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Interplay between Star Formation & AGN Feedback in Galaxy Formation Simulations

恒星形成之间的相互作用

基本信息

批准号：
1951902
负责人：
金额：
--
依托单位：
University of Cambridge
依托单位国家：
英国
项目类别：
Studentship
财政年份：
2017
资助国家：
英国
起止时间：
2017 至无数据
项目状态：
已结题

来源：
https://gtr.ukri.org/projects?ref=studentship-1951902
关键词：
Interplay between Star Formation AGN

项目摘要

Major observational facilities, like JWST and ALMA, are dedicated to understanding the interaction between black holes and their host galaxies. In particular, the role of black holes in the formation and evolution of dwarf galaxies is hotly debated. While the ACDM model has been successful in reproducing the observed large-scale structure, discrepancies between theory and observation remain on smaller scales. For example, the theory results in a higher abundance of low-mass dwarf galaxies than has so far been observed (the missing satellite problem). In addition, the observed dark matter distribution in dwarf galaxies seems to follow a core profile rather than the cusp profile predicted by the cold dark matter model. Baryonic processes, in particular supernova feedback, are usually invoked as a solution to the above issues. However, supernova feedback might not be powerful enough for massive dwarf galaxies and getting the energetics right requires fine-tuning. Including additional baryonic processes, like AGN feedback, could resolve these problems.It is therefore timely to study the physical properties of dwarf galaxies. The aim of this project is to develop state-of-the-art numerical methods considering star formation and AGN feedback in tandem. We would like to determine whether AGN feedback could significantly affect dwarf galaxy evolution. Moreover, we would like to investigate whether our model for baryonic processes could significantly alter the distribution of dark matter. The GAIA survey may make it possible to dynamically determine the dark matter distribution of the local dwarfs providing us with valuable observational data to compare to. Investigating which physical processes shape the luminosity function of galaxies, and in particular determining whether AGN feedback also affects the low-mass end, would allow us to expand the scope of this project to the full galaxy population.

主要的观测设施，如JWST和阿尔马，致力于了解黑洞与其宿主星系之间的相互作用。特别是，黑洞在矮星系形成和演化中的作用引起了激烈的争论。虽然ACDM模型成功地再现了观测到的大尺度结构，但理论和观测之间的差异仍然存在于较小的尺度上。例如，该理论导致低质量矮星系的丰度比迄今为止观察到的要高（丢失卫星问题）。此外，观测到的暗物质在矮星系中的分布似乎遵循核心轮廓，而不是冷暗物质模型预测的尖点轮廓。重子过程，特别是超新星反馈，通常被用来解决上述问题。然而，超新星的反馈对于大质量矮星系来说可能不够强大，并且需要进行微调才能获得正确的能量。如果加入额外的重子过程，如活动星系核的反馈，就可以解决这些问题，因此研究矮星系的物理性质是及时的。这个项目的目的是发展最先进的数值方法，考虑到星星的形成和活动星系核的反馈串联。我们想确定活动星系核的反馈是否会显著影响矮星系的演化。此外，我们还想研究我们的重子过程模型是否能显著改变暗物质的分布。GAIA的调查可能使我们有可能动态地确定当地矮星的暗物质分布，为我们提供有价值的观测数据进行比较。调查哪些物理过程塑造了星系的光度函数，特别是确定AGN反馈是否也影响低质量端，将使我们能够将该项目的范围扩展到整个星系群。