Galactocentric radial (V_R) and azimuthal (V_ϕ) velocity, and orbital-element properties for the newly identified N-rich stars. The color-coding of the symbols in the panels is based on their [Fe/H], while the gray background shading represents the KDE model of the overlaid points, excluding the HVNS candidates (see text). The distribution of the velocity component V_R vs. V_ϕ is shown in panel a. The blue dashed line represents the approximate region for sources with the Gaia-Enceladus-Sausage-like kinematics in V_R vs. V_ϕ, based on Belokurov et al. (2018). The area occupied by disk-like stars is also highlighted with the empty black circle. The perigalactic (b), apogalactic distances (c), and the maximum vertical excursion (d) from the Galactic plane as a function of the orbital eccentricity are shown. Black up-tick symbols mark the stars with likely chaotic behavior, i.e., those with orbits that change their direction of motion from prograde to retrograde (and vice versa) with respect to the direction of Galactic rotation, while the small, empty black concentric symbols indicate the stars with retrograde orbits. Uncertainties are shown as gray plus symbols in each panel. The large star symbols mark the two HVNS candidates assuming the Bayesian StarHorse heliocentric distance estimations, while the large hexagonal markers refer to the same stars with Bailer-Jones heliocentric distance estimations.