EAGLE-like simulation models do not solve the entropy core problem in groups and clusters of galaxies
EAGLE-like simulation models do not solve the entropy core problem in groups and clusters of galaxies
复制标题
类似 EAGLE 的模拟模型不能解决星系群和星系团中的熵核心问题
DOI：
10.1093/mnras/stad342
复制
发表时间：
2023
影响因子：
4.8
通讯作者：
Altamura E
中科院分区：
文献类型：
--
作者：
Altamura E
最近的高分辨率宇宙学流体动力学模拟运行的各种代码系统地预测大量的熵在低红移的集群内介质，导致平坦的熵分布和抑制冷核人口。这一预测与X射线对星系团和星系团的观测结果不一致。我们使用EAGLE星系形成模型的一个新的实现来研究中心熵和轮廓形状对亚网格模型变化的敏感性，该亚网格模型应用于一组质量M500 = 8.8 × 1012 M <$和一个质量为2.9 × 1014 M <$的星系团的放大宇宙学模拟。使用我们的参考模型，校准匹配恒星的场星系的质量函数，我们证实，我们模拟的集团和集群包含热气体的核心熵太高。在没有人工传导、金属冷却或活动星系核（AGN）反馈的情况下运行的额外模拟会产生较低的熵水平，但仍然无法重现观察到的轮廓。相反，这两个物体在没有超新星反馈的情况下运行，显示出显着的熵增加，这可以归因于过度冷却和星星形成。活动星系核加热温度的变化不会对轮廓形状产生很大的影响，而只会对整体的归一化产生影响。最后，我们比较了运行与四个活动星系核加热方案，并获得类似的配置文件，与双极活动星系核加热，产生更高，更均匀的熵分布的例外。我们的研究留下了一个开放的问题，是否熵核心问题的模拟，特别是缺乏幂律冷核心配置文件，产生不正确的物理假设，缺少物理过程，或不足的数值分辨率。
Recent high-resolution cosmological hydrodynamic simulations run with a variety of codes systematically predict large amounts of entropy in the intra-cluster medium at low redshift, leading to flat entropy profiles and a suppressed cool-core population. This prediction is at odds with X-ray observations of groups and clusters. We use a new implementation of the EAGLE galaxy formation model to investigate the sensitivity of the central entropy and the shape of the profiles to changes in the sub-grid model applied to a suite of zoom-in cosmological simulations of a group of massM500= 8.8 × 1012M⊙and a cluster of mass 2.9 × 1014M⊙. Using our reference model, calibrated to match the stellar mass function of field galaxies, we confirm that our simulated groups and clusters contain hot gas with too high entropy in their cores. Additional simulations run without artificial conduction, metal cooling or active galactic nuclei (AGN) feedback produce lower entropy levels but still fail to reproduce observed profiles. Conversely, the two objects run without supernova feedback show a significant entropy increase which can be attributed to excessive cooling and star formation. Varying the AGN heating temperature does not greatly affect the profile shape, but only the overall normalization. Finally, we compared runs with four AGN heating schemes and obtained similar profiles, with the exception of bipolar AGN heating, which produces a higher and more uniform entropy distribution. Our study leaves open the question of whether the entropy core problem in simulations, and particularly the lack of power-law cool-core profiles, arise from incorrect physical assumptions, missing physical processes, or insufficient numerical resolution.
SWIFT：具有相互依赖的细粒度任务分配的 SPH
DOI：
--
发表时间：
2018
期刊：
影响因子：
--
作者：
M. Schaller;P. Gonnet;A. B. G. Chalk;P. Draper
通讯作者：
P. Draper