RUI/AAG - Studying Metals in Quasars From the Sloan Digital sky Survey: Observing Changes in Galaxy Properties Over Time via Absorption Spectra

RUI/AAG - 通过斯隆数字巡天研究类星体中的金属：通过吸收光谱观察星系特性随时间的变化

• 批准号: 1615296
• 负责人: Kathy Cooksey
• 金额: $ 13.83万
• 依托单位: University of Hawaii at Hilo
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2016
• 资助国家: 美国
• 起止时间: 2016-09-01 至 2022-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1615296&HistoricalAwards=false
• 关键词: RUI; AAG; Studying; Metals; Quasars

Part 1The proposed research aims to connect gas clouds and gaseous structures with galaxies and their change over time. The observations of elements heavier than helium in these gas clouds provides important constraints on the overall amount of these elements produced and spread through space, and the physical environments of gas clouds themselves. The proposal seeks to study a large sample of quasars from an important sky survey, using the quasars like a flash light to observe gas clouds (and their properties) between us and the more distant quasars.Part 2The large-scale gaseous structure of the Universe is affected by the production and dispersal of chemical elements by galactic processes. Quasar absorption-line (QAL) spectroscopy is a powerful tool for probing the large-scale gaseous structure and its change over time. There is an emerging consensus that strong absorption-line systems trace the extended gaseous halos of galaxies. The evidence relies on direct detections of strong absorbers near galaxies as well as absorber properties changing with galaxies. The large scale of this enriched circum-galactic medium (CGM) enables the study of galaxy formation and change with relatively little observational expense, at a wide range of redshifts. Open questions in astronomy motivate the research: What are the chemical properties of the extended gaseous halos of galaxies? Which type of absorption-line systems are associated with what class of galaxies? Where are the missing metals? Toward what galaxies are potential cold flows flowing?

第一部分：本研究的目的是将气体云和气体结构与星系及其随时间的变化联系起来。在这些气体云中比氦重的元素的观测提供了重要的限制，这些元素的总量产生和通过空间传播，以及气体云本身的物理环境。该计划旨在研究一个重要的巡天观测中的大量类星体样本，利用类星体像闪光灯一样观察我们和更遥远的类星体之间的气体云（及其性质）。第二部分宇宙的大尺度气体结构受到星系过程中化学元素的产生和扩散的影响。类星体吸收线（QAL）光谱是探测大尺度气体结构及其随时间变化的有力工具。有一个正在形成的共识，强吸收线系统跟踪星系的扩展气体晕。证据依赖于直接探测到的强吸收体附近的星系以及吸收体的性质随星系的变化。这种丰富的环银河系介质（CGM）的大尺度使研究星系的形成和变化，相对较少的观测费用，在广泛的红移。天文学中的未决问题激发了这项研究：星系扩展的气体晕的化学性质是什么？哪种类型的吸收线系统与哪类星系有关？丢失的金属在哪里？潜在的冷流流向哪个星系？