High Redshift Star Formation under Fuzzy Dark Matter Conditions

模糊暗物质（FDM）已被提出作为冷暗物质（CDM）范式的潜在替代方案，并因其能够解决CDM的许多观测问题（尖端-核心问题，缺失卫星问题等）而受到广泛关注。我们希望对FDM进行一些第一次放大模拟，以检查FDM对原始恒星形成气体中恒星形成和碎片的影响，从而研究在FDM条件下第一批恒星是如何形成的，以及与目前的CDM范式相比，FDM的独特性质如何影响这一过程。我们打算使用宇宙流体力学代码AREPO来进行这些模拟。从长远来看，这将是为了将我们的发现与可能区分FDM的观测结果联系起来，比如21厘米的全球信号和功率谱，这些信号和功率谱受最早恒星的性质、分布和初始质量函数的影响。此外，在大尺度上观察FDM影响的初步工作表明，这些早期恒星形成于丝状结构中，而不是像CDM所期望的那样形成光晕。因此，我们打算进行的更详细的工作可能会证实这一发现，并提供FDM的直接观测特征，如果JWST等新望远镜发现早期恒星形成于丝状而不是光晕。

Fuzzy Dark Matter (FDM) has been proposed as a potential alternative to the Cold Dark Matter (CDM) paradigm and has gained a lot of recent attention due to its ability to solve many observational problems with CDM (cusp-core problem, missing satellites problem, etc) . We wish to carry out some of the first zoom in simulations of FDM to examine the effects of FDM on star formation and fragmentation in the primordial star forming gas, and thereby investigate how the first stars formed under FDM conditions and how the unique properties of FDM affect this process when compared to the current CDM paradigm. We intend to use the cosmological hydrodynamics code AREPO to conduct these simulations. Long term, this would then be done with a view to linking our findings to potential observables that could distinguish FDM such as the 21-cm global signal and power spectrum, which are affected by the nature, distribution, and initial mass function of the earliest stars. Additionally, preliminary work looked at the effects of FDM on large scales suggested that these early stars formed in filamentary structures as opposed to halos as is expected to be the case CDM and so the more detailed work we intend to conduct may confirm this finding and provide a direct observational signature of FDM if new telescopes such as JWST find early stars forming in filaments rather than in halos.