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Fig. 9.


Left three panels: distribution of angular momentum Lz, sorted by relative uncertainty and depict three close in views groups of with 75 stars with mean Lz uncertainties of first 0.5%, second 5%, and third 30% in order to demonstrate the precision reached for different parallax qualities. Red is mean Lz for each star and blue their 1σ area. A white dashed line indicated the Solar angular momentum. Average parallax precisions are indicated in the top of each panel. The best precision on parallaxes also lead to the most precise Lz. The values of the least precise momenta (third panel) are significantly lower than those of the Sun, even when taking the standard deviation of the angular momentum estimates into account. Due to the selection of stars and the density structure of the disc, these stars are statistically further away and are expected to be at larger Galactic heights and closer to the Galactic centre. We note that their angular momenta are also different from the majority of stars, which have a Sun-like angular momenta, as shown in the fourth panel. For a discussion of the angular momenta of the stars in the chemodynamical context see Sect. 5.

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