Early Galaxies in Cold andWarm DarkMatter Universes

结构形成的标准范式依赖于暗物质的本质是基本冷的假设(CDM)，然而，经常倡导用来解决CDM小尺度问题的一个有趣的替代方案是热暗物质(WDM)。后者应具有不可忽略的热速度，从而导致小型结构的倾倒。据推测，这种倾销在早期被加强了。在这个项目中，我们提出了对原始暗物质晕中的非平衡分子网络、气体冷却、恒星形成、反馈效应和化学浓缩等N体流体力学专用数值模拟的精确分析。主要目标是在CDM和WDM中为第一个十亿年的早期星系形成奠定坚实的理论基础，并量化WDM造成的小范围倾倒的影响。通过对早期清洁发展机制和波分复用结构的热、化学和动力学特征进行完整的描述，将有可能量化这两种情况下的原始发光发射，并通过对宇宙再电离的预期影响对暗物质的性质施加限制。

The standard paradigm of structure formation relies on the assumption that the nature of dark matter is basically cold (CDM), however, an interesting alternative often advocated to solve CDMsmall-scale problems is warm dark matter (WDM). This latter should have a non-negligible thermal velocity which results in a dumping of small structures. Such dumping is supposedly enhanced at early times. In this project accurate analyses of dedicated numerical N-body hydrodynamical simulations including non-equilibrium molecular networks, gas cooling, star formation, feedback effects and chemical enrichment in primordial dark-matter haloes are proposed. The main goal is to lay down a solid theoretical background for early galaxy formation in the first billion year both in CDM and WDM and to quantify the effects of the small-scale dumping due toWDM. By performing a complete characterization of thermal, chemical and dynamical features of early CDM and WDM structures it will be possible to quantify primordial luminous emissions in the two scenarios and to pose limits on the dark-matter nature through the expected implications on cosmic reionization.