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Results. We illustrate our profile-fitting technique and present the K\,{\sci} velocity structure of the dense ISM along the paths to all targets. As avalidation test of the dust map, we show comparisons between distances toseveral reconstructed clouds with recent distance assignments based ondifferent techniques. Target star extinctions estimated by integration in the3D map are compared with their K\,{\sc i} 7699 A absorptions and the degree ofcorrelation is found comparable to the one between the same K\,{\sc i} line andthe total hydrogen column for stars distributed over the sky that are part of apublished high resolution survey. We show images of the updated dustdistribution in a series of vertical planes in the Galactic longitude interval150-182.5 deg and our estimated assignments of radial velocities to the opaqueregions. Most clearly defined K\,{\sc i} absorptions may be assigned to a densedust cloud between the Sun and the target star. It appeared relativelystraightforward to find a velocity pattern consistent will all absorptions andensuring coherence between adjacent lines of sight, at the exception of a fewweak lines. We compare our results with recent determinations of velocities ofseveral clouds and find good agreement. These results demonstrate that theextinction-K\,{\sc i} relationship is tight enough to allow linking the radialvelocity of the K\,{\sc i} lines to the dust clouds seen in 3D, and that theircombination may be a valuable tool in building a 3D kinetic structure of thedense ISM. We discuss limitations and perspectives for this technique.

Towards a 3D kinetic tomography of Taurus clouds: I -- Linking neutral potassium and dust