tokens: projected orbital arrangements in motion in Figure 17 . Figure 5. Smoothed representation of the pole vision image of the circularized orbit distribution shown in Figure 4 (f). We subtracted the distribution expected from 39 randomly oriented orbits. Here the 39 orbits are generated, assuming a sin i uniform distribution for the inclinations, and a circular uniform distribution of the longitude of ascending node after setting e = 0 and a = const. As in Figure 4 (f), the black lines indicate the directions of the disks and the white line the direction of the Galactic plane. The two orbital disk systems are well separable (see above) but rather thick. Furthermore, the orthogonal X-shaped disk structure becomes apparent only in alternating zones in the position angle histogram (see Figure 8 ) and in Ω diagrams as well (see Figure 6 ). This leads to the fact that they cannot easily be recognized in polar diagrams as used by, e.g., Gillessen et al. ( 2017 ) in their Figure 12 or Yelda et al. ( 2014 ) in their Figure 21. In Figure 6 , we show the inclination of the stars as a function of the longitude of the ascending node Ω. The color indicates their membership in either the red or the black disk. It becomes clear that the two disks cannot easily be identified as the angular momentum vectors of the disk members point in opposite directions. Comparing Figure 8 and Figure 6 , one can also see that the two disks can be better separated by evaluation in the position angle histogram instead of evaluating the longitude of the ascending node Ω. Figure 6. The inclination as a function of the (LOAN) longitude of the ascending node Ω. However, compared to Figure 6 , the inclined and face-on representations of the disk members as shown in Figure 4 are better grouped together, because the direction of the angular momentum vector is not relevant in this representation. Here, looking at circularized orbits as described above is more successful in searching for face-on orbits that bunch close to the circumference of the sky-projected distributions as in Figures 4 (g) or (h). In Figures 7 (a) and (b), we show the inclinations of the two stellar systems. On the right-hand side of Figure 7 , we show the distribution of inclinations for all stars within the central acrseconds for which we can provide Newtonian orbital fits. In particular, the distributions for the two disks do not follow a sin i distribution as one might have expected for a fully randomized scenario. There is a clear clustering of inclinations around a mean value of ∼90° with the bulk of the higher inclined stellar orbits contained within an interval width of 50° (red disk with bulk between 80° and 130°) or even a width of only 40° (black disk with bulk between 70° and 110°). In comparison to the expected width of about 100° for a sin i distribution, this implies that the two separate disk are highly biased toward high inclinations. There are also no stars with inclinations in the intervals 0°–20°
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