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

在邻近星系中的超大质量黑洞的质量与它们的宿主凸起的质量有很好的相关性。追踪这种相关性到高红移，到星系年轻时的回望时间，是非常有趣的。这样的观测为星系形成的理论模型提供了基本的限制。我们建议继续进行研究，旨在确定在许多不同的红移黑洞的质量-隆起质量的关系。在本地宇宙之外，这只能通过使用1型活动星系核的宿主星系来实现。我们已经开发了一种方法来获得光度估计的恒星核球质量的活动星系核宿主星系的光学紫外颜色的去混图像，我们现在适用于活动星系核样品在不同的红移。为了理解和控制样本选择效应和本征散射的影响，需要对样本的构造和观测过程进行建模。这一目标将通过蒙特-卡罗模拟来实现，我们已经开始为此开发工具。最后，我们还计划从空间分辨的发射线速度场确定类星体宿主的动力学质量。

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.