半解析星系小尺度结构功率谱的量化
Quantifying the power spectrum of small-scale structure in semi-analytic galaxies
摘要：
在冷暗物质（CDM）结构形成的图片，星系质量分布预测有相当数量的小尺度结构。强引力透镜已被证明是研究这种小尺度结构的有用工具。大部分的注意力都被赋予了通过透镜建模来检测单个的暗物质暗晕，但是最近的工作表明，可以使用功率谱分析来探测整个暗物质暗晕。在本文中，我们量化模拟星系的小尺度结构的功率谱，理解理论预测的目标，并设置阶段使用测量的功率谱来测试暗物质模型。我们使用一个样本的模拟星系产生的\texttt{Galacticus}半解析模型来确定的功率谱分布首先在CDM范例，然后在一个温暖的暗物质的情况下。我们发现，星系强透镜尺度（$k\sim 1$ kpc $^{-1}$）的功率谱的斜率和振幅的测量可以用来区分CDM和备用暗物质模型，特别是如果最大的subhalos可以通过引力成像直接检测。
英文摘要：
In the cold dark matter (CDM) picture of structure formation, galaxy mass distributions are predicted to have a considerable amount of structure on small scales. Strong gravitational lensing has proven to be a useful tool for studying this small-scale structure. Much of the attention has been given to detecting individual dark matter subhalos through lens modeling, but recent work has suggested that the full population of subhalos could be probed using a power spectrum analysis. In this paper we quantify the power spectrum of small-scale structure in simulated galaxies, with the goal of understanding theoretical predictions and setting the stage for using measurements of the power spectrum to test dark matter models. We use a sample of simulated galaxies generated from the \texttt{Galacticus} semi-analytic model to determine the power spectrum distribution first in the CDM paradigm and then in a warm dark matter scenario. We find that a measurement of the slope and amplitude of the power spectrum on galaxy strong lensing scales ($k\sim 1$ kpc$^{-1}$) could be used to distinguish between CDM and alternate dark matter models, especially if the most massive subhalos can be directly detected via gravitational imaging.
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