Collaborative Research: Galactic Winds and the Multiphase Structure of the Circum-Galactic Medium

合作研究：银河风和环银河介质的多相结构

• 批准号: 2205724
• 负责人: Thomas Quinn
• 金额: $ 43.95万
• 依托单位: University of Washington
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2022
• 资助国家: 美国
• 起止时间: 2022-09-01 至 2025-08-31
• 项目状态: 未结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=2205724&HistoricalAwards=false
• 关键词: Collaborative; Research; Galactic; Winds; Multiphase

Massive galaxies are embedded in a dynamic reservoir of particles and dark matter called the circumgalactic medium (CGM). The CGM not only represents a fossil record of galaxy formation, it also continues to shape their evolution through the interaction of cool infalling gas with outflows driven by stellar winds and supernovae. This research team will develop a state-of-the-art hydrodynamic galaxy simulation code to study the complex interplay between star formation induced outflows and the CGM. Synthetic UV absorption line spectra derived from these simulations will be directly compared with Hubble Space Telescope data to advance our understanding of the structure and dynamics of the CGM. These simulations will also be used in a program for pre-majors in science from underrepresented groups. The program will introduce them to the use of computer simulations in astrophysics and encourage them to consider a technically oriented major program of study. The research team will first incorporate the PhEW (Physically Evolved Winds) sub-grid model into the hydrodynamic galaxy simulation code ChaNGa and verify its accuracy. Once validated, they will begin modeling the CGM of current epoch Milky Way-like galaxies and begin making comparisons between the synthetic UV spectra with HST data. Through a series of such simulations that systematically explore a range of evolutionary paths, the team will try to assess which aspects of the CGM's absorption line properties are robust against galaxy history and which are more directly connected to star formation. Finally, the team will explore how CGM structure is affected by PhEW as a function of galaxy mass and environment by running a simulation that evolves galaxies within a cosmological volume (Romulus25; 25 Mpc sided cube). This will allow investigations of how the simulated HST/COS spectra vary as a function of galaxy type, mass, and environment and how the CGM evolves across these parameters.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.

巨大的星系嵌入粒子和暗物质的动态储存库中，称为环星系介质（CGM）。 CGM不仅代表了星系形成的化石记录，它还通过冷却的流入气体与由恒星风和超新星驱动的流出物的相互作用继续塑造星系的演化。该研究小组将开发最先进的流体动力学星系模拟代码，以研究恒星形成引起的流出与 CGM 之间复杂的相互作用。从这些模拟中得出的合成紫外吸收线光谱将直接与哈勃太空望远镜数据进行比较，以加深我们对 CGM 结构和动力学的理解。这些模拟还将用于针对代表性不足群体的科学专业预科课程。 该计划将向他们介绍计算机模拟在天体物理学中的应用，并鼓励他们考虑以技术为导向的主要研究计划。研究团队将首先将PhEW（物理演化风）子网格模型纳入流体动力学星系模拟代码ChaNGa中，并验证其准确性。一旦得到验证，他们将开始对当前历元类银河系星系的 CGM 进行建模，并开始将合成的紫外光谱与 HST 数据进行比较。通过一系列系统地探索一系列演化路径的模拟，该团队将尝试评估 CGM 吸收线特性的哪些方面对星系历史具有鲁棒性，哪些方面与恒星形成更直接相关。最后，该团队将通过运行在宇宙体积（Romulus25；25 Mpc 立方体）内演化星系的模拟，探索 CGM 结构如何受到 PhEW 作为星系质量和环境函数的影响。这将允许研究模拟的 HST/COS 光谱如何随着星系类型、质量和环境的变化而变化，以及 CGM 如何在这些参数上演变。该奖项反映了 NSF 的法定使命，并通过使用基金会的智力价值和更广泛的影响审查标准。