  Due to their star formation history (SFH), the stellar population in Dwarf
Galaxies (DG) is likely to have a metallicity spread which is best traced by
the morphology of the Red Giant Branch (RGB). We probe here a purely empirical
approach aimed at estimating average metallicity (Z) and Z spread by comparing
the Color-Magnitude Diagrams (CMD) of galactic Globular Clusters (GCs) with
those of two DGs: Leo A (HST data) and Phoe (VLT Fors2 data).
