论文标题
将通用气体密度曲线与Galaxy簇中核心口气的X射线光度联系起来，最高为Z〜1.1
Linking a universal gas density profile to the core-excised X-ray luminosity in galaxy clusters up to z ~ 1.1
论文作者
论文摘要
我们研究了93个SZE选择的物体，研究了星系簇气体密度曲线的规律性以及与YX代理Myx的核心光度，LXC和质量之间的关系的联系。样品跨度m500 = [0.5-20] x 10e14 msun，位于红移0.05 <z <1.13。使用XMM-Newton观测值，我们得出了SZE选择系统的平均ICM密度曲线，并通过质量和红移确定其缩放。该平均轮廓的演变比自相似（A_Z = 2.09 +/- 0.02）稍强，并且对质量具有显着依赖性（A_M = 0.22 +/- 0.01）。与半径的平均缩放率的偏差表明核心区域和大容量的演变不同。我们测量固有散射的径向变化，发现红移的略微演变。 SZE选择系统的平均轮廓描述了低红移时X射线选择的系统的平均轮廓。缩放的核心特性在以后的时间呈阳性偏斜，这表明在较低的红移处中心峰值物体的发生率增加。 LXC和MYX之间的关系具有13％的固有散射。使用模拟，我们研究了选择效应，内在散射和协方差对这种关系的影响。斜率对数量之间的选择和内在散射不敏感。但是，散射非常取决于LXC和YX之间的协方差。考虑到我们使用YX代理来确定质量的情况，我们估计了相对于22％的真实质量的固有散射的上限。我们探测密度曲线的散射与LXC-M关系中的连接。我们的结果表明，ICM批量大致发展，核心区域分别演变。表示气体含量与质量的变化；并表明LXC与基础质量有着密切的关系。
We investigate the regularity of galaxy cluster gas density profiles and the link to the relation between core-excised luminosity, LXc, and mass from the Yx proxy, MYx, for 93 SZE-selected objects. The sample spans masses M500=[0.5 - 20] x 10e14 Msun, and lies at redshifts 0.05<z<1.13. Using XMM-Newton observations, we derive an average ICM density profile for the SZE-selected systems and determine its scaling with mass and redshift. This average profile evolves slightly stronger than self-similar (a_z = 2.09+/-0.02), and has significant dependence on mass (a_M = 0.22 +/- 0.01). Deviations from the average scaling with radius indicate different evolution for the core regions and the bulk. We measure the radial variation of the intrinsic scatter, finding a slight evolution with redshift. The average profile of the SZE-selected systems describes that of X-ray-selected systems at low redshift. The scaled core properties are positively skewed at later times, suggesting an increased incidence of centrally peaked objects at lower redshifts. The relation between LXc and MYx has an intrinsic scatter of 13%. Using simulations, we investigate the impact of selection effects, intrinsic scatter, and covariance on this relation. The slope is insensitive to selection and intrinsic scatter between quantities; however, the scatter is very dependent on the covariance between LXc and Yx. Accounting for our use of the Yx proxy to determine the mass, we estimate an upper limit to the intrinsic scatter with respect to the true mass of 22%. We probe the connection between the scatter in density profiles and that in the LXc-M relation. Our results suggest that the ICM bulk evolves approximately self-similarly, with the core regions evolving separately; indicate a variation of the gas content with mass; and show that LXc has a tight relation to the underlying mass.
