Zoom onto the MatisseGauguin Kiel diagram for stars in a very restricted metallicity domain, −0.05 < [M/H] < 0.00 dex, and with high-quality spectra. The RGB and AGB sequences appear as two resolved parallel tracks. The very close-by RGB bump and HB clump are also isolated. A sequence of young stars (with ages of less than ∼1 Gyr) can be identified in the hotter side, with an overdensity at around T_eff ∼ 5000 K. These are second red clump objects, i.e. massive stars burning He in their core.