Non-linear evolution of suppressed dark matter primordial power spectra
Non-linear evolution of suppressed dark matter primordial power spectra
复制标题
抑制暗物质原初功率谱的非线性演化
DOI：
10.1111/j.1365-2966.2005.09032.x
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发表时间：
2005
影响因子：
4.8
通讯作者：
J. Silk
中科院分区：
文献类型：
--
作者：
C. Boehm;H. Mathis;J. Devriendt;J. Silk
我们研究了宇宙学结构形成过程中小尺度功率产生的程度和速度，其中原始功率谱在给定波数之外受到强烈抑制。我们首先总结了人们期望出现这种抑制功率谱的情况，并指出它们的多样性。然后，我们采用指数截止（其表征了暖暗物质（WDM）模型）作为截止形状的模板，并重点关注从 10 6 到 10 9 h -1 M ○ 的阻尼尺度。 。使用高分辨率模拟，我们表明功率谱的抑制部分快速（重新）生成，并赶上了未抑制功率谱的线性和非线性演化。从 z = 2 开始，功率谱的原始截止点为 10 9 h -1 M ○。与进化的冷暗物质（CDM）功率谱几乎无法区分。在截断功率谱的情况下，也会出现 Zaldarriaga、Scoccimarro 和 Hui 中描述的针对具有不同谱指数的功率谱的吸引子。在~ 100 h -1 kpc 下测量 z ∼ 0 非线性功率谱不能排除线性功率谱衰减低于~10 9 h -1 M ○ 的可能性。 。因此，WDM或类似特征的场景应该很难通过这种方式排除。
We address the degree and rapidity of generation of small-scale power over the course of structure formation in cosmologies where the primordial power spectrum is strongly suppressed beyond a given wavenumber. We first summarize the situations where one expects such suppressed power spectra and point out their diversity. We then employ an exponential cut-off, which characterizes warm dark matter (WDM) models, as a template for the shape of the cut-off and focus on damping scales ranging from 10 6 to 10 9 h -1 M ○. . Using high-resolution simulations, we show that the suppressed part of the power spectrum is quickly (re)generated and catches up with both the linear and the non-linear evolution of the unsuppressed power spectrum. From z = 2 onwards, a power spectrum with a primordial cut-off at 10 9 h -1 M ○. becomes virtually indistinguishable from an evolved cold dark matter (CDM) power spectrum. An attractor such as that described in Zaldarriaga, Scoccimarro & Hui for power spectra with different spectral indices also emerges in the case of truncated power spectra. Measurements of z ∼ 0 non-linear power spectra at ∼ 100 h -1 kpc cannot rule out the possibility of linear power spectra damped below ∼10 9 h -1 M ○. . Therefore, WDM or scenarios with similar features should be difficult to exclude in this way.