Notes. The first row indicates how the photo- or astrometric parallax uncertainty of the stars was treated. Hereby smoothing refers to weighting a voxel in the line of sight by the survival function of the star radial distance. The distance of the furthest point in the reconstruction is given in the second row. The dimensions of the smallest voxel are given in the third row. For the reconstruction of Sale & Magorrian (2018) the concept of voxel resolution is not readily applicable; Sale & Magorrian (2018) use 140 inducing points spanning a region for which one could evaluate the posterior mean at any point. The resolution for Green et al. (2018) and Rezaei Kh et al. (2018) is different in radial/angular direction, we report only radial resolution for Rezaei Kh et al. (2018) and both for Green et al. (2018). The fourth row provides the number of used data points. The fifth row indicates whether the power spectrum is inferred. The sixth row states which kind of correlations are assumed for the reconstruction. Whether positivity of dust density is enforced can be read in the seventh row. The second to last row states the method, with which the posterior summary statistics was calculated from the unnormalized log posterior. In the last row the data sets used for the reconstruction are listed.