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Fig. 14

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Chemical abundances of red giant stars in the Galactic disc in three bins of Galactocentric radius. Top row: [α/Fe] vs. [Fe/H] diagrams for the high-resolution samples of Bensby et al. (2010); Alves-Brito et al. (2010) and Bensby et al. (2011). The authors collected high-resolution spectra and performed a manual spectroscopic analysis for their sample. Second and third rows: density plot of the chemical abundance plane in the same radiall bins for the APOGEE HQk and HQ samples, with respect to the orbital parameters (Rmed, zmax < 2 kpc) and the real-space coordinates (R, z < 2 kpc), respectively. As before, in this plot we restrict these samples to a smaller temperature range (4000 K <Teff < 5000 K), for which ASPCAP currently gives the most reliable values for the [α/Fe] abundance ratio. We confirm the result of (Bensby et al. 2011) that the radial scale length of the thick disc is much shorter than that of the thin disc: in the 11 <Rmed < 13 kpc bin, almost no stars with thick disc abundance pattern are present. Bottom row: MDFs for the three radial bins, again with respect to orbital (grey) and real-space (black) coordinates (here we are using the full temperature range of the HQ sample defined in Table 1).

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