An Observational Study of Galaxy Properties in the Early Universe

早期宇宙星系特性的观测研究

• 批准号: 15540228
• 负责人: SHIMASAKU Kazuhiro
• 金额: $ 1.47万
• 依托单位: The University of Tokyo
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (C)
• 财政年份: 2003
• 资助国家: 日本
• 起止时间: 2003 至 2004
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-15540228/
• 关键词: galaxies; large-scale structure of the universe; early universe; galaxy evolution; 遠方宇宙

How galaxies formed and evolved is one of the fundamental issues in modern astronomy. To address this, issue, it is essential to observe very distant galaxies (i.e., galaxies in very early universes). The purpose of this research is to detect a large number of galaxies at redshift >5 using the 8.2m Subaru Telescope and study the statistical properties (such as luminosity function and spatial clustering) of very distant galaxies. The age of the universe at z=5 is 1.2 Giga years old, which is less than 10% of the current age, 14 Giga years.We made deep imaging observations in a blank field called ‘'Subaru Deep Field' in a number of bandpasses with a wide-field prime-focus camera on the Subaru Telescope, to select about 2000 galaxies over a redshift range of z=4-6. We found that the number density of bright galaxies increases by an order of magnitude from z=6 to z=4. This implies that we have located the era of the intense formation of massive galaxies. We infer that these bright galaxies are progenitors of galaxies seen in present-day galaxy groups and clusters. We also found in our sample that galaxies are distributed quite inhomogeneously in space, forming large-scale structures. This discovery is important in discussing the formation history of large-scale structure commonly seen in the present-day universe. Finally, we studied the photometric properties of red galaxies at redshift 1-2 using optical and infrared data and discussed their evolution in number density and color.

星系如何形成和演化是现代天文学的基本问题之一。为了解决这个问题，观测非常遥远的星系（即，早期宇宙中的星系）。本研究的目的是利用8.2米的斯巴鲁望远镜探测大量红移>5的星系，并研究非常遥远星系的统计性质（如光度函数和空间聚类）。宇宙在z=5时的年龄是1.2Giga，不到当前年龄14 Giga的10%。我们用斯巴鲁望远镜上的宽视场主焦点相机在一个称为“斯巴鲁深场”的空白场中进行了多次带通的深成像观测，选择了z=4-6的红移范围内的大约2000个星系。我们发现明亮星系的数密度从z=6到z=4增加了一个数量级。这意味着我们已经定位了大质量星系激烈形成的时代。我们推断，这些明亮的星系是在今天的星系群和星系团中看到的星系的祖先。在我们的样本中，我们还发现星系在空间中分布非常不均匀，形成了大尺度结构。这一发现对于讨论当今宇宙中常见的大尺度结构的形成历史具有重要意义。最后，我们利用光学和红外观测数据研究了红移1-2的红星系的光度性质，讨论了它们的数密度和颜色演化。

项目成果

Miyazaki, My Shimasaku, K., Okamura, S. et al.: "Evolution of Elliptical Galaxies at Z【greater than or similar】1 Revealed from a Large, Multicolor Sample of Extremely Red Objects"Publications of the Astronomical Society of Japan. 55. 1079-1103 (2003)

Miyazaki、My Shimasaku, K.、Okamura, S. 等人：“从极红色天体的大型多色样本中揭示 Z【大于或相似】1 处椭圆星系的演化”日本天文学会出版物。 55. 1079-1103 (2003)

Subaru Deep Survey. VI. A Census of Lyman Break Galaxies at z【similar or equal】4 and 5 in the Subaru Deep Fields : Clustering Properties

斯巴鲁深部巡天 VI。斯巴鲁深部区域中 z【相似或相等】4 和 5 处的莱曼裂痕星系的普查：聚类属性

• 发表时间: 2004
• 期刊: Astrophysical Journal 611
• 作者: Ouchi;M.
• 通讯作者: M.

Hamaya, T., Shimasaku, K.et al.: "Properties of host haloes of Lyman-break Galaxies and Lyman α Emitters from their Number Densities and Angular Clustering"Monthly Notices of the Royal Astronomical Society. 347. 813-823 (2004)

Hamaya, T., Shimasaku, K.等人：“莱曼断裂星系和莱曼 α 发射体的数量密度和角聚类的主晕属性”皇家天文学会月刊 347. 813-823 (2004)。 ）

Properties of host halos of Lyman-break galaxies and Lyman alpha emitters from their number densities and angular clustering

莱曼断裂星系和莱曼 α 发射体的主晕的属性（来自其数量密度和角聚类）

• 发表时间: 2003
• 期刊: Monthly Notices of the Royal Astronomical Society 347
• 作者: Hamana;T. et al.
• 通讯作者: T. et al.

Evolution of Elliptical Galaxies at z 1 Revealed from a Large, Multicolor Sample of Extremely Red Objects ∗

• DOI: 10.1093/pasj/55.6.1079
• 发表时间: 2002-10
• 期刊: Publications of the Astronomical Society of Japan
• 影响因子: 2.3
• 作者: Masayuki Miyazaki;K. Shimasaku;T. Kodama;S. Okamura;H. Furusawa;M. Ouchi;F. Nakata;M. Doi;M. Hamabe;M. Kimura;Y. Komiyama;S. Miyazaki;C. Nagashima;T. Nagata;T. Nagayama;Y. Nakajima;H. Nakaya;A. Pickles;S. Sato;K. Sekiguchi;M. Sekiguchi;K. Sugitani;T. Takata;Motohide Tamura;M. Yagi;N. Yasuda