Shape and strength of the silicate emission feature of our FFPMOs with a disk (before and after dereddening) and a sample of brown dwarfs, T Tauri stars, and Herbig Ae/Be stars from I. Pascucci et al. (2009). The error bars indicate the upper and lower values for a change in A_V of ±1 mag. In comparison, this shows that the silicates in the disk around FFPMOs are processed to a higher degree than their massive counterparts.