CAREER: Tracing Gaseous Galaxy Evolution and Galaxies as a Teaching Tool for Middle School and College Students

职业：追踪气态星系演化和星系作为中学生和大学生的教学工具

• 批准号: 0748334
• 负责人: Mary Putman
• 金额: $ 61.41万
• 依托单位: Regents of the University of Michigan - Ann Arbor
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2008
• 资助国家: 美国
• 起止时间: 2008-05-01 至 2008-12-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0748334&HistoricalAwards=false
• 关键词: CAREER; Tracing; Gaseous; Galaxy; Evolution

Gaseous probes of the universe can be explored in detail at low redshift and provide insight into how galaxies form and evolve throughout time. Dr. Mary Putman (University of Michigan) will address key unknowns of galaxy formation and evolution by examining gas dynamics and ionization in the Galactic halo and gas enrichment in nearby dwarf galaxies. The hot diffuse halo may still harbor a substantial amount of a galaxy's baryons and fuel galaxy disks. This halo medium can be probed with high-velocity clouds (HVCs) in the Galactic halo that show a "head-tail" structure, or a high column density head trailed by a diffuse tail. Simulations of these clouds moving through the halo will be compared to the observations, and by combining these comparisons with HVC distance constraints, the elusive density distribution, size, and mass of the diffuse Galactic halo will be probed. The origin and role of the diffuse halo will subsequently be assessed. The amount of ionizing radiation escaping from spiral galaxy disks will be investigated with H-alpha observations of Galactic halo clouds. The radiation in the Galactic halo will be investigated with H-alpha maps of HVCs at a range of distances. This will include the Magellanic Stream, a gaseous halo feature that is intriguingly bright in H-alpha emission. Gaseous flows within the building blocks of galaxies will be probed with metallicity measurements of H-II regions found in the outer gaseous disks of dwarf galaxies (well beyond an existing stellar component). This will address how dwarfs evolve and where the metals produced by the stars in these galaxies have gone.As a part of this work, Dr. Putman will extend this research on galaxy evolution to middle schools throughout the Detroit-area through presentations done by University of Michigan undergraduate and graduate students. The impact of this program is two-fold. First, middle-school students in diverse school districts will experience an engaging, interactive program designed to trigger or maintain their interest in the sciences at a key stage of their development. Second, college students, and the future science educators, will reap the benefits of service learning by being trained to do the presentations.

可以在低红移时详细探讨宇宙的气态探针，并洞悉星系如何在整个过程中形成和发展。玛丽·普特曼（Mary Putman）博士（密歇根大学）将通过检查银河系的气体动力学和电离的关键未知数，并在附近的矮人星系中的气体动力学和电离。 热弥漫性光环仍然可能拥有大量银河的重子和燃料星系磁盘。可以用银河光环中的高速云（HVC）探测该光环介质，该介质显示出“头尾”结构，或者由弥漫性尾巴尾随的高柱密度头。 将将这些云通过光环移动的模拟与观测值进行比较，通过将这些比较与HVC距离约束结合在一起，将探测出难以捉摸的密度分布，尺寸和弥漫性银河系子的质量。随后将评估弥漫性光环的起源和作用。 将研究从螺旋星系磁盘中逃脱的电离辐射量，将通过H-Alpha观察到银河系光云的观测值进行研究。银河系子中的辐射将使用HVC的H-Alpha图在一系列距离进行研究。这将包括麦哲伦流，这是一种气态光环特征，在H-Alpha发射中非常有趣。 星系块内的气态流将通过对矮星系外气态磁盘中的H-II区域的金属测量进行探测（远远超出了现有的恒星组件）。这将解决这些星系中星星中恒星生产的金属生产的位置。作为这项工作的一部分，Putman博士将通过密歇根大学大学生和研究生的演讲将有关星系进化的研究扩展到整个底特律地区的中学。该计划的影响是两个方面。首先，不同学区的中学学生将体验一项引人入胜的互动计划，旨在在其发展的关键阶段触发或保持对科学的兴趣。其次，大学生和未来的科学教育者将通过接受培训来进行演讲，从而获得服务学习的好处。