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The "Disk of satellites" (DoS) around Milky Way is a highly debated topicwith conflicting interpretations of observations and their theoretical models.We perform a comprehensive analysis of all dwarfs detected in the Milky Way andfind that the DoS structure depends strongly on the plane identification methodand the sample size. In particular, we demonstrate that a smaller sample sizeproduces a higher anisotropy of the spatial distribution and a strongerclustering of the angular momentum of the satellites. Moreover, we calculatethe evolution of the 11 classical satellites with proper motion measurementsand find that the thin DoS they currently reside in is transient. Furthermore,we analyze two cosmological simulations using the same initial conditions of aMilky Way-sized galaxy, an N-body run with dark matter only and a hydrodynamicone with both baryonic and dark matter, and find that the hydrodynamicsimulation produces more anisotropic distribution of satellites than the N-bodyone. Our results suggest that an anisotropic distribution of satellites ingalaxies can originate from baryonic processes in the hierarchical structureformation model, but the claimed highly-flattened, coherently-rotating DoS ofthe Milky Way may be a small-number selection effect. These findings may helpresolve the contradictory claims of DoS in other galaxies and the discrepancyamong numerical simulations.

Is there a disk of satellites around the Milky Way?