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Fig. 7.

image

Upper panels: vector point diagrams, from Gaia proper motions, of stars belonging to the Mg-rich and Mg-poor sequences (left and right, respectively). Lower panels: longitudinal proper motion component versus heliocentric radial velocity of stars belonging to the Mg-rich and Mg-poor sequences (left and right, respectively). In each panel, the Spearman correlation coefficient ρs and its respective p-value are quoted. In all panels, mean error bars in proper motions and velocity are smaller than point sizes.

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