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We present a new semi-analytical model of the population of satellitegalaxies of the Milky Way, aimed at estimating the effect of the spatialstructure of reionisation at galaxy scale on the properties of the satellites.In this model reionisation can be either: (A) externally-driven and uniform, or(B) internally-driven, by the most massive progenitor of the Milky-Way. In thelatter scenario the propagation of the ionisation front and photon dilutionintroduce a delay in the photo-evaporation of the outer satellites' gas withrespect to the inner satellites. As a consequence, outer satellites experiencea longer period of star formation than those in the inner halo. We use simplemodels to account for star formation, the propagation of the ionisation front,photo-evaporation and observational biases. Both scenarios yield a modelsatellite population at z=0 that matches the observed luminosity function andmass-to-light ratios. However, the predicted population for scenario (B) issignificantly more extended spatially than for scenario (A), by about 0.3 dexin distance, resulting in a much better match to the observations. The survivalof this structural signature imprinted by the local UV field duringreionisation on the radial distribution of satellites makes it a promising toolfor studying the reionisation epoch at galaxy scale in the Milky Way and nearbygalaxies resolved in stars with forthcoming large surveys. However, more workis needed to determine how the effect reported here can be disentangled fromthat of cosmic variance between different realisations of Milky Way haloes.

A signature of the internal reionisation of the Milky Way?