Some studies of the Milky Way halo and all studies of the thick disk populations suffer from difficulties cleanly separating out one galactic component from another. This is largely due to magnitude limitations, which produces a bias towards local solar neighborhood samples, where the separation of the thick disk from the halo populations of the Milky Way is problematic. Most studies have relied on metallicity or kinematics to attempt to disentangle halo samples from thin and thick disk samples. Using the new large data sets from the ESA Gaia mission, the NASA Kepler mission, the SDSS/APOGEE survey and knowledge of stellar interiors we explore the candidate halo and thick disk giants using Galactic position, kinematics, mass, age, and chemistry. We explore the correlations with chemical abundance ratios such as mass and [C/Fe] and how these may inform future efforts to make clean samples of Milky Way stellar components.