论文标题
揭示宇宙网络的黑线
Revealing the Dark Threads of the Cosmic Web
论文作者
论文摘要
现代宇宙学预测，今天我们宇宙中的重要性已经汇集到一个通俗地称为宇宙网络的庞大的丝状结构网络。由于此问题在电磁上是看不见的（即深色），要么是在发射中的图像太分散，因此该宇宙Web范式的测试受到限制。广场调查确实显示了星系分布中的网络样结构，但这些发光的星系占重型物质的10％。通过遥远的类星体光谱法支持该模型的阶层介质（IGM）吸收的统计数据尚未将弥漫性IGM与Web结合起来。在这里，我们报告了一种受到物理多头性粘液模具启发的新方法，该方法能够从星系调查中推断宇宙网的密度场。将我们的技术应用于当地宇宙的星系和吸收线调查，我们证明了大部分IGM确实存在于宇宙网络中。从宇宙网络丝的郊区，大约是宇宙平均物质密度（RHO_M）和大约。 5来自附近星系的病毒半径，我们检测到增加的H I吸收特征，向更高的密度和圆形培养基，至大约。 200 rho_m。但是，在最密集的环境中抑制了吸收，表明在星系内的细丝和/或反馈过程中，冲击加热和电离。
Modern cosmology predicts that matter in our Universe has assembled today into a vast network of filamentary structures colloquially termed the Cosmic Web. Because this matter is either electromagnetically invisible (i.e., dark) or too diffuse to image in emission, tests of this cosmic web paradigm are limited. Wide-field surveys do reveal web-like structures in the galaxy distribution, but these luminous galaxies represent less than 10% of baryonic matter. Statistics of absorption by the intergalactic medium (IGM) via spectroscopy of distant quasars support the model yet have not conclusively tied the diffuse IGM to the web. Here, we report on a new method inspired by the Physarum polycephalum slime mold that is able to infer the density field of the Cosmic Web from galaxy surveys. Applying our technique to galaxy and absorption-line surveys of the local Universe, we demonstrate that the bulk of the IGM indeed resides in the Cosmic Web. From the outskirts of Cosmic Web filaments, at approximately the cosmic mean matter density (rho_m) and approx. 5 virial radii from nearby galaxies, we detect an increasing H I absorption signature towards higher densities and the circumgalactic medium, to approx. 200 rho_m. However, the absorption is suppressed within the densest environments, suggesting shock-heating and ionization deep within filaments and/or feedback processes within galaxies.
