the frequency of carbon-enhanced metal-poor (CEMP) stars below this value is around 75%. We also examine how the cumulative frequency of CEMP stars varies across different luminosity classes. The giant sample exhibits a cumulative CEMP frequency of 32% for [\[Fe/H\]]{} $\leq -2.5$, 31% for [\[Fe/H\]]{} $\leq
    -3.0$, and 33% for [\[Fe/H\]]{} $\leq -3.5$; a roughly constant value. For the main-sequence turnoff stars, we obtain a lower cumulative CEMP frequency, around 10% for [\[Fe/H\]]{} $\leq -2.5$, presumably due to the difficulty of identifying CEMP stars among warmer turnoff stars with weak CH $G$-bands. The dwarf population displays a large change in the cumulative frequency for CEMP stars below \[Fe/H\] = –2.5, jumping from 15% for [\[Fe/H\]]{} $\leq -2.5$ to about 75% for [\[Fe/H\]]{} $\leq
    -3.0$. When we impose a restriction with respect to distance from the Galactic mid-plane ($|Z| < 5$ kpc), the frequency of the CEMP giants does not increase at low metallicity ([\[Fe/H\]]{} $<-2.5$), but rather, decreases, due to the dilution of C-rich material in stars that have undergone mixing with CNO-processed material from their interiors. The frequency of CEMP stars near the main-sequence turnoff, which are not expected to have experienced mixing, increases for [\[Fe/H\]]{} $\leq -3.0$. The 