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Article Contents

ABSTRACT

1.INTRODUCTION

2.STAR FORMATION HISTORIES FROM COLOUR-MAGNITUDE DIAGRAMS: THE METHOD

2.1.Building a synthetic population

2.2.Stellar ages from a CMD

2.3.Deep is better

3.DEDUCING THE SFH: GUIDELINES

3.1.A changing landscape

3.2.To grid or not to grid

3.3.Maximum Likelihood

3.4.Wondering in the parameter space

3.5.A practical example

3.6.Uncertainties affecting the synthetic CMD procedures

3.7.Completeness

3.8.IMF

3.9.Binaries

3.10.Metallicity and metallicity spread

3.11.Helium content

3.12.Reddening and distance

3.13.Additional issues

4.STAR FORMATION HISTORIES OF RESOLVED DWARFS FROM SYNTHETIC CMD ANALYSES: RESULTS

5.CONCLUDING REMARKS

REFERENCES