As in Fig. 2 but considering stars with lower metallicity, that is, −0.5 ≤ [Fe/H] ≤ −0.2. Stars of higher metallicity (−0.15 ≤ [Fe/H] ≤ 0.2) are represented by grey dots in the background. Already from this plot one sees that in this sample young metal poor stars are rare while old stars are present in both metallicity bins. Stars in the core-He burning phase are shown light blue.