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Precise Measurements of the Hubble Constant and Structures of Clusters of Galaxies

哈勃常数和星系团结构的精确测量

基本信息

批准号：
14540230
负责人：
MIYOSHI Shigeru
金额：
$ 1.66万
依托单位：
Kyoto Sangyo University
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (C)
财政年份：
2002
资助国家：
日本
起止时间：
2002 至 2004
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-14540230/
关键词：
clusters of galaxies high temperature plasma Sunvaev-Zel'dovich effect Hubble constant dark matter density fluctuation gravitational lensing density distribution 密度ゆらぎ X線天文学天体プラズマ宇宙膨張 X線表面輝度分布ダークマター等温ベータモデル

项目摘要

On the theoretical and observational investigations of the structure of clusters of galaxies, we established a new model of intracluster gas distribution. The fitting of our model with observational data is considerably better than the isothermal beta model, and the cluster mass distribution derived by using our model has a tendency to solve the discrepancy between the values obtained from the X-ray and the gravitational-lensing data. We made also the analysis of X-ray data of A2029 obtained with XMM-Newton. A2029 is a typical cD-type cluster of galaxies having a giant cD galaxy in the center. Although the data analysis of this cluster is still going on, many interesting results have been obtained. For example, in the central region a two-temperature model is preferred to some ordinary single temperature models.On the measurement of the Hubble constant, Ho, using the Sunyaev-Zel'dovich effect, we succeeded to obtain available data for five distant (0.143【less than or equal】z【less than or equal】0.282) clusters of galaxies observed with ROSAT, ASCA (X-ray) and the Ryle Telescope (radio). The obtained value of Ho for these clusters are considerably scattered, and their mean value is 66+11/-10 (random) +9/-8 (systematic) km/s/Mpc for a ACDM (ΩM=0.3, ΩA=0.7) flat universe. This value of Ho is slightly less than the value of Ho=71±2 km/s/Mpc obtained from WMAP observations of the cosmic microwave background radiation, but they are in good agreement within their errors.

通过对星系团结构的理论和观测研究，我们建立了星系团内气体分布的新模型。我们的模型与观测数据的拟合比等温β模型好得多，并且使用我们的模型导出的星系团质量分布有解决从X射线和引力透镜数据获得的值之间的差异的趋势。本文还对A2029的XMM-牛顿法X射线数据进行了分析。A2029是一个典型的cD型星系团，中心有一个巨大的cD星系。虽然对这一聚类的数据分析仍在进行中，但已经获得了许多有趣的结果。在利用Sunyaev-Zel'dovich效应测量Hubble常数Ho时，我们成功地获得了ROSAT、ASCA（X射线）和Ryle望远镜（射电）观测到的5个（0.143[小于或等于]z[小于或等于]0.282）星系团的有效数据。在ACDM（ΩM=0.3，ΩA=0.7）平坦宇宙中，它们的平均值为66+11/-10（随机）+9/-8（系统）km/s/Mpc。这个Ho值略小于WMAP宇宙微波背景辐射观测得到的Ho=71±2 km/s/Mpc，但在误差范围内，两者吻合得很好。