Correlations between stellar properties. All stars have been selected to be plausible RGB members (probability ﹩{P}_{\mathrm{RGB}}\gt 0.1﹩) and to have velocity uncertainties smaller than ﹩5\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩. The blue circles in all panels represent stars within ﹩10^{\prime} ﹩ of the cluster center and which are also radial velocity members (﹩| v-{v}_{\mathrm{Pal}5}| \lt 10\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩). In panels (a) and (d), we show the giant–dwarf discrimination based on the DDO 51 photometry. The dashed line shows our visually selected boundary to separate giants (below the line) from dwarfs (above the line). Panels (b) and (e) likewise show the giant–dwarf discrimination, but this time using the line index criteria of Battaglia & Starkenburg (2012; together with their boundary). As before, the dwarfs lie above the boundary. Finally, in (c) and (f), we display our selection based on our spectroscopic metallicity measurements.