The X-ray structure of the Perseus cluster of galaxies
The X-ray structure of the Perseus cluster of galaxies
复制标题
英仙座星系团的 X 射线结构
DOI：
10.1086/154574
复制
发表时间：
1976
期刊：
影响因子：
--
通讯作者：
J. Culhane
中科院分区：
文献类型：
--
作者：
R. S. Wolff;R. Mitchell;P. Charles;J. Culhane
英仙座星团中的x射线源已经被哥白尼卫星和哥伦比亚大学发射的探空火箭仪器研究过。对这些观测所得的空间和光谱数据进行了分析。得到的表面亮度分布表明，该源由与NGC 1275相关的致密核心和更大的发射体积组成。通过图像重建技术检查了中央核心区的结构，揭示了急剧下降的光度函数和南北延伸。核心区的发射光谱与周围区域的发射光谱相区别，发现氢柱密度为2.5 x 10的21次方/平方厘米，并将等温和绝热气体球模型进行了比较，表明至少需要两个组分才能提供x射线发射。
The X-ray source in the Perseus cluster has been studied both by the Copernicus satellite and by sounding-rocket instruments flown by Columbia University. The spatial and spectral data from these observations are examined. A surface brightness distribution is obtained which shows that the source consists of a compact core associated with NGC 1275 and a more extended emission volume. The structure of the central core region has been examined by means of an image reconstruction technique, revealing a steeply declining luminosity function and north-south elongation. The spectrum of the emission of the core region is distinguished from that of the surrounding area and found to be consistent with a hydrogen column density of 2.5 x 10 to the 21th/sq cm. A comparison between the isothermal and adiabatic gas sphere models is presented which shows the need for at least two components to provide the X-ray emission.