Abstract
In this study we propose to constrain through the local stellar kinematics, the overall shape of the Milky Way dark matter halo. We base on the principle that the shape of the halo implies the existence of families of periodic orbits that support the triaxial shape. These groups would appear as kinematic co-mobile stars in the halo of the Galaxy. Our analysis uses simulations of the orbital structure in dark halos with different structures. We will discuss how to distinguish them from mobile groups created for accretion events in the Galaxy past.
