晕子结构对原初功率谱的下限限制
A lower bound on primordial power spectrum from halo substructure
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中文总结 AI 辅助
研究特定波长尺度原初曲率微扰对晕和次晕结构的影响，通过计算主晕演化与次晕质量函数，发现为符合观测，在\(10 - 30\)Mpc\(^{-1}\)波数处原初曲率微扰的凸起幅度需达\(10^{-9}\)或更大。
中文摘要 AI 辅助
我们研究了特定波长尺度的原初曲率微扰如何影响晕和次晕结构。本文考虑的原初功率谱具有近乎标度不变的形式，在波数\(k = \mathcal{O}(1)\)Mpc\(^{-1}\)处有截止，在更小尺度上有额外的对数正态凸起。我们计算了主晕演化以及次晕质量函数。为与恒星流和引力透镜数据的观测一致，在波数\(10 - 30\)Mpc\(^{-1}\)处应存在通常与原初曲率微扰的\(10^{-9}\)相同或更大的凸起幅度。
英文摘要
We investigate how the primordial curvature perturbation of a certain wavelength scale affects the halo and subhalo structure. Primordial power spectrum considered in this paper features a nearly scale-invariant form with a cutoff at the wavenumber $ k = \mathcal{O}(1)~$Mpc$^{-1}$ and an additional log-normal bump at smaller scales. We compute the host halo evolution, as well as the subhalo mass function. To be consistent with the observations of stellar streams and gravitational lensing data, the amplitude of the bump that is typically the same or larger than $10^{-9}$ of the primordial curvature perturbation should be present at the wavenumbers of $10$ - $30$ Mpc$^{-1}$.
