Abstract
Inside the Local Group, the satellite galaxies of the Milky Way don't have an isotropic distribution, instead most of them lie on structure almost perpendicular to the plane of the disk of the galaxy, called VPOS. At present there is not a theoretical model that correctly explain both the abundance and spatial distribution of these objects within the Local Group. This work presents a study, using Newtonian N-body numerical simulations, on the formation of disk satellites of the Milky Way (DoS) from accretion of dwarf galaxies that fall into the dark matter halo of the Milky Way following parabolic orbits with initial distances of 4, 2 and 1 Mpc. We analysed the morphological properties of dwarfs after 10 Gy of fall proposed for interaction with the Milky Way, the obtained spatial distributions about the plane of the host galaxy and the radial distances at which they are located. We found that, after 10 Gy of fall, the structures remain compact while keeping its spherical profile. Only associations of dwarf galaxies at distances of 1 Mpc manage to enter the halo of the Galaxy and could be considered as progenitors of DoS. This is supported by the fact that these closest associations are those that had precipitated into the halo of the Galaxy, and there are not observed associations of dwarfs at these distances, being the association 14+12 the closest to the Milky Way at 1.37 Mpc.
