Two Populations of Carbon-Enhanced Metal-Poor Stars in the Disk System
  of the Milky Way
  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.
