Star Formation Histories of Dwarf Galaxies from the Colour-Magnitude Diagrams of Their Resolved Stellar Populations
Figure 7
Effect of different completeness limits: in Figure 7(a) the SFH is recovered using only stars brighter than . In this case, most of the information is still retrieved. In (b) this limit is lowered at as expected, most of the old star formation (older than 1 Gyr) is much more uncertain.
