论文标题
银河系的磁盘系统中的两个碳增强金属贫困星人
Two Populations of Carbon-Enhanced Metal-Poor Stars in the Disk System of the Milky Way
论文作者
论文摘要
我们介绍了来自Aaomega的Aaomega Galactic结构演化（AEGIS）调查的恒星的低分辨率（$ r \ sim 1300 $）光谱的化学分析，重点介绍了两个关键的碳增强金属损伤（CEMP）恒星（CEMP）的恒星（CEMP）的恒星（$ l_z $ l_z <$ l_z < 1000 \，$ kpc $ \，$ km $ \，$ s $^{ - 1} $）和强烈的先行（$ l_z> 1000 \，$ kpc $ \，$ km $ \，$ s $ \，$ s $^{ - 1} $）的人口。基于它们的化学和运动学特征，以及与最近文献中发现的类似人群的比较，我们将前者与源自$ gaia $ sausage或$ gaia $ gaia $ enceladus的前静脉内部人口相关联。后者的种群与金属螺旋厚盘（MWTD）有关。我们在银河系的形成历史的背景下讨论了它们的含义。
We present a chemo-dynamical analysis of low-resolution ($R \sim 1300$) spectroscopy of stars from the AAOmega Evolution of Galactic Structure (AEGIS) survey, focusing on two key populations of carbon-enhanced metal-poor (CEMP) stars within the disk system of the Milky Way: a mildly prograde population ($L_z < 1000\,$kpc$\,$km$\,$s$^{-1}$) and a strongly prograde ($L_z > 1000\,$kpc$\,$km$\,$s$^{-1}$) population. Based on their chemical and kinematic characteristics, and on comparisons with similar populations found in the recent literature, we tentatively associate the former with an ex-situ inner-halo population originating from either the $Gaia$ Sausage or $Gaia$-Enceladus. The latter population is linked to the metal-weak thick-disk (MWTD). We discuss their implications in the context of the formation history of the Milky Way.
