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Fig. 17.


Distribution of the sample stars in the R − z plane (top left) as well as the three actions JR − Jz (top right), JR − Jϕ = Lz (bottom left), and Jz − Lz (bottom right). With exception of the top left panel (coloured by parallax precision), colour indicates the number of stars per bin in each panel, with a lower limit of five stars per bin. Individual stars outside the bins are shown as black dots. Top left panel: increasing distance from the Sun, the parallax precision decreases. It also shows that with the exception of two special pointings, the Galactic plane (|b| < 10 deg) is neglected by GALAH. The individual action angle plots show that most of the stars move on circular orbits with solar Galactocentric orbit and angular momentum. Top right corner: decreasing density with a diagonal pattern up to a line which intercepts with JR at 150 kpc km s−1 and Jz at 20 kpc km s−1 and with only few stars with larger actions. The JR − Lz shows trends of a minority of stars to be on eccentric orbits which have their apocentre in the solar neighbourhood (sub-solar Lz and increased JR) or eccentric orbits with pericentres in the solar vicinity (super-solar Lz and increased JR). While stars do not show increased vertical actions in the Jz − Lz plane (bottom right), an increase vertical actions can be seen for stars with solar angular momentum.

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