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The Local Group of galaxies offer some of the most discriminating tests ofmodels of cosmic structure formation. For example, observations of the MilkyWay (MW) and Andromeda satellite populations appear to be in disagreement withN-body simulations of the "Lambda Cold Dark Matter" ({\Lambda}CDM) model: thereare far fewer satellite galaxies than substructures in cold dark matter halos(the "missing satellites" problem); dwarf galaxies seem to avoid the mostmassive substructures (the "too-big-to-fail" problem); and the brightestsatellites appear to orbit their host galaxies on a thin plane (the "planes ofsatellites" problem). Here we present results from APOSTLE (A Project OfSimulating The Local Environment), a suite of cosmological hydrodynamicsimulations of twelve volumes selected to match the kinematics of the LocalGroup (LG) members. Applying the Eagle code to the LG environment, we find thatour simulations match the observed abundance of LG galaxies, including thesatellite galaxies of the MW and Andromeda. Due to changes to the structure ofhalos and the evolution in the LG environment, the simulations reproduce theobserved relation between stellar mass and velocity dispersion of individualdwarf spheroidal galaxies without necessitating the formation of cores in theirdark matter profiles. Satellite systems form with a range of spatialanisotropies, including one similar to that of the MW, confirming that such aconfiguration is not unexpected in {\Lambda}CDM. Finally, based on the observedvelocity dispersion, size, and stellar mass, we provide new estimates of themaximum circular velocity for the halos of nine MW dwarf spheroidals.

The APOSTLE simulations: solutions to the Local Group's cosmic puzzles