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tokens: of the bolometric luminosity are presented in Fig. 10 . The bulk of the NIR emission is produced close to the inner edge of the thin disk, that is, the sublimation radius, consistent with observations (continuum reverberation mapping: e.g., Suganuma et al. 2006 ; interferometry: e.g., Kishimoto et al. 2011 ). Without a wind component, the model NIR luminosities are about 50% higher than those of the model with a wind component for type 1 objects, because the wind provides a nonnegligible NIR extinction. As expected, the NIR luminosities decrease significantly once the inner thin gas disk is hidden by the thick gas disk. We observe a less significant drop of the NIR luminosities for high inclination angles ( i >65°) in the presence of a wind. We interpret the additional NIR emission as the contribution of the unobscured basis of the wind to the NIR emission. Whereas the ratio between the NIR and bolometric luminosity is about 1∕10 for the basic wind model, it increases by a factor of ~1.5 and ~2 when the puff-up is located at a and 2 times smaller distance from the central black hole ( Fig. 11 ). The increase of the NIR luminosity due to higher dust temperatures is stronger than the decrease due to the smaller area where hot dust can be found. Fig. 10 Model NIR luminosities as a function of the bolometric luminosity. Blue represents type 1, red represents type 2. The Circinus model is shown with crosses and pluses; the NGC 1068 model with squares and triangles. The inclination angles of type 2 objects are indicated: i = 50° (green line), i = 70° (orange line), i = 90° (yellow line). Left panel : wind with 1∕ z density profile. Right panel : no wind component. The dotted lines correspond to L NIR = ξ L bol with ξ = 1, 1∕3, and 1∕10. Fig. 11 Model NIR luminosities as a function of the bolometric luminosity for the 1∕ z winds for a ( left panel ) and 2 ( right panel ) times smaller inner radius of the thin gas disk. The dotted lines correspond to L NIR = ξ L bol with ξ = 1, 1∕3, and 1∕10. The NIR luminosities as a function of the MIR luminosities are presented in Fig. 12 . As for the previous correlations, the differences between the 1∕ z and 1∕ z 2 models are minor. Whereas type 1 objects show NIR/MIR ratios between 0.5 and 1, the NIR luminosities of type 2 models are more than five times smaller than the MIR luminosities. For luminosities smaller than 10 44 erg s −1 and inclination angles between 50° and 60° the MIR/NIR luminosity ratio is about ten. The model with an inner radius located at 2 × r sub (right panel of Fig. 13 ) reproduces the observations of Burtscher et al. (2015) best. Fig. 12 Model NIR luminosities as a function of the MIR luminosity. Blue represents type 1, red represents type 2. The Circinus model is shown with crosses and pluses; the NGC 1068 model with squares and triangles. The inclination angles of type 2 objects are indicated: i = 50° (green line), i = 70°(orange line), i = 90° (yellow line). Left panel : wind with 1∕ z