Large-Scale Structure in the Local Universe

本地宇宙中的大尺度结构

• 批准号: 8715260
• 负责人: Alan Dressler
• 金额: $ 12.29万
• 依托单位: Carnegie Institution of Washington
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 1988
• 资助国家: 美国
• 起止时间: 1988-07-01 至 1992-06-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=8715260&HistoricalAwards=false
• 关键词: Large; Scale; Structure; Local; Universe

Studies of large-scale structure of the universe are providing, at the present time, the strongest constraints on models of the early universe. There is good evidence for complex structure on the scale of 30 to 60 million light years that may be compatible with current models, however, the larger 150 to 300 million light year structures, still controversial, pose a much greater difficulty. A chief ambiguity in interpretation is that galaxy distributions may present a biased mapping of the distribution of mass. However, velocity mapping - measuring deviations from a smooth Hubble flow - makes it possible to infer all the mass and allows simple comparison with theory and model simulations. Three programs that follow from the mapping of the local Hubble flow with elliptical galaxies will be carried out. The original study found a large-scale flow pattern pointing toward the intersection of the galactic and supergalactic planes. One of the programs is a redshift survey to map the "Great Attractor", an enormous overdensity in the galaxy distribution that may be responsible for the flow pattern. The second program is to carry out more measurements of deviations from pure Hubble flow in this direction by finding distances to elliptical and spherical galaxies using a distance relation and by infering distances to spiral galaxies with the (optical) Tully-Fisher relation. The third program is a further investigation of the suitability of the distance relation to measurement of the Hubble constant. The Hubble constant provides a relation between the redshift and the distance of a galaxy.

对宇宙大尺度结构的研究提供了， 目前，对早期模型的约束最强 宇宙 有很好的证据表明， 3000万到6000万光年的尺度，可能与 然而，目前的模型，更大的1.5亿至3亿光年， 仍然有争议的结构造成了更大的困难。 解释中的一个主要模糊之处是星系分布 可能呈现出质量分布的偏差映射。 然而，速度映射-测量与平滑 哈勃流-使得推断所有的质量成为可能， 与理论和模型模拟的简单比较。 三个程序，从当地的哈勃映射遵循 与椭圆星系的流动将进行。 原始 研究发现了一种大规模的流动模式， 银河系和超银河系平面的交叉点。 之一 计划是一个红移调查，以绘制“伟大的吸引力”， 星系分布中的巨大密度 负责流动模式。 第二个方案是携带 更多的测量偏离纯哈勃流在这一点上， 通过查找到椭圆和球面的距离来确定方向 星系使用距离关系和推断距离， 螺旋星系与（光学）塔利-费舍尔关系。 的 第三个程序是进一步调查的适用性， 距离与哈勃常数的测量有关。 的 哈勃常数提供了红移和 一个星系的距离