Collaborative Research: The Structure and Origin of the Galactic Halo

合作研究：银河晕的结构和起源

• 批准号: 0098518
• 负责人: Edward Olszewski
• 金额: $ 18.7万
• 依托单位: University of Arizona
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2001
• 资助国家: 美国
• 起止时间: 2001-07-01 至 2005-06-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0098518&HistoricalAwards=false
• 关键词: Collaborative; Research; Structure; Origin; Galactic

AST 0098518OlszewskiThis is a collaborative research project involving scientists at 3 institutions: Dr. Edward Olszewski, at the University of Arizona, Dr. Mario Mateo, at the University of Michigan, and Dr. Heather Morrison, at Case Western Reserve University. These researchers are mapping a region of our Galaxy that was hitherto unreachable. They will complete an imaging survey that has been underway for several years, and they will carry out a comprehensive spectroscopic follow-up of halo-star candidates identified in the survey. The survey is undertaken to directly assess the degree to which accretion has formed the majority of the Galaxy's halo. The main focus of the survey is finding candidate halo stars that inhabit the outer parts of the Galactic halo. The final sample of halo stars from the survey will allow placement of strong limits on the existence of halo substructure and will very likely provide direct evidence of such structure if it comprises more than 10% to 20% of the luminous halo. A profound change is underway in how astronomers believe galaxies, such as ours, formed. Older notions of a single, monolithic collapse of the outer Galaxy on a relatively short timescale have begun to be superseded by the idea that much of the Galaxy formed from the accretion of much smaller systems over the entire age of the Universe. Most data supporting this accretion-driven model is somewhat indirect and involves expectations of sophisticated models of how galaxies form in an expanding Universe. Recently, the Sagittarius dwarf galaxy has provided strong evidence that at least part of our halo stars and clusters have come from an accreted satellite. ***

AST 0098518 Olszewski这是一个合作研究项目，涉及3个机构的科学家：亚利桑那大学的Edward Olszewski博士，密歇根大学的Mario Mateo博士和凯斯西储大学的石楠莫里森博士。 这些研究人员正在绘制银河系中一个迄今为止无法到达的区域。 他们将完成一项已经进行了几年的成像调查，并将对调查中确定的晕星候选者进行全面的光谱跟踪。 进行这项调查是为了直接评估吸积形成银河系大部分晕的程度。 调查的主要重点是寻找居住在银河系晕外部的候选晕星。 调查的最终晕星样本将允许对晕子结构的存在进行严格的限制，并且如果它包含超过10%至20%的发光晕，则很可能提供这种结构的直接证据。 天文学家对像我们这样的星系是如何形成的看法正在发生深刻的变化。 旧的观念，一个单一的，整体崩溃的外部星系在一个相对较短的时间尺度已经开始被取代的想法，大部分的银河系形成的吸积小得多的系统在整个宇宙的年龄。 大多数支持这种吸积驱动模型的数据都是间接的，涉及到星系如何在膨胀的宇宙中形成的复杂模型的期望。 最近，人马座矮星系提供了强有力的证据，证明我们的晕星和星团中至少有一部分来自吸积卫星。 ***