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Fig. 17

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The left panels show the comparison of the [Fe/H] MD (upper) and [Mg/H] MD (lower) with the thin (blue) and thick (green) discs MD in the solar neighbourhood from the study of Fuhrmann (2008). The distinction between the three populations is clear from their [Fe/H] and [Mg/H] MD in their global shapes, their mean values and the metallicity range they cover. In the middle panels the bulge [Mg/H] and [Fe/H] MD are compared to a close box model with a yield p =  −0.27 and  − 0.06 for Fe and Mg respectively (black line) and to the previous thin disc MD shifted by  + 0.35 (blue) according to the results of the Gaussian separation (see Sect. 4.2 and Table 5). The combination of these two MD convolved are compared to the observed ones (right panels) for Fe (upper) and Mg (lower). For both elements, the model MD shows a very good agreement with the observed one. A small difference (compared to the relative errors) exists on the high metallicities tails: the high metallicity tail of the Mg and Fe MD decrease more sharply than the model distributions.

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