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Redshift evolution of the hot intracluster gas metallicity in the C-EAGLE cluster simulations
Monthly Notices of the Royal Astronomical Society ( IF 4.7 ) Pub Date : 2021-07-28 , DOI: 10.1093/mnras/stab2194
Francesca A Pearce 1 , Scott T Kay 1 , David J Barnes 2 , Yannick M Bahé 3 , Richard G Bower 4
Affiliation  

The abundance and distribution of metals in galaxy clusters contain valuable information about their chemical history and evolution. By looking at how metallicity evolves with redshift, it is possible to constrain the different metal production channels. We use the C-EAGLE clusters, a sample of 30 high-resolution (mgas ≃ 1.8 × 106 M⊙) cluster zoom simulations, to investigate the redshift evolution of metallicity, with particular focus on the cluster outskirts. The early enrichment model, in which the majority of metals are produced in the core of cluster progenitors at high redshift, suggests that metals in cluster outskirts have not significantly evolved since z = 2. With the C-EAGLE sample, we find reasonable agreement with the early enrichment model as there is very little scatter in the metallicity abundance at large radius across the whole sample, out to at least z = 2. The exception is Fe for which the radial dependence of metallicity was found to evolve at low redshift as a result of being mainly produced by Type Ia supernovae, which are more likely to be formed at later times than core-collapse supernovae. We also found considerable redshift evolution of metal abundances in the cores of the C-EAGLE clusters that has not been seen in other simulations or observation-based metallicity studies. Since we find this evolution to be driven by accretion of low-metallicity gas, it suggests that the interaction between outflowing, AGN-heated material and the surrounding gas is important for determining the core abundances in clusters.

中文翻译:

C-EAGLE 星团模拟中热星团内气体金属丰度的红移演化

星系团中金属的丰度和分布包含有关其化学历史和演化的宝贵信息。通过观察金属丰度如何随红移变化,可以限制不同的金属生产渠道。我们使用 C-EAGLE 星团(30 个高分辨率(mgas ≃ 1.8 × 106 M⊙)星团缩放模拟样本)来研究金属量的红移演化,特别关注星团外围。早期富集模型,其中大部分金属在高红移的簇前体的核心产生,表明自 z = 2 以来簇外围的金属没有显着进化。对于 C-EAGLE 样本,我们发现与早期富集模型有合理的一致性,因为在整个样品的大半径范围内金属丰度丰度几乎没有分散,至少 z = 2。发现金属丰度的径向依赖性演变的 Fe 除外由于主要由 Ia 型超新星产生,因此红移较低,与核心坍缩超新星相比,Ia 型超新星更可能形成较晚的时间。我们还发现了 C-EAGLE 星团核心中金属丰度的相当大的红移演变,这在其他模拟或基于观测的金属丰度研究中未见。由于我们发现这种演化是由低金属度气体的吸积驱动的,这表明流出的、受活动星系核加热的物质与周围气体之间的相互作用对于确定星团中的核心丰度很重要。
更新日期:2021-07-28
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