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We map the kinematics of stars in simulated galaxy disks with spiral armsusing the velocity ellipsoid vertex deviation (l$_v$). We use test particlesimulations, and for the first time, fully self-consistent high resolutionN-body models. We compare our maps with the Tight Winding Approximation modelanalytical predictions. We see that for all barred models spiral arms rotateclosely to a rigid body manner and the vertex deviation values correlate withthe density peaks position bounded by overdense and underdense regions. In suchcases, vertex deviation sign changes from negative to positive when crossingthe spiral arms in the direction of disk rotation, in regions where the spiralarms are in between corotation (CR) and the Outer Lindblad Resonance (OLR). Bycontrast, when the arm sections are inside the CR and outside the OLR, l$_v$changes from negative to positive.We propose that measurements of the vertexdeviations pattern can be used to trace the position of the main resonances ofthe spiral arms. We propose that this technique might exploit future data fromGaia and APOGEE surveys. For unbarred N-body simulations with spiral armscorotating with disk material at all radii, our analysis suggests that no clearcorrelation exists between l$_v$ and density structures.

A novel method to bracket the corotation radius in galaxy disks: vertex deviation maps