论文标题
暗物质局部密度确定：最近的观察和未来前景
Dark matter local density determination: recent observations and future prospects
论文作者
论文摘要
该报告总结了估计暗物质局部密度（$ρ_ {\ mathrm {dm，\ odot}} $）方面取得的进展，这对于暗物质直接检测实验尤为重要。我们概述并比较了估计$ρ_ {\ mathrm {dm，\ odot}} $的最常见方法以及最近的研究结果，包括从ESA/Gaia卫星观察到的那些研究中受益的研究。大多数本地分析的结果在$ρ_ {\ mathrm {dm，\ odot}}} \ simeq \ text {0.4--0.6} \，\ mathrm {gev / cm^3} = \ text = \ text {0.011--016--016} \ od od，Mathrm {0.4--0.6} \ od，Mathrm {0.4--0.6} = {0.011--016} \ od，mathrm {而$ρ_{\ mathrm {dm，\ odot}} \ simeq \ text {0.3--0.5} \，\ Mathrm {gev / cm^3} = \ text = \ text {0.0088----0.013} \，pcorperred略低的范围。鉴于最近的发现，我们讨论了超越我们定义为理想星系的近似值的重要性（一个带有轴对称形状的稳态星系和整个平面上的镜子对称性），以提高$ρ_{\ mathrm {dm，\ odot}} $测量的精度。特别是，我们回顾了越来越多的证据证明银河系的当前配置中的局部不平衡和损坏的对称性，以及与重子的银河系分布相关的不确定性。最后，我们对已提出的新想法发表评论，这些想法进一步限制了$ρ_ {\ mathrm {dm，\ odot}} $的价值，其中大部分将从Gaia的最终数据发布中受益。
This report summarises progress made in estimating the local density of dark matter ($ρ_{\mathrm{DM,\odot}}$), a quantity that is especially important for dark matter direct detection experiments. We outline and compare the most common methods to estimate $ρ_{\mathrm{DM,\odot}}$ and the results from recent studies, including those that have benefited from the observations of the ESA/Gaia satellite. The result of most local analyses coincide within a range of $ρ_{\mathrm{DM,\odot}} \simeq \text{0.4--0.6}\,\mathrm{GeV/cm^3} = \text{0.011--0.016}\,\mathrm{M_\odot / pc^3}$, while a slightly lower range of $ρ_{\mathrm{DM,\odot}} \simeq \text{0.3--0.5}\,\mathrm{GeV/cm^3} = \text{0.008--0.013}\,\mathrm{M_\odot / pc^3}$ is preferred by most global studies. In light of recent discoveries, we discuss the importance of going beyond the approximations of what we define as the Ideal Galaxy (a steady-state Galaxy with axisymmetric shape and a mirror symmetry across the mid-plane) in order to improve the precision of $ρ_{\mathrm{DM,\odot}}$ measurements. In particular, we review the growing evidence for local disequilibrium and broken symmetries in the present configuration of the Milky Way, as well as uncertainties associated with the Galactic distribution of baryons. Finally, we comment on new ideas that have been proposed to further constrain the value of $ρ_{\mathrm{DM,\odot}}$, most of which would benefit from Gaia's final data release.
