Red clump stars in chemical abundance space. Left: distribution of the APOGEE RC stars in the [α/Fe]-metallicity plane. The α-rich stars are highlighted manually. Middle: same stars in the [Ca/Fe]-metallicity plane. The [Ca/Fe] abundances do not have the same discriminating power as [α/Fe], which accounts for O, Mg, Si, S, and Ca for APOGEE. Right: distribution of the Gaia RC-GSP-Spec stars in the [α/Fe]-metallicity plane. The contours enclose 99%, 95%, 90%, 80%, and 50% of the sample. The Gaiaα-abundances are dominated by Ca lines and do not allow us to reliably distinguish the α-rich from the α-poor disc stars.