The metallicity of our program clusters on the C09 scale is plotted here against HB-type from Mackey & van den Bergh (2005). Isochrones are from Rey et al. (2001), and are separated by 1.1 Gyr from top to bottom. The oldest isochrone gives the age of clusters at R < 8 kpc (Rey et al. 2001). Pal 7 is not present in Mackey & van den Bergh (2005), so it is not plotted here. The arrows connect the position of the cluster if another [Fe/H] estimate is used, to the position determined by our metallicity scale. The other scale is H10 on the upper panel, and Appendix 1 of C09 in the lower panel. Consistent changes for both scales are those of NGC 7006, NGC 6569, and NGC 6715 which become younger, and that of NGC 6558 which becomes older. Pyxis, Terzan 3, and Lynga 7 appear only in the upper panel because they have no [Fe/H] estimates in C09. Comparing our abundances to H10 only, Lynga 7 becomes older, while the other two become younger. In fact Pyxis would now be as young as Rup106.