An observational program is described which has as its goal a high resolution, three-dimensional survey of the dust component of the interstellar medium in the solar neighborhood. A network of approx.3450 bright A and F stars was established in the northern hemisphere with the intent that the stars act as probes for the detection of interstellar reddening. In conjunction with empirical calibrations by Crawford, uupsilonby..beta.. photometries yielded precise intrinsic colors and absolute magnitudes that, in turn, allowed the determination of the color excess and the position of each star in a rectangular coordinate system centered on the Sun. The results are summarized in a series of plots where several dust concentrations are readily apparent. In order of galactic longitude, these regions correspond to the inner portions of the Ophiuchus, Cepheus, and Taurus cloud complexes. A bridge of absorbing material, passing through Cassiopeia and Perseus, connects the latter two concentrations; the Ophiuchus complex extends into Aquila. These concentrations are characterized by small-scale irregularities both in density and spatial event. Comparison of the present results with previous investigations shows that this study provides a more definitive map of the spatial distribution of interstellar dust within several hundred parsecs of the Sun.