Movie version of Figs. 3 to 5 are only available in electronic form at http://www.edpsciences.org

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The direction of the planet's motion does not affect the disk structure in this model, since a planet's secular perturbations are equivalent to those from the ring formed by spreading the planet's mass along its orbit (Murray & Dermott 1999).

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... FWHM

While the PSF of the ACS observations had a FWHM of 5 AU, the image in Fig. 10a has also been deprojected and smoothed azimuthally along $\sim$ 18 AU arcs leading to a smoothing function which varies across the image. However, the apparently higher resolution of the models in Fig. 10 is more likely to be caused by the difference in the distributions of the planetesimals in the disk (shown in the figures) and those of the dust grains seen in the observation (see Sect. 3.2).

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