silicate. The icy grain model is shown as a dotted line in Figure \[fig:sed\]. This model has a total dust surface area of 14AU$^2$ and a mass of order 10$M_\oplus$ if the size distribution is extrapolated up to 1000km size objects.

The parameters from of this model are degenerate for the data in hand; for example the size distribution could be shallower and the fraction of silicates higher (e.g. $q=1.83$ and $f_{\rm sil} = 4\%$). If we allow the minimum grain size to be larger than the blowout limit, the disk is well fit by amorphous silicate grains with $q=1.9$ and $D_{\rm
  bl} = 10\mu$m. The disk spectrum can even be fit with a single size population of 25$\mu$m icy grains. However, the predictions for the flux at millimeter wavelengths depend on the size distribution, with lower fluxes for steeper size distributions. Therefore, grain properties and size distribution can be further constrained in the future with deep (sub)mm continuum measurements.

In summary, it is hard to constrain the grain sizes or properties. There is a difference in the required minimum grain size that depends on composition. Because icy grains are reflective at optical wavelengths, a detection of the disk in 