Notes. The first row indicates how the 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, as is described in Eq. (7). 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 theposterior mean at any point. The resolution for Green et al. (2018) contains two values because the resolution is different in radial and angular directions. The fourth row provides the number of data points used. The fifth row indicates whether or not the power spectrum is inferred. The sixth row states which kind of correlations are assumed for the reconstruction. Whether or not 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 non-normalized log posterior. In the last row the data sets used for the reconstruction are listed.