Left: decomposed SEDs. The black solid lines show the Kurucz models and the Spitzer IRS spectra. The black dots represent the observed photometry corrected for extinction (see also Appendix A). The solid purple line is the sum of the flux of all the components. The dashed yellow and dashed-dotted green lines are the halo and inner disk components, respectively. The triple dotted dashed red line indicates the emission from the wall (from the wall radius to 3 AU outwards). The dotted blue line shows the emission from the rest of the outer disk. Note that the IRAS photometry and Spitzer spectrum do not match very well for HD 97048, this may be caused by the difference in beam sizes. Right: azimuthally averaged radial brightness profiles of the Q-band relative to the maximum flux. The central wavelengths of these images are 18.8 μm for HD 169142 and Oph IRS 48 and 24.5 μm for HD 97048 and HD 135344 B. The 24.5 μm fit to HD 169142 can be found in Honda et al. (2012). The grey diamonds indicate the PSF of the calibration star. The red triangles show the observation of the science targets. The error bars indicate the one sigma error on the azimuthally averaged radial brightness profiles. The solid purple line shows our best-fit model.
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