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Forsterite is one of the crystalline dust species that is often observed inprotoplanetary disks and solar system comets. Being absent in the interstellarmedium, it must be produced during the disk lifetime. It can therefore serve asa tracer of dust processing and disk evolution, which can lead to a betterunderstanding of the physical processes occurring in the disk, and possiblyplanet formation. However, the connection of these processes with the overalldisk crystallinity remains unclear. We aim to characterize the forsteriteabundance and spatial distribution in the disk of the Herbig Be star HD 100546,to investigate if a connection exists with the large disk gap. We use a 2Dradiative transfer code, MCMax, to model the circumstellar dust around HD100546. We use VISIR Q-band imaging to probe the outer disk geometry andmid-infrared features to model the spatial distribution of forsterite. Thetemperature-dependent shape of the 69 micron feature observed with HerschelPACS is used as a critical tool to constrain this distribution. We find acrystalline mass fraction of 40 - 60 %, located close to the disk wall between13 and 20 AU, and possibly farther out at the disk surface. The forsterite isin thermal contact with the other dust species. We put an upper limit on theiron content of forsterite of 0.3 %. Optical depth effects play a key role inexplaining the observed forsterite features, hiding warm forsterite from viewat short wavelengths. The disk wall acts as a showcase: it displays a localizedhigh abundance of forsterite, which gives rise to a high observedcrystallinity, while the overall mass fraction of forsterite is a factor of tenlower.

Low abundance, strong features: Window-dressing crystalline forsterite in the disk wall of HD 100546