  We present a new technique to determine age and metallicity of old stellar
populations (globular clusters and elliptical galaxies) using an iterative
principal component analysis on narrow band (Str\"omgren) colors. Our technique
is capable of reproducing globular cluster [Fe/H] values to 0.02 dex and CMD
ages to 1.0 Gyrs. We also present preliminary results on the application of our
technique to a sample of high mass, field ellipticals and low mass, cluster
dwarf ellipticals. We confirm the results of earlier studies which find that
globular clusters increase in metallicity with age and that age and metallicity
increase with galaxy mass. However, we find that dwarf ellipticals deviate from
the elliptical sequence by having little to no correlation between age and
metallicity.
