Abstract details

The stellar distribution on a CMD is related with the age and metallicity distribution of stars, caused itself by the star formation history (SFH). It is possible to compute the latter with a relatively high degree of accuracy from deep enough CMDs, reaching the oldest turn-offs. Most current methods are based on CMD parameterization. This allows an efficient comparison of an observed CMD with arbitrary linear combinations of similar parameterizations of simple synthetic population CMDs. Here we review this method specifically refereeing to our stellar populations and SFH computation codes IAC-star and IAC-pop and show recent results on the SFH of the dwarf galaxy of Phoenix.