天然气河流I.：揭示高红移纤维的性质
Rivers of Gas I.: Unveiling The Properties of High Redshift Filaments
摘要：
在高红移时，宇宙网被广泛认为会对嵌入其中的星系的形态、动力学和恒星形成率产生重大影响，这突出表明需要对这样一个宇宙网络的性质进行全面研究。考虑到这一目标，我们进行了分析的高$z$气体和暗物质（DM）丝周围的银河系的祖先模拟与{ \sc ramses}自适应网格细化（AMR）代码从宇宙尺度（$\sim$ 1 Mpc）下降到其DM晕主机维里半径（$\sim$ 20 kpc在$z=4$）。气体和DM细丝的径向密度分布被发现具有相同的功能形式，即一个plummer样的配置文件修改，以考虑到这些细丝嵌入的壁。从模拟测量的典型灯丝芯半径$r_0$是一致的，在流体静力平衡的等温圆柱体。这样一个分析模型还预测了红移的核心半径的细丝在公平的协议DM $(r_0 \propto (1+z)^{-3.18\pm 0.28})$的测量值的演变。气体丝芯以$(r_0 \propto (1+z)^{-2.72\pm 0.26})$形式生长。在气体和DM中，温度和涡度在细丝的边缘急剧下降，提供了一个很好的方式来约束外部细丝半径。当反馈包括气体温度和涡度场强烈扰动，阻碍了在星系附近的测量。然而，从气体密度场测量的细丝的芯半径在很大程度上不受反馈的影响，并且中值中心密度仅减小约20%。
英文摘要：
At high redshift, the cosmic web is widely expected to have a significant impact on the morphologies, dynamics and star formation rates of the galaxies embedded within it, underscoring the need for a comprehensive study of the properties of such a filamentary network. With this goal in mind, we perform an analysis of high-$z$ gas and dark matter (DM) filaments around a Milky Way-like progenitor simulated with the {\sc ramses} adaptive mesh refinement (AMR) code from cosmic scales ($\sim$1 Mpc) down to the virial radius of its DM halo host ($\sim$20 kpc at $z=4$). Radial density profiles of both gas and DM filaments are found to have the same functional form, namely a plummer-like profile modified to take into account the wall within which these filaments are embedded. Measurements of the typical filament core radius $r_0$ from the simulation are consistent with that of isothermal cylinders in hydrostatic equilibrium. Such an analytic model also predicts a redshift evolution for the core radius of filaments in fair agreement with the measured value for DM $(r_0 \propto (1+z)^{-3.18\pm 0.28})$. Gas filament cores grow as $(r_0 \propto (1+z)^{-2.72\pm 0.26})$. In both gas and DM, temperature and vorticity sharply drop at the edge of filaments, providing an excellent way to constrain the outer filament radius. When feedback is included the gas temperature and vorticity fields are strongly perturbed, hindering such a measurement in the vicinity of the galaxy. However, the core radius of the filaments as measured from the gas density field is largely unaffected by feedback, and the median central density is only reduced by about 20%.
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