do not adjust their Rb abundances. @abia01 adopt a Rb $gf$ value that differs from ours, so we adjust their Rb abundances by +0.08 dex. It is not clear what Rb $gf$ was used by @gonzalez98. Fortunately, Arcturus was also part of their sample. They derived an abundance \[Rb/H\] = $-$0.45 and so we adjust their Rb abundances by $-$0.1 dex. @smith00 find \[Rb/H\] = $-$0.52 and so we do not adjust their Rb abundances.

Lead abundances
---------------

The Pb abundances were determined via spectrum synthesis of the Pb[i]{} line near 4058 Å (see Figures \[fig:b708\_pb\] and \[fig:m13\_l973\_pb\]). Abundances from the Pb line near 3683 Å could not be determined due to the lack of flux in the blue for these cool giants. While the region centered near 4058 Å is crowded with molecular lines of CH as well as atomic lines from Mg, Ti, Mn, Fe, and Co, our syntheses provide a very good fit to the region demonstrating that reliable Pb abundances can be extracted. The macroturbulent broadening was estimated by fitting the profiles of the nearby lines. We adopted the same $gf$ value used by @aoki00 [@aoki01; @aoki02]. Following @aoki02, our synthesis accounted for the hyperfine and 