arXiv 1910.143662019-10-31astro-ph.GAhep-ph

根据最近观测确定暗物质局域密度

Dark matter local density determination based on recent observations

Pablo F. de Salas

备注：: To appear in TAUP2019 proceedings at Journal of Physics: Conference Series
DOI：: 10.1088/1742-6596/1468/1/012020

摘要：

暗物质的局域密度是一个重要的量。一方面，它的价值是暗物质直接探测搜索所需要的。另一方面，对局部暗物质密度的精确和可靠的测定将有助于我们了解银河系暗物质晕的形状，这在暗物质间接探测搜索以及许多天体物理学和宇宙学研究中起着重要作用。有不同的方法可用于确定当地的暗物质密度。其中，研究一组选定的示踪剂的垂直运动学或银河系的旋转曲线是常见的。最近对当地暗物质密度的估计使用了欧空局/盖亚任务进行的精确观测。然而，尽管盖亚的观测数据质量很高，但对当地暗物质密度的不同分析产生了不同的结果。在简要回顾了估计暗物质局域密度的最常用方法之后，我们在这里讨论了最近分析结果差异的不同解释。最后，我们提出了新的方法，已在文献中提出，可以帮助我们提高我们的知识，这一重要的数量。

英文摘要：

The local density of dark matter is an important quantity. On the one hand, its value is needed for dark matter direct detection searches. On the other hand, a precise and robust determination of the local dark matter density would help us learn about the shape of the dark matter halo of our Galaxy, which plays an important role in dark matter indirect detection searches, as well as in many studies in astrophysics and cosmology. There are different methods available to determine the local dark matter density. Among them, it is common to study either the vertical kinematics of a selected group of tracers or the rotation curve of the Milky Way. Recent estimates of the local dark matter density have used the precise observations conducted by the ESA/Gaia mission. However, in spite of the quality of the data released by Gaia's observations, different analyses of the local dark matter density produce dissimilar results. After a brief review of the most common methods to estimate the local density of dark matter, here we argue about different explanations for the discrepancies in the results of recent analyses. We finish by presenting new approaches that have been proposed in the literature and could help us improve our knowledge of this important quantity.

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