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Fig. 11


Kinematical properties of the local chemically defined “thick” and “thin” discs (cf. Fig. 10). Left: the Toomre diagram ( vs. V, see Feltzing et al. 2003) of Galactocentric velocities (with respect to the local standard of rest). The dashed curves indicate constant space motion. We can confirm the rotational lag of the thick disc found by numerous other studies, but find the value of this lag to be very much dependent on the exact separation between thick and thin discs in the chemical plane (ΔV ≈ 20–70 km s-1). Right: the ezmax plane used by Boeche et al. (2013a) to separate stellar populations into orbital families, indicated by the dashed lines. We will use this kinematical division in future analyses to compare with their findings.

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