Modeling the Cosmic Melting Pots in the Outskirts of Galaxies and Galaxy Clusters

模拟星系和星系团外围的宇宙大熔炉

• 批准号: 1412768
• 负责人: Daisuke Nagai
• 金额: $ 49.4万
• 依托单位: Yale University
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2014
• 资助国家: 美国
• 起止时间: 2014-08-15 至 2018-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1412768&HistoricalAwards=false
• 关键词: Modeling; Cosmic; Melting; Pots; Outskirts

Understanding the growth of galaxies and galaxy clusters is one of the most significant outstanding problems in our knowledge of the universe. On the largest scales, the universe has a filamentary structure, with gas and dark matter interweaving in a series of threads. The gradual flow and build-up of gas along this "cosmic web" ultimately leads to the formation of protogalaxies and protoclusters. Despite this, the precise manner in which galaxies and their clusters eventually form remains poorly understood. A breakthrough step, enabled by this research, is to connect and synthesize our knowledge of the gas in the outskirts of galaxies with that in galaxy clusters.This program will address a number of critical questions regarding the structure and flow of gas by using a suite of high-resolution cosmological simulations. The PI will principally use the Adaptive Refinement Tree (ART) code, but will also compare the results of these simulations with detailed multi-wavelength observations of clusters and the circumgalactic medium. The work will lead to new insights into the baryon budgets in galaxies and clusters, the impact of galactic feedback on extended halo gas, the environmental dependence of galaxy evolution, and the quenching of star formation in galaxies. The PI will also develop a hands-on computational astrophysics curriculum to expand minority involvement in computational science, in collaboration with the Science, Technology, and Research Scholars (STARS) program at Yale University. Furthermore, the data products of the simulations will be made available via online publicly-accessible databases.

了解星系和星系簇的增长是我们对宇宙知识中最重要的问题之一。在最大的尺度上，宇宙具有丝状结构，气体和暗物质在一系列线程中交织在一起。沿着这种“宇宙网络”的逐渐流动和气体堆积最终导致了原藻和原始群体的形成。尽管如此，星系及其簇最终形成的确切方式仍然知之甚少。这项研究实现的突破性步骤是将我们对星系郊区气体的知识与星系簇中的气体联系起来。该程序将通过使用高分辨率宇宙学模拟的套件来解决有关气体结构和气流的许多关键问题。 PI将主要使用自适应改进树（ART）代码，但还将将这些模拟的结果与簇和圆形培养基的详细多波长观测值进行比较。这项工作将导致对星系和簇中的巴里昂预算的新见解，银河反馈对延长光环气体的影响，银河系进化的环境依赖性以及星系中星星形成的淬火。 PI还将开发一个动手计算天体物理学课程，以扩大与耶鲁大学的科学，技术和研究学者（Stars）计划合作的计算科学参与。此外，模拟的数据产品将通过在线公开访问数据库提供。