Same as Figure 7 but for heavier elements and overall metallicity. The left column shows uncorrected solar relative abundances ([ϵ/H]) for stars with ﹩\mathrm{log}g\geqslant 4﹩ and the right column stars with ﹩3\leqslant \mathrm{log}g\lt 4﹩, both with S/N ≥ 100 and ﹩v\sin i\leqslant 3.0﹩ km s⁻¹. The black dashed line is a Gaussian kernel regression fit to the points and their uncertainties between the vertical dotted lines. The colored points are binary pairs in our sample, and their average slopes roughly follow the trend line. Between 6300 and 5300 K, most elements show no significant trends in abundance with respect to ﹩{T}_{\mathrm{eff}}﹩, though yttrium shows very strong correlations over the entire temperature range.