Fig. 11
As in Fig. 10, in the case of NGC 6121. In the case of V versus cU,B,I CMD, we found that rMS and bMS contain 60 ± 7% and 40 ± 8% of MS stars in panel c1), 61 ± 6% and 39 ± 7% of MS stars in panel c2), respectively. In the case of B versus (U − B) CMD, we found that rMS and bMS contain 67 ± 7% and 33 ± 10% of MS stars in panel f1), 75 ± 13% and 25 ± 14% of MS stars in panel f2), respectively.
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