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To characterize the mechanisms of planet formation it is crucial toinvestigate the properties and evolution of protoplanetary disks around youngstars, where the initial conditions for the growth of planets are set. Our goalis to study grain growth in the disk of the young, intermediate mass starHD163296 where dust processing has already been observed, and to look forevidence of growth by ice condensation across the CO snowline, alreadyidentified in this disk with ALMA. Under the hypothesis of optically thinemission we compare images at different wavelengths from ALMA and VLA tomeasure the opacity spectral index across the disk and thus the maximum grainsize. We also use a Bayesian tool based on a two-layer disk model to fit theobservations and constrain the dust surface density. The measurements of theopacity spectral index indicate the presence of large grains and pebbles($\geq$1 cm) in the inner regions of the disk (inside $\sim$50 AU) and smallergrains, consistent with ISM sizes, in the outer disk (beyond 150 AU).Re-analysing ALMA Band 7 Science Verification data we find (radially)unresolved excess continuum emission centered near the location of the COsnowline at $\sim$90 AU. Our analysis suggests a grain size distributionconsistent with an enhanced production of large grains at the CO snowline andconsequent transport to the inner regions. Our results combined with the excessin infrared scattered light found by Garufi et al. (2014) suggests the presenceof a structure at 90~AU involving the whole vertical extent of the disk. Thiscould be evidence for small scale processing of dust at the CO snowline.

Dust properties across the CO snowline in the HD 163296 disk from ALMA and VLA observations