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Debris disks or belts are important signposts for the presence of collidingplanetesimals and, therefore, for ongoing planet formation and evolutionprocesses in young planetary systems. Imaging of debris material at smallseparations from the star is very challenging but provides valuable insightsinto the spatial distribution of so-called hot dust produced by solid bodieslocated in or near the habitable zone. We report the first detection ofscattered light from the hot dust around the nearby (d = 28.33 pc) A star HD172555. We want to constrain the geometric structure of the detected debrisdisk using polarimetric differential Imaging (PDI) with a spatial resolution of25 mas and an inner working angle of about 0.1$''$. We measured the polarizedlight of HD 172555, with SPHERE-ZIMPOL, in the very broad band (VBB;$\lambda=735$ nm) filter for the projected separations between 0.08$''$ (2.3au) and 0.77$''$ (22 au). We constrained the disk parameters by fitting modelsfor scattering of an optically thin dust disk taking the limited spatialresolution and coronagraphic attenuation of our data into account. Thegeometric structure of the disk in polarized light shows roughly the sameorientation and outer extent as obtained from thermal emission at 18 $\mu$m.Our image indicates the presence of a strongly inclined ($i\sim 103.5^\circ$),roughly axisymmetric dust belt with an outer radius in the range between0.3$''$ (8.5 au) and 0.4$''$ (11.3 au). We derive a lower limit for thepolarized flux contrast ratio for the disk of $(F_{\rm pol})_{\rm disk}/F_{\rm\ast}> (6.2 \pm 0.6)\cdot 10^{-5}$ in the VBB filter. This ratio is small, only9 %, when compared to the fractional infrared flux excess ($\approx 7.2\cdot10^{-4}$). The model simulations show that more polarized light could beproduced by the dust located inside 2 au, which cannot be detected with theinstrument configuration used.

Detection of scattered light from the hot dust in HD 172555