介绍RomulusC：一个具有前所未有分辨率的星系团宇宙学模拟
Introducing RomulusC: A Cosmological Simulation of a Galaxy Cluster with Unprecedented Resolution
摘要：
我们目前的第一个结果从RomulusC，最高分辨率的宇宙流体动力学模拟的星系团运行到目前为止。RomulusC是一种放大模拟光环的方法，其$z=0$质量为$10^{14}$ M $_{\odot}$，使用与Romulus25相同的子网格物理和分辨率运行（Tremmel等人，2017）。凭借前所未有的质量和空间分辨率，RomulusC代表了一个独特的机会，可以研究致密环境中星系的演化，直到矮质量。我们证明了RomulusC的结果在一个集群内介质（ICM）与观察一致。最亮的星系团（BCG）的恒星形成历史和恒星质量与观测和丰度匹配结果一致，表明我们的子网格模型，优化只再现场矮和银河系质量星系的观测，能够产生合理的星系质量和恒星形成历史在更高的质量系统。来自超大质量黑洞（SMBHs）的反馈通过驱动与低熵核心共存的大规模准直外流来调节恒星的形成。我们发现，与低至矮星系质量的场相比，非BCG星系团成员星系基本上被猝灭，并且在低质量时，猝灭与质量或距星系团中心的距离无关。这种增强的猝灭粒子数超出了$R_{200}$，并在高红移处就位。同样，我们预测SMBH活动在BCG之外的星系团内受到显着抑制，但显示当只关注最大质量星系中最明亮的AGN时，这种效果可能会丢失。
英文摘要：
We present the first results from RomulusC, the highest resolution cosmological hydrodynamic simulation of a galaxy cluster run to date. RomulusC, a zoom-in simulation of a halo with $z=0$ mass $10^{14}$ M$_{\odot}$, is run with the same sub-grid physics and resolution as Romulus25 (Tremmel et al. 2017). With unprecedented mass and spatial resolution, RomulusC represents a unique opportunity to study the evolution of galaxies in dense environments down to dwarf masses. We demonstrate that RomulusC results in an intracluster medium (ICM) consistent with observations. The star formation history and stellar mass of the brightest cluster galaxy (BCG) is consistent with observations and abundance matching results, indicating that our sub-grid models, optimized only to reproduce observations of field dwarf and Milky Way mass galaxies, are able to produce reasonable galaxy masses and star formation histories in much higher mass systems. Feedback from supermassive black holes (SMBHs) regulates star formation by driving large-scale, collimated outflows that coexist with a low entropy core. We find that non-BCG cluster member galaxies are substantially quenched compared to the field down to dwarf galaxy masses and, at low masses, quenching is seen to have no dependence on mass or distance from the cluster center. This enhanced quenched population extends beyond $R_{200}$ and is in place at high redshift. Similarly, we predict that SMBH activity is significantly suppressed within clusters outside of the BCG, but show how the effect could be lost when only focusing on the brightest AGN in the most massive galaxies.
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