  We have used a Monte Carlo radiative transfer code to produce edge-on images
of dusty galactic disks, allowing a fraction of the dust to be distributed in
clumps. Synthetic images of edge-on galaxies have been constructed for
different amounts of dust, distributions of clumps and fractions of dust in
clumps, following the formalism of Bianchi et al. (1999). We have also
considered models with stellar emission embedded in the clumps. The synthetic
images have been fitted with analytical models made with smooth distributions
of dust, adopting the procedure developed by Xilouris et al. (1999) to fit
optical images of real edge-on galaxies. We have compared the parameters
determined by the fit with the input parameters of the models. For the clumping
distributions adopted in this paper, the neglect of clumping results in
underestimating the amount of dust in a galaxy. However, the underestimation is
never larger than 40%.
