For the past 150 years, the prevailing view of the local Interstellar Medium (ISM) was based on a peculiarity known as the Gould's Belt 1, 2, 3, 4 , an expanding ring of young stars, gas, and dust, tilted about 20 ∘ to the Galactic plane. Still, the physical relation between local gas clouds has remained practically unknown because the distance accuracy to clouds is of the same order or larger than their sizes 5, 6, 7 . With the advent of large photometric surveys 8 and the Gaia satellite astrometric survey 9 this situation has changed 10 . Here we report the 3-D structure of all local cloud complexes. We find a narrow and coherent 2.7 kpc arrangement of dense gas in the Solar neighborhood that contains many of the clouds thought to be associated with the Gould Belt. This finding is inconsistent with the notion that these clouds are part of a ring, disputing the Gould Belt model. The new structure comprises the majority of nearby starforming regions, has an aspect ratio of about 1:20, and contains about 3 million solar masses of gas. Remarkably, the new structure appears to be undulating and its 3-D distribution is well described by a damped sinusoidal wave on the plane of the Milky Way, with an average period of about 2 kpc and a maximum amplitude of about 160 pc. Our results represent a first step in the revision of the local gas distribution and Galactic structure and offer a new, broader context to studies on the transformation of molecular gas into stars.To reveal the physical connections between clouds in the local ISM, we determined the 3-D distribution of all local clouds complexes 11 by deriving accurate distances to 380 lines of sight. The lines of sight were chosen to include not only all known local clouds 10, 12 but also potential bridges between them, as traced by lower column density gas. Figure 1 presents the distribution of lines of sight studied towards the Galactic anti-center and illustrates our overall approach. Each line of sight covers an area in the sky of about 450 arcmin 2 and includes both foreground and background stars to a particular cloud. The distances and the colors of these stars are used to compute a distance to the cloud (see the Methods section).In Figure 2 (interactive) we present the distribution of cloud distances to all of the studied lines of sight in a Cartesian XYZ frame where X increases towards the Galactic center, Y increases along the direction of rotation of the Galaxy, and Z increases upwards out of the Galactic plane. In the XY projection (a top-down view of the Galactic disk), it is clear that cloud complexes are not randomly distributed but instead tend to form elongated and relatively linear arrangements. Surprisingly, we find that one of the nearest structures, at about 300 pc from the Sun at its closest point, is exceptionally straight and narrow in the XY plane. This straight structure (1) undulates systematically in the Z-axis for about 2.7 kpc on the XY plane, (2) is co-planar for essentially its entire extent, and(3) displays radial velocities 13 indicat...