As in Figure 5, but for the 22 stars of the Odenkirchen et al. (2009) sample. The membership probability criterion used here is ﹩{P}_{\mathrm{RGB}}\times {P}_{\mathrm{DDO}51}﹩, since we do not have access to the relevant spectral information to calculate ﹩{P}_{\mathrm{BS}12}﹩ or ﹩{P}_{[\mathrm{Fe}/{\rm{H}}]}﹩ for the entire sample. Panel (b) shows the 18 stars within the velocity selection box of Figure 5(a). The positions of two likely non-member stars (with ﹩{P}_{\mathrm{membership}}\lt 0.2)﹩ are shown with pentagonal “star” glyphs. One can see that the high-likelihood stars follow very closely the fit to the matched-filter map (red line).