The cosmic evolution of the black hole mass / bulge mass ratio

附近星系中的超大质量黑洞的质量与它们所在的凸起的质量有很好的相关性。将这种关联追溯到高红移，追溯到星系年轻时的回顾时代，是非常有意义的。这样的观测为星系形成的理论模型提供了基本的约束。我们建议继续进行一项研究，以确定黑洞在许多不同红移时的质量-膨胀质量关系。在局部宇宙之外，这只能使用类型1活动星系核的宿主星系来完成。我们开发了一种方法，从解混图像中的光学-UV颜色获得AGN宿主星系的恒星膨胀质量的光度估计，现在我们将其应用于不同红移的AGN样本。为了理解和控制样本选择效应和本征散射的影响，我们需要对样本结构和观察过程进行建模。这一目标将通过蒙特卡罗模拟实现，我们已经开始为其开发工具。最后，我们还计划从空间分辨的发射线速度场中确定类星体主机的动力学质量。

The masses of supermassive black holes in nearby galaxies are well correlated with the masses of their hosting bulges. It is of great interest to follow this correlation out to high redshifts, into look-back times when galaxies were young. Such observations provide fundamental constraints on theoretical models of galaxy formation. We propose to continue a study aiming at the determination of the black hole mass - bulge mass relation at many different redshifts. Outside the local universe, this can only be done using host galaxies of type 1 Active Galactic Nuclei.We have developed a method to obtain photometric estimates of the stellar bulge masses of AGN host galaxies from optical-UV colours in the deblended images, which we now apply to AGN samples at different redshifts. In order to understand and control the influence of sample selection effects and intrinsic scatter, we need to model the sample construction and observing process. This aim will be achieved by means of Monte-Carlo simulations, for which we already started to develop the tools. Finally, we also plan to determine dynamical masses of QSO hosts from spatially resolved emission line velocity fields.