论文标题
银河系矮卫星的暗物质光环特性：对卫星的化学动力演变的影响，对$λ$ CDM的挑战
Dark matter halo properties of the Galactic dwarf satellites: implication for chemo-dynamical evolution of the satellites and a challenge to $Λ$CDM
论文作者
论文摘要
阐明银河矮卫星中的暗物质密度曲线不仅对于理解暗物质的精髓，而且对卫星本身的发展至关重要。在这项工作中，我们介绍了银河超品种（UFD）和弥漫性星系中暗物质密度的当前限制。将我们构建的非球体质量模型应用于25个UFD和2个漫射卫星的当前可用的运动学数据，但我们发现，尽管大多数星系对推断的暗物质密度概况均具有巨大的不确定性，但Eridanus〜II，Segue〜I，Segue〜I，Segue〜I和Willman〜1 Faver Cuspy Central 〜1 faver Cuspy Cusspy Cusspy Cusspy Cuss Press a a Beias的效果。我们将结果与平面上的模拟Subhalos在150 〜PC的暗物质密度与周围距离之间进行了比较。我们发现，最观察到的卫星和模拟的subhalos类似地分布在该平面上，除了Antlia〜2，火山口〜2和Tucana〜3，不到密度的十分之一。尽管有很大的潮汐作用，但常用的subhalo发现者检测到的Subhalos很难解释如此巨大的偏差。我们还估计了卫星的动态质量与光比，并确认该比率与恒星质量和金属性有关。图卡纳〜3在很大程度上偏离了这些关系，同时它遵循质量金属关系。这表明图卡纳〜3具有核心的暗物质光环，尽管其比率存在明显的不确定性。
Elucidating dark matter density profiles in the Galactic dwarf satellites is essential to understanding not only the quintessence of dark matter, but also the evolution of the satellites themselves. In this work, we present the current constraints on dark matter densities in the Galactic ultra-faint dwarf (UFD) and diffuse galaxies. Applying our constructed non-spherical mass models to the currently available kinematic data of the 25 UFDs and 2 diffuse satellites, we find that whereas most of the galaxies have huge uncertainties on the inferred dark matter density profiles, Eridanus~II, Segue~I, and Willman~1 favor cuspy central profiles even considering effects of a prior bias. We compare our results with the simulated subhalos on the plane between the dark matter density at 150~pc and the pericenter distance. We find that the most observed satellites and the simulated subhalos are similarly distributed on this plane, except for Antlia~2, Crater~2, and Tucana~3, which are less than one tenth of the density. Despite considerable tidal effects, the subhalos detected by commonly-used subhalo finders have difficulty in explaining such a huge deviation. We also estimate the dynamical mass-to-light ratios of the satellites and confirm the ratio is linked to stellar mass and metallicity. Tucana~3 deviates largely from these relations, while it follows the mass-metallicity relation. This indicates that Tucana~3 has a cored dark matter halo, despite a significant uncertainty in its ratios.
