arXiv 1910.005502019-10-01hep-phastro-ph.COhep-ex

用于光暗物质直接探测实验的暖暗物质门框

The Warm Dark Matter Doorframe for Light Dark Matter Direct Detection Experiments

Ran Huo, Tao Xu

备注：: 7 pages, 3 figures

摘要：

如果暗物质甚至已经与可见扇区充分热接触并且足够亮（$m_χ\lesssim\mathcal{O}(10)~\text{keV}$），则从可见扇区继承的热运动将导致显著的自由流效应，其受到结构形成约束，类似于基准热暖暗物质模型。在这里，我们确定的相互作用负责这种热接触的相互作用探测的深层地下暗物质直接探测实验。用动力学解耦技术在$m_χ$与$σ$图上详细地确定了束缚形状，并发现重铸当前的Lyman- $α$束缚给出了$m_χ\gtrsim73~\text{keV}$的约束，并且对于具有一些模型依赖性的较小截面的$σ<10^{-46}~\text{cm}^2$，它被放松到$m_χ\gtrsim35~\text{keV}$。对于光暗物质直接探测实验来说，这可以被视为一个通用的“禁止”约束，而已知的警告是，如果暗物质是具有早期玻色-爱因斯坦凝聚形式的轴子，或者如果存在自由流的布朗运动保护。

英文摘要：

If dark matter has even been in sufficient thermal contact with the visible sector and sufficiently light ($m_χ\lesssim\mathcal{O}(10)~\text{keV}$), the thermal motion inherited from the visible sector will cause significant free streaming effect which is subject to the structure formation constraint, similar to the benchmark thermal warm dark matter model. Here we identify the interaction responsible for such thermal contact to be the interaction probed by the deep underground dark matter direct detection experiments. With the kinetic decoupling technique on the $m_χ$ vs. $σ$ plot we determine the bound shape in detail, and find that recasting the current Lyman-$α$ bound gives a constraint of $m_χ\gtrsim73~\text{keV}$, and it gets relaxed to $m_χ\gtrsim35~\text{keV}$ for a smaller cross section of $σ<10^{-46}~\text{cm}^2$ with some model dependence. That can be taken as a generic ``no go'' constraint for light dark matter direct detection experiments, and the known caveats are if dark matter is axion-like with an early Bose-Einstein condensation form, or if there is Brownian motion protection of the free streaming.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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