Fitting procedure for three sightlines from Schlafly et al. (2014), with a sightline from Hercules (l = 45.°1, b = 8.°9) shown in the top panel, Mon OB1 (l = 201.°4, b = 1.°1) in the middle panel, and Orion (l = 208.°4, b = −19.°6) in the bottom panel. The background grayscale shows the stacked distance–extinction posteriors for all the stars used in the fit. The most probable distance and extinction to every star are marked with red crosses. The blue line shows the typical extinction profile inferred for the sightline. Prior to the cloud distance D_C (at distance modulus μ_C), the magnitude of the extinction profile is equal to the foreground extinction, with the median foreground extinction f shown via the blue horizontal line. The probable range of distances to the cloud is shown via the inverted blue histogram at the top of each panel, with the median cloud distance marked via the blue vertical line. On either side we show the 16th and 84th percentile of the cloud distance (derived from our dynesty “chain”) via the vertical blue dashed lines. Beyond the cloud distance, the bottom and top blue lines show the 16th and 84th percentile of the Planck-based extinction toward the stars, multiplied by the median normalization factor N inferred for the sightline. The distance uncertainties do not include any systematic uncertainties, which we estimate to be 5% for this work and 10% for Schlafly et al. (2014). An interactive version of this figure showing the differences before and after Gaia is available at https://faun.rc.fas.harvard.edu/czucker/Paper_Figures/threepanel_comp.html and in the online version of the published article.

An interactive version of this figure is available in the online journal.