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tokens: ) multi-redshift sample used Spitzer -IRS data to constrain the torus SED. This sample was discussed in great detail by Lusso et al. ( 2013 ), who showed a very good agreement with their results. Thus the data we present here represent well the results of Maiolino et al. ( 2007 ). Figure 9 shows all the NIR–MIR-based compilations of C f , including ours, for the case of complete isotropic dust emission ( b = 1) on the left, and maximum anisotropy ( b = 0) on the right. For the present sample, we only show the case of Bol 1350 = 2. The uncertainty on represents the range in this property that is used to derive the median values. The uncertainty on / is taken from the original papers (Lusso et al. 2013 ; Roseboom et al. 2013 ) or from the present calculations. Given the uncertainties on and , we estimate a combined uncertainty on C f of at least ±0.2 dex at all . We also show, as blue open squares, the median values obtained from Shen et al. ( 2011 ) and shown in Figure 8 left panel (). Figure 9. Covering factor as a function of in large AGN samples. Open black squares: the Mor Netzer ( 2012 ) sample. Full black circles: the Lusso et al. ( 2013 ) sample. Open red circles: the Roseboom et al. ( 2013 ) sample. Open blue circles: the the present z = 2–3.5 sample without the weak-NIR sources. Open blue squares: SDSS sources from the Shen et al. ( 2011 ) catalog with the same redshift and luminosity as the present sample and measured as explained in the text. The left panel shows the covering factors under the assumption of isotropic dust emission. As explained in the text, the Roseboom et al. ( 2013 ) values are scaled up by factors of 1.5–1.8 to allow for the different assumed bolometric correction factors. The parallel dotted lines show the range of ±0.15 dex around the mean value of 0.68. The right panel shows the same data for the case of complete anisotropy ( b = 0 in Equation ( 3 )). The dotted lines indicate a range of ±0.15 dex around 0.4. Figure 10. Median (top) and mean stacks. In each part, the high luminosity group is shown in the upper row and the low luminosity group in the lower row. From left to right: 250, 350, and 500 μ m. The crosses mark the centers of the stacks. The diagrams presented here show that all medians of all the samples used here, at all , are confined to a band of width ±0.15 dex in / around 0.68 for the isotropic case, and 0.4 for the case of complete anisotropy. Because much of the uncertainty in C f is systematic and depends on the poorly known bolometric correction factor, the inclusion of a large number of individual measurements cannot improve the situation by much. Thus, the torus covering factors that are based on NIR–MIR measurements show no indication for a decrease of C f with increasing source luminosity. This finding seems to contradict earlier findings, such as those presented by Lusso et al. ( 2013 ) and Roseboom et al. ( 2013 ). An independent way of estimating the covering factor is to compare the