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Antiprotons are regarded as a powerful probe for Dark Matter (DM) indirectdetection and indeed current data from \PAMELA\ have been shown to lead tostringent constraints. However, in order to exploit theirconstraining/discovery power properly, great attention must be put into effects(linked to their propagation in the Galaxy) which may be perceived assubleading but actually prove to be quite relevant. We revisit the computationof the astrophysical background and of the DM antiproton fluxes fully includingthe effects of: diffusive reacceleration, energy losses including tertiarycomponent and solar modulation (in a force field approximation). Using theupdated proton and helium fluxes just released by the \AMS\ experiment wereevaluate the secondary astrophysical antiproton to proton ratio and itsuncertainties, and compare it with the ratio preliminarly reported by \AMS. Wefind no unambiguous evidence for a significant excess with respect toexpectations. Yet, some preference for a flatter energy dependence of thediffusion coefficient (with respect to the {\sc Med} benchmark often used inthe literature) starts to emerge. Finally, we provide a first assessment of theroom left for exotic components such as Galactic Dark Matter annihilation,deriving new stringent constraints.

A fussy revisitation of antiprotons as a tool for Dark Matter searches