Collaborative Research: Evolution of Cosmic Structure and of the Galactic Spheroid Population

AST-1010033/1009908 Primack/Klypin宇宙中的大部分恒星质量位于银河系球状体中，其中也有超大质量黑洞（SMBH）。 这些关键结构的起源可以通过新的多波长测量观测和改进的理论的相互作用来澄清，这对于指导和解释观测至关重要。 这项研究的重点是宇宙结构的增长，以及早期有效的星星形成的两种相反的影响，以及大质量暗物质晕中这一过程的淬灭，这两种效应共同控制着蓝色和红色星系的形成。 这个项目应该区分由冷气体流入和盘不稳定性以及主要和次要合并的替代物所造成的星系球状体的形成。 这项工作还应确定核活动相对于阈值质量以上的晕中维里冲击加热的作用，区分卫星和中心淬火，并了解星星形成的关闭与球状恒星成分和SMBH的发展之间的串扰。 早期型星系形成的详细模型将与合并和其他过程的观测结果进行比较，以达到高红移，也可以详细研究附近星系的特性。 这项工作得到了最近完成和计划的后续计算机模拟的大型计划的支持，使用最新的宇宙学参数，具有高质量和空间分辨率。 更多的高分辨率流体动力学模拟将澄清星系形成过程，并允许计算运动学、光谱和图像，包括尘埃散射和吸收。 至关重要的是，模拟是“观察”的方式，准确地模仿观测的真实的星系。该小组将涉及学生从代表性不足的群体在天体物理理论研究，包括能力，以理解的影响，最新的观测。 这项工作推动了计算范围，所有的代码和输出都将提供给天体物理界。 计划中的计算机可视化将有助于理解模拟，同时使其他研究人员和公众可以访问结果。

AST-1010033/1009908Primack/KlypinThe majority of the stellar mass in the Universe lies in galactic spheroids, which also host supermassive black holes (SMBH). The origin of these key structures can be clarified through the interplay of new multi-wavelength survey observations and improved theory, essential for guiding and interpreting the observations. This research focuses on the growth of cosmic structure and on the two opposing effects of early, efficient star formation, and the quenching of this process in massive dark-matter halos, which together govern the formation of blue and red galaxies. This project should discriminate between galaxy spheroid buildup by cold gas inflows and disk instabilities and the alternative of major and minor mergers. The work should also identify the roles of nuclear activity versus virial shock heating in halos above a threshold mass, distinguish satellite from central quenching, and understand the cross-talk between the shutdown of star formation and the development of spheroidal stellar components and SMBHs. Detailed models of early-type galaxy formation will be compared with observations of mergers and other processes out to high redshifts, and also of nearby galaxies whose properties can be studied in detail. The work is supported by a large program of recently completed and planned follow-on computer simulations, using the most up-to-date cosmological parameters and having high mass and spatial resolution. Additional high-resolution hydrodynamic simulations will clarify galaxy formation processes and permit the calculation of kinematics, spectra and images, including dust scattering and absorption. It is crucial that simulations are 'observed' in ways that accurately mimic observations of real galaxies.The team will involve students from underrepresented groups in astrophysical theory research, including the ability to understand the implications of the latest observations. This work pushes the computational envelope, and all codes and outputs will be available to the astrophysical community. Planned computer visualizations will help to understand the simulations while simultaneously making the results accessible to other researchers and to the public.