All Figures

	Figure 1: V-band surface brightness profiles perpendicular to the galactic disk for the model and the fits described in Sect. 3.3. Three cuts are shown, at distances 0 (brightest profile), 1, and 2 (dimmest profile) from the center along the galaxy's major axis.
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In the text

	Figure 2: K'-band surface brightness profiles along the minor axis for the models with a single dust disk and the model with two dust disks, together with their fits.
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In the text

Figure 3: NGC 4013. From top to bottom: the V-band image, the fit to the V-band image and the residuals; the K'-band image, the fit to the K'-band image and the residuals. Images and models are displayed with the modified logarithmic visualization method of Jarrett et al. (2003). The scale of residuals is linear: the bar with gray shades helps to distinguish regions with values in the ranges [-50%, -30%], [-30%, -10%], [-10%, 10%], [10%, 30%], and [30%, 50%] from lighter to darker. All regions with values outside these ranges are coded black. The horizontal size of the box is 6.

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In the text

Figure 4: NGC 4013. Surface brightness profiles for cuts perpendicular ( left panels) and parallel ( right panels) to the galactic disk, for the V-band ( top panels) and the K'-band ( bottom panels) images. In the left panels, profiles are shown for distances from the fitted center along the galactic plane corresponding to 0 (minor axis), 1/8 and 1/4 of the horizontal extent of the fitted area. Median values have been taken on a cut width of 2% that extent. The topmost data (crosses) refer to the minor axis, whose maximum has been assigned magnitude zero. Crosses refer to profiles on the right side of the images (with respect to Fig. 3) and are progressively displaced downward of 1.5 mag when moving from the center outward. Diamonds refer to the left side profiles, and are further displaced by 0.5 mag from their specular profile on the right side. The same scheme is adopted for the surface brightness profiles parallel to the major axis, shown in the right panels: profiles are shown for cuts at 0 (major axis; crosses), 1/8 and 1/4 of the vertical extent of the fitted area, above (crosses) and below (diamonds) the galactic plane. Median values have been taken over a cut width of 4% that extent. To reduce the cluttering of symbols only one point every three is plotted in horizontal profiles. Profiles are displaced in the same manner as in the left panels. In all panels, the curves refer to analogous cuts on the fitted images. Gaps in both model and data correspond to masked areas (i.e. stars). The shaded boxes in the upper part of the left (right) panels show the position and extent of the cuts displayed in the right (left) panels.

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In the text

	Figure 5: NGC 4217. Image order is the same as in Fig. 3. The horizontal size of the box is 8.
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In the text

	Figure 6: NGC 4302. Image order is the same as in Fig. 3. The horizontal size of the box is 8.
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In the text

	Figure 7: NGC 5529. Image order is the same as in Fig. 3. The horizontal size of the box is 7.
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In the text

	Figure 8: NGC 5746. Image order is the same as in Fig. 3. The horizontal size of the box is 8.
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In the text

	Figure 9: NGC 5965. Image order is the same as in Fig. 3. The horizontal size of the box is 6.
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In the text

	Figure 10: UGC 4277. Image order is the same as in Fig. 3. The horizontal size of the box is 4.
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In the text

	Figure 11: Same as Fig. 4, but for NGC 4217.
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In the text

	Figure 12: Same as Fig. 4, but for NGC 4302.
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In the text

	Figure 13: Same as Fig. 4, but for NGC 5529.
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In the text

	Figure 14: Same as Fig. 4, but for NGC 5746.
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In the text

	Figure 15: Same as Fig. 4, but for NGC 5965.
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In the text

	Figure 16: Same as Fig. 4, but for UGC 4277.
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In the text