After setting the offset at solar temperatures to zero, we subtracted our fits from the solar relative abundances of all stars to arrive at our final abundances. Stars with ﹩\mathrm{log}g﹩ < 3.0 were not corrected because there were too few stars in this range in our sample to determine any trends. The left column shows the full, uncorrected sample, and the right shows the sample after trend corrections were applied to dwarfs and subgiants based on the slowly rotating, high-S/N members of each group.