Results from the V − I versus I CMD analyses of DG-5 (left) and DG-22 (right): solved SFH from the synthetic CMD method using 357 SSPs (in black) compared with the simulation star-particle data (in red) for the simulated dwarf galaxies DG-5 and DG-22 (see Table 1 for more details). Panels a: SFR as a function of the lookback time; panels b: cumulative mass fraction; and panels c: AMR. The gray points in the AMR depict the age bins where less than 1% of the total star formation took place, the black and gray lines show the error on the solved metallicity, and the scattered red points in the AMR show the true metallicities of each of the star particles in various age bins.