Horizon Run 5 宇宙学流体动力学模拟：探测从千秒差距到十亿秒差距尺度的星系形成
The Horizon Run 5 Cosmological Hydrodynamic Simulation: Probing Galaxy Formation from Kilo- to Giga-parsec Scales
AI总结：
本文介绍 HR5 高分辨率宇宙学流体动力学模拟，结合丰富子网格物理、混合并行 RAMSES 与 PGalF 后处理，再现星系形成观测并揭示 BAO 尺度上的流体动力学偏差。
摘要：
Horizon Run 5（HR5）是一项宇宙学流体动力学模拟，在捕捉宇宙 Gpc 尺度性质的同时达到了 1 kpc 的分辨率。在模拟盒内部，我们对一个体积为 1049×119×127 cMpc³ 的高分辨率长方体区域进行了放大。用于模拟星系形成的子网格物理过程包括辐射加热/冷却、UV 背景、恒星形成、超新星反馈、追踪氧和铁增丰的化学演化、超大质量黑洞增长，以及以双喷流加热模式呈现的活动星系核（AGN）反馈。针对该模拟，我们实现了 RAMSES 的混合 MPI-OMP 版本，专门面向现代众核多线程并行架构。除传统模拟快照外，还在运行过程中实时生成了光锥数据。在后处理方面，我们扩展了 Friends-of-Friend（FoF）算法，并开发了新的星系搜寻器 PGalF，用于分析 HR5 的输出。该模拟成功再现了宇宙恒星形成历史和星系分布连通性等观测结果。我们在广泛尺度范围内识别宇宙学结构，从长度为数 cMpc 的纤维，到半径约 100 cMpc 的空洞。模拟还表明，小尺度上的流体动力学效应会影响星系成团性，直至接近并超越重子声学振荡（BAO）尺度的极大尺度。因此，将该尺度用作宇宙标准尺时应保持谨慎：需要仔细理解相应偏差。该模拟预计将成为解释未来深空宇宙巡测的宝贵资源。
英文摘要：
Horizon Run 5 (HR5) is a cosmological hydrodynamical simulation which captures the properties of the Universe on a Gpc scale while achieving a resolution of 1kpc. Inside the simulation box we zoom-in on a high-resolution cuboid region with a volume of $1049\times119\times127\,{\rm cMpc}^3$.The sub-grid physics chosen to model galaxy formation includes radiative heating/cooling, UV background, star formation, supernova feedback, chemical evolution tracking the enrichment of oxygen and iron, the growth of supermassive black holes and feedback from active galactic nuclei (AGN) in the form of a dual jet-heating mode. For this simulation we implemented a hybrid MPI-OMP version of RAMSES, specifically targeted for modern many-core many thread parallel architectures. In addition to the traditional simulation snapshots, light-cone data was generated on the fly. For the post-processing, we extended the Friends-of-Friend (FoF) algorithm and developed a new galaxy finder PGalF to analyse the outputs of HR5. The simulation successfully reproduces observations, such as the cosmic star formation history and connectivity of galaxy distribution, We identify cosmological structures at a wide range of scales, from filaments with a length of several cMpc, to voids with a radius of ~100 cMpc. The simulation also indicates that hydrodynamical effects on small scales impact galaxy clustering up to very large scales near and beyond the baryonic acoustic oscillation (BAO) scale. Hence, caution should be taken when using that scale as a cosmic standard ruler: one needs to carefully understand the corresponding biases. The simulation is expected to be an invaluable asset for the interpretation of upcoming deep surveys of the Universe.
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