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

关于星系如何在冷暗物质宇宙演化的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？这些特性在整个宇宙历史中是如何演变的？恒星和AGN如何调节星系性质的演化？数值模拟和理论模型是探索这些问题的宝贵工具，但是所涉及的巨大动态范围，以及看似合理的潜在物理的复杂性，限制了这种计算的从头开始预测能力。在达勒姆的狄拉克超级计算机和巴黎的居里上进行的Eagle模拟，产生了一群具有与观测到的非常相似的特性的星系。Eagle已经比以前的模拟项目有了巨大的进步，但是有限的数值分辨率仍然阻碍我们研究星系形成的重要方面。例如，高红移的详细特性是什么，z10，星系群是詹姆斯韦伯太空望远镜的主要目标，被认为是再电离的驱动因素，这是洛法的一个关键科学领域。模拟能否再现类银河系星系的详细特性（凸起/盘的特性、棒状的出现、恒星晕、星系卫星的特性）——这是盖亚背景下一个重要的研究领域。简单地提高分辨率不是一个选择，因为当前的代码不能扩展到当前超级计算机的数千核，也不能利用新一代的硬件加速器，如英特尔的Phi和英伟达的GPU。该项目将利用新的swift代码，该代码是由icc、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）的背景下合作开发的。swift2使用基于任务的并行性，异步通信，并旨在利用AVX，扩展到Phi和gpu正在进行中。你将为开发swift做出贡献，特别是使其适应eagle的星系形成模块。然后，您将使用新的代码以前所未有的现实主义执行单个星系和星系团的缩放模拟。将这些结果与观测结果进行比较，将为目前模拟器无法获得的小规模清洁发展机制范式提供关键的测试。

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.