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Fig. 9


The chemical plane using “local” APOGEE HQk stars (d < 1 kpc, left) compared to the very local high-resolution HARPS FGK dwarf sample (d < 0.1 kpc, right) of Adibekyan et al. (2011). Orbits for the HARPS sample were computed in the same manner as for the APOGEE stars. Although the sampled volumes are quite different in size, the general resemblance of both plots is reassuring. Both plots exhibit the intriguing “gap” between high- and low-α population, and in both samples it is not straightfroward to explain by selection effects.

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