Project Title: Hydrodynamical simulations of galaxy formation in the Planck cosmogony

项目名称：普朗克宇宙演化中星系形成的流体动力学模拟

• 批准号: 1611002
• 金额: --
• 依托单位: Durham University
• 依托单位国家: 英国
• 项目类别: Studentship
• 财政年份: 2015
• 资助国家: 英国
• 起止时间: 2015 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=studentship-1611002
• 关键词: Project; Title; Hydrodynamical; simulations; galaxy

The basic model for how galaxies form within the framework of a cold dark matter cosmogony has been established for many years, however many crucial aspects are still poorly understood. For example, what physical processes determine galaxy stellar masses and galaxy sizes? How do these properties evolve throughout cosmic history? How do stars and AGN regulate the evolution of galaxy properties? Numerical simulations and theoretical models are a valuable tool for exploring these questions, but the huge dynamic range involved, and the complexity of the plausible underlying physics, limits the ab initio predictive power of such calculations. The Eagle simulations1 , performed on the Dirac supercomputer in Durham and on curie in Paris, produced a population of galaxies with properties very simulated to those observed. eagle has been a tremendous improvement over previous simulation projects, however the limited numerical resolution still prevents us from examining important aspects of galaxy formation. For example what are the detailed properties of the high redshift, z 10, population of galaxies that are a major target for the James Webb Space Telescope and are thought to be the driver of reionisation, a key science area of lofar. Can simulations reproduce the detailed properties of Milky Way-like galaxies (bulge/disk properties, occurrence of bars, stellar halos, properties of satellites of galaxies) - an important research area in the context of gaia. Simply increasing resolution is not an option because current codes do not scale to the thousands of cores of current supercomputers, nor can they exploit the new generation of hardware accelerators such as intel's Phi and nvidia's GPU. This project will take advantage of the new swift code, developed in Durham in collaboration between the icc, Computer Science, and intel in the context of Durham's status as Intel Parallel Computing Centre (IPCC). swift2 uses task-based parallelism, asynchronous communication, and is designed to take advantage of AVX, with extensions to Phi and GPUs in progress. You will contribute to developing swift, in particular adapting it to include the galaxy formation modules from eagle. You will then use the new code to perform zoomed simulations of individual galaxies and clusters of galaxies at unprecedented realism. Comparing these to observations will provide crucial tests of the CDM paradigm on the small scales that are not currently accessible to simulators.

星系如何在冷暗物质宇宙框架内形成的基本模型已经建立了很多年，然而许多关键的方面仍然知之甚少。例如，什么物理过程决定了星系的恒星质量和星系大小？这些特性是如何在整个宇宙历史中进化的？恒星和活动星系核如何调节星系属性的演化？数值模拟和理论模型是探索这些问题的宝贵工具，但涉及的巨大动态范围以及看似合理的基础物理的复杂性，限制了此类计算的从头计算预测能力。在达勒姆的狄拉克超级计算机和巴黎的居里星系上进行的Eagle模拟1产生了一组星系，其性质与观测到的星系非常相似。EAGLE已经比以前的模拟项目有了巨大的改进，但是有限的数值分辨率仍然阻碍了我们研究星系形成的重要方面。例如，高红移z10星系群的详细性质是什么，这些星系群是詹姆斯·韦伯太空望远镜的主要目标，被认为是LOFAR的关键科学领域--再电离的驱动力。模拟能否再现类银河系的详细属性(凸起/盘状属性、星条的出现、恒星晕、星系卫星的属性)--这是GAIA背景下的一个重要研究领域。简单地提高分辨率不是一种选择，因为目前的代码不能扩展到当前超级计算机的数千个核心，也不能利用新一代硬件加速器，如英特尔的Phi和英伟达的GPU。该项目将利用国际刑事法院、计算机科学和英特尔在达勒姆作为英特尔并行计算中心(IPCC)的背景下合作在达勒姆开发的新的快速代码。Swift2使用基于任务的并行和异步通信，旨在利用AVX，并正在对Phi和GPU进行扩展。你将为开发SWIFT做出贡献，特别是对它进行调整，以包括Eagle的星系形成模块。然后，您将使用新代码以前所未有的真实感对单个星系和星系团执行缩放模拟。将这些与观测值进行比较，将在目前模拟器无法访问的小范围内对清洁发展机制范例进行至关重要的测试。