Fig. 2.
Observational properties (Teff and νmax, where 
, see Sect. 3) of stars with −0.15 ≤ [Fe/H] ≤ 0.2 in different age bins. Stars in the core-He burning phase are depicted in red. Age increases from left to right, where one notices how young stars populate almost exclusively the secondary clump. Age is inferred using the method described in Sect. 3.
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