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The age-metallicity relation is fundamental to study the formation andevolution of the disk. Observations have shown that this relation has a largescatter which can not be explained by observational errors only. That scatteris hence attributed to the effects of radial migration in which stars tracingdifferent chemical evolution histories in the disk get mixed. However, therecent study of Nissen et al. 2020, using high precision observational data ofsolar type stars, found two relatively tight age-metallicity relations. Onesequence of older and metal-richer stars probably traces the chemicalenrichment history of the inner disk while the other sequence of younger andmetal-poorer stars the chemical enrichment history of the outer disk. Ifuncertainties in age measurements increase, these sequences mix explaining thescatter of the one relation observed in other studies. This work follows up onthese results, by analysing an independent sample of red clump giants observedby APOGEE. Since ages for red giants are significantly more uncertain, the[C/N] ratios are considered as a proxy for age. This larger dataset is used toinvestigate these relations at different Galactic radii, finding that thesedistinct sequences exist only in the solar neighbourhood. The APOGEE dataset isfurther used to explore different abundance and kinematical planes to shedlight on the nature of these populations.

Two sequences in the age-metallicity relation as seen from [C/N] abundances in APOGEE