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The paper presents new high angular resolution ALMA 1.3 mm dust continuumobservations of the protoplanetary system AS 209 in the Ophiuchus star formingregion. The dust continuum emission is characterized by a main central core andtwo prominent rings at $r = 75\,$au and $r = 130\,$au intervaled by two gaps atat $r = 62\,$au and $r = 103\,$au. The two gaps have different widths anddepths, with the inner one being narrower and shallower. We determined thesurface density of the millimeter dust grains using the 3D radiative transferdisk code \textsc{dali}. According to our fiducial model the inner gap ispartially filled with millimeter grains while the outer gap is largely devoidof dust. The inferred surface density is compared to 3D hydrodynamicalsimulations (FARGO-3D) of planet-disk interaction. The outer dust gap isconsistent with the presence of a giant planet ($M_{\rm planet} \sim0.8\,M_{\rm Staturn}$); the planet is responsible for the gap opening and forthe pile-up of dust at the outer edge of the planet orbit. The simulations alsoshow that the same planet can give origin to the inner gap at $r = 62\,$au. Therelative position of the two dust gaps is close to the 2:1 resonance and wehave investigated the possibility of a second planet inside the inner gap. Theresulting surface density (including location, width and depth of the two dustgaps) are in agreement with the observations. The properties of the inner gappose a strong constraint to the mass of the inner planet ($M_{\rm planet} <0.1\,M_{\rm J}$). In both scenarios (single or pair of planets), thehydrodynamical simulations suggest a very low disk viscosity ($\alpha <10^{-4}$). Given the young age of the system (0.5 - 1 Myr), this result impliesthat the formation of giant planets occurs on a timescale of $\lesssim$ 1\,Myr.

ALMA continuum observations of the protoplanetary disk AS 209. Evidence of multiple gaps opened by a single planet