论文标题
部分可观测时空混沌系统的无模型预测
The quasi-adiabatic relaxation of haloes in the IllustrisTNG and EAGLE cosmological simulations
论文作者
论文摘要
已知重力绑定的光环的暗物质含量会受到其托管的星系和气体的影响。我们表征了在流体动力模拟套件中质量和鹰的质量四个数量级超过四个数量级的光环的响应。我们在球形平均的准绝热松弛框架中介绍了简单的拟合功能，该框架可以准确捕获我们探索的Halo质量和以光晕的距离的全部范围内的暗物质响应。我们表明，通常使用的方案考虑了球形暗物质外壳的半径$ r_f/r_i-1 $的相对变化，仅是其质量$ m_i/m_f-1 $的相对变化的函数，并不能准确地描述Illustristng和Eagle中大多数光环的测量响应。相反，$ r_f/r_i $另外取决于以光环为中心的距离$ r_f/r _ {\ rm vir} $，用于病毒半径$ r _ {\ rm vir} $的光环，在Illartistng和Eagle之间非常相似。我们还考虑了以前未建模的效果，可能是由反馈相关的流出驱动的，其中具有$ r_f/r_i \ simeq1 $（即没有放松）的外壳具有$ m_i/m_f $与Unity有显着不同的。我们的结果立即适用于许多半分析工具，用于建模银河系和大规模结构。我们还研究了这种反应对超出总质量的几种光环和星系性能的依赖性，发现它主要与光晕浓度和恒星形成速率有关。我们讨论了这些结果的可能扩展，以建立对暗物质与重子之间小规模联系的更深入的物理理解。
The dark matter content of a gravitationally bound halo is known to be affected by the galaxy and gas it hosts. We characterise this response for haloes spanning over four orders of magnitude in mass in the hydrodynamical simulation suites IllustrisTNG and EAGLE. We present simple fitting functions in the spherically averaged quasi-adiabatic relaxation framework that accurately capture the dark matter response over the full range of halo mass and halo-centric distance we explore. We show that commonly employed schemes, which consider the relative change in radius $r_f/r_i-1$ of a spherical dark matter shell to be a function of only the relative change in its mass $M_i/M_f-1$, do not accurately describe the measured response of most haloes in IllustrisTNG and EAGLE. Rather, $r_f/r_i$ additionally explicitly depends upon halo-centric distance $r_f/R_{\rm vir}$ for haloes with virial radius $R_{\rm vir}$, being very similar between IllustrisTNG and EAGLE and across halo mass. We also account for a previously unmodelled effect, likely driven by feedback-related outflows, in which shells having $r_f/r_i\simeq1$ (i.e., no relaxation) have $M_i/M_f$ significantly different from unity. Our results are immediately applicable to a number of semi-analytical tools for modelling galactic and large-scale structure. We also study the dependence of this response on several halo and galaxy properties beyond total mass, finding that it is primarily related to halo concentration and star formation rate. We discuss possible extensions of these results to build a deeper physical understanding of the small-scale connection between dark matter and baryons.
