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Gaia data are revolutionizing our knowledge of the evolutionary history ofthe Milky Way. 3D maps of the interstellar dust provide complementaryinformation and are a tool for a wide range of uses. We aimed at building 3Dmaps of the dust in the Local arm and surrounding regions. To do so, Gaia DR2photometric data were combined with 2MASS measurements to derive extinctiontowards stars that possess accurate photometry and relative uncertainties onDR2 parallaxes smaller than 20\%. We applied to the extinctions a newhierarchical inversion algorithm adapted to large datasets and to ainhomogeneous target distribution. Each step associates regularized Bayesianinversions along radial directions and a subsequent inversion in 3D of theirresults. Each inverted distribution serves as a prior for the subsequent stepand the spatial resolution is progressively increased. We present the resulting3D distribution of the dust in a 6 x 6 x 0.8 kpc3 volume around the Sun. Itsmain features are found to be elongated along different directions that varyfrom below to above the mid-plane: the outer part of Carina-Sagittarius, mainlylocated above the mid-plane, the Local arm/Cygnus Rift around and above themid-plane and the fragmented Perseus arm are oriented close to the direction ofcircular motion. The long spur (nicknamed the split) that extends between theLocal Arm and Carina-Sagittarius, the compact near side of Carina-Sagittariusand the Cygnus Rift below the Plane are oriented along l=40 to 55 deg. Dustdensity images in vertical planes reveal in some regions a wavy pattern andshow that the solar neighborhood within 500 pc remains atypical by its extentabove and below the Plane. We show several comparisons with the locations ofmolecular clouds, HII regions, O stars and masers. The link between the dustconcentration and these tracers is markedly different from one region to theother.

Gaia-2MASS 3D maps of Galactic interstellar dust within 3 kpc