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The satellites of the Milky Way and Andromeda represent the smallest galaxieswe can observe in our Universe. In this series of papers we aim to shed lighton their formation and evolution using cosmological hydrodynamical simulations.In this first paper we focus on the galaxy properties before accretion, bysimulating twenty seven haloes with masses between $5\times 10^8$ and $10^{10}M_\odot$. Out of this set nineteen haloes successfully form stars, while eightremain dark. The simulated galaxies match quite well present day observedscaling relations between stellar mass, size and metallicity, showing that suchrelations are in place before accretion. Our galaxies show a large variety ofstar formation histories, from extended star formation periods to singlebursts. As in more massive galaxies, large star formation bursts are connectedwith major mergers events, which greatly contribute to the overall stellar massbuild up. The intrinsic stochasticity of mergers induces a large scatter in thestellar mass halo mass relation, up to two orders of magnitude. Despite thebursty star formation history, on these mass scales baryons are veryineffective in modifying the dark matter profiles, and galaxies with a stellarmass below $\approx 10^6 M_\odot$ retain their cuspy central dark matterdistribution, very similar to results from pure N-body simulations.

The edge of galaxy formation I: formation and evolution of MW-satellites analogues before accretion