 0.1]$ with uncertainty of $σ_α= 0.4$--0.5, which is consistent with no evolution. The comoving field decreases with redshift with a slope of $γ= α- 2 = [-2.2, -1.9]$. The mean field strength at $z=0$ is in the range $B_{f,0}=39$--84~nG. For a typical filament gas overdensity of $δ_g=10$ the filament field strength at $z=0$ is in the range $B_{f,0}^{10}=8$--26~nG. A primordial stochastic magnetic field model with initial comoving field of $B_{\rm Mpc} = 0.04$--0.11~nG is favoured. The primordial uniform field model is rejected.
