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We analyze orbits of stars and dark matter out to three effective radii for42 galaxies formed in cosmological zoom simulations. Box orbits always dominateat the centers and $z$-tubes become important at larger radii. We connect theorbital structure to the formation histories and specific features (e.g. disk,counter-rotating core, minor axis rotation) in two-dimensional kinematic maps.Globally, fast rotating galaxies with significant recent in situ star formationare dominated by $z$-tubes. Slow rotators with recent mergers have significantbox orbit and $x$-tube components. Rotation, quantified by the$\lambda_R$-parameter often originates from streaming motion of stars on$z$-tubes but sometimes from figure rotation. The observed anti-correlation of$h_3$ and $V_0 / \sigma$ in rotating galaxies can be connected to a dissipativeformation history leading to high $z$-tube fractions. For galaxies with recentmergers in situ formed stars, accreted stars and dark matter particles populatesimilar orbits. Dark matter particles have isotropic velocity dispersions.Accreted stars are typically radially biased ($\beta \approx 0.2 - 0.4$). Insitu stars become tangentially biased (as low as $\beta \approx -1.0$) ifdissipation was relevant during the late assembly of the galaxy. We discuss therelevance of our analysis for integral field surveys and for constraininggalaxy formation models.

Stellar orbits in cosmological galaxy simulations: the connection to formation history and line-of-sight kinematics