论文标题
在银河系中心测试模糊暗物质理论的预测
Testing the Prediction of Fuzzy Dark Matter Theory in the Milky Way Center
论文作者
论文摘要
模糊的暗物质模型（FDM，也称为量子波暗物质模型）认为，质量为$ \ sim10^{ - 22} {\; {\ rm ev}} $的光玻色子是宇宙中暗物质的候选者。 FDM最重要的预测之一是形成孤子芯，而不是星系中心的密度尖端。如果FDM是暗物质的正确理论，那么预测的孤子核可以帮助以银河系形成中央分子区（CMZ）。我们提出了气流模式的高分辨率流体力学模拟，以基于现实的银河系潜力来限制孤子核的特性。我们发现需要一个密集的中心才能形成合理的CMZ。 CMZ的大小和运动学对银河系内封闭的质量轮廓提供了相对较强的约束。如果不考虑孤子芯，则单独的紧凑型核凸块具有径向变化的质量与光比可以与观察到的CMZ的大小和运动学相匹配。一个质量为$ \ oft4.0 \ times10^8 {\; {\ rm m} _ {\ odot}} $和$ \ of of loct of0.05 {\; {\ rm kpc}} $的核心半径，加上较小的核凸起，较小的核凸起，并且恒定的质量与光比也同意当前数据。这样的FDM Soliton Core对应于$ \ sim2-7 \ times10^{ - 22} {\; {\ rm ev}} $的玻色子质量，可以通过改进的银河系中心的质量与光比的确定进一步限制。
The fuzzy dark matter model (FDM, also known as quantum wave dark matter model) argues that light bosons with a mass of $\sim10^{-22}{\;{\rm eV}}$ are a possible candidate for dark matter in the Universe. One of the most important predictions of FDM is the formation of a soliton core instead of a density cusp at the center of galaxies. If FDM is the correct theory of dark matter, then the predicted soliton core can help to form the Central Molecular Zone (CMZ) in the Milky Way. We present high-resolution hydrodynamical simulations of gas flow patterns to constrain the properties of the soliton core based on a realistic Milky Way potential. We find that a dense center is required to form a reasonable CMZ. The size and kinematics of the CMZ offer a relatively strong constraint on the inner enclosed mass profile of the Galaxy. If a soliton core is not considered, a compact nuclear bulge alone with a radially varying mass-to-light ratio can match the observed size and kinematics of the CMZ. A soliton core model with a mass of $\approx4.0\times10^8{\; {\rm M}_{\odot}}$ and a core radius of $\approx0.05{\;{\rm kpc}}$, together with a less massive nuclear bulge with a constant mass-to-light ratio, also agrees nicely with the current data. Such a FDM soliton core corresponds to a boson mass of $\sim2-7\times10^{-22}{\;{\rm eV}}$, which could be further constrained by the improved determination of the mass-to-light ratio in the Galactic center.
