Fig. 7
Left panel: logarithmically-scaled, binned CMD used in the maximum-likelihood fit for SFH; right panel: best-fit model. Without differential reddening, there is clear separation between the MS and BL stars, which are mingled together in the data. The AGB stands out as being poorly-fit; the mismatch occurs because of the large number of stars fainter than m814 ≈ 26, which are part of the same stellar population as the AGB stars.
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