Stellar Dynamics in Galaxies and Galaxy Clusters

我们将研究与宇宙学有关的各种恒星动力学问题。基于最大熵轨道的星系模型技术将被用来重新确定椭圆星系中的质光比(M/L)。将开发方法来尝试解决椭圆体中的速度弥散张量是否随着半径的增大而变得更加相切，或者椭圆体是否具有巨大的光晕。考虑到(被忽略的)存在不同分量的真实内部失调的可能性，我们将探索具有扭曲等光线的恒星系统的动力学。最近的结果表明星系核中有非常大的M/L，这些结果的动力学后果将被研究。通过将暗物质与星系分开处理，以前关于星系团形成的工作将扩展到不同的宇宙学。这些数值模拟的目的将是探索星系团形成和演化过程中暗物质和发光物质的分离，更好地了解星系团轮廓是否可以用来估计宇宙的质量密度，研究盘状星系的形成和星系质量和光度函数的演化，并试图了解亚星系团是否可以用作宇宙学探测器。

A variety of stellar dynamical problems which bear on cosmology will be investigated. A maximum entropy - orbit based galaxy modelling technique will be used to redetermine mass to light ratios (M/L's) in elliptical galaxies. Methods will be developed to attempt to resolve whether the velocity dispersion tensor in ellipticals becomes more tangential with increasing radius, or whether the ellipticals have massive halos. The dynamics of stellar systems with twisted isophotes will be explored considering the (neglected) possibility that there are real internal misalignments of different components. The dynamical consequences of the recent results indicating very large M/L's in galactic nuclei will be studied. Previous work on the formation of clusters will be extended to different cosmologies by treating the dark matter separately from the galaxies. The purpose of these numerical simulations will be to explore the separation of dark matter from luminous matter during cluster formation and evolution, to understand better whether cluster profiles can be used to estimate the mass density of the Universe, to study the formation of disk galaxies and the evolution of galaxy mass and luminosity functions, and to attempt to understand whether subclustering can be used as a cosmological probe.