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Multiwavelength dust continuum and polarization observations arising fromself-scattering have been used to investigate grain sizes in young disks.However, the polarization by self-scattering is low in face-on optically thickdisks and puts some of the size constraints from polarization on hold,particularly for the younger and more massive disks. The 1.3 mm emissiondetected toward the hot ($\gtrsim$400 K) Class 0 disk IRAS 16293-2422 B hasbeen attributed to self-scattering, predicting grain sizes between 200-2000$\mu$m. We investigate the effects of grain size in the resultant flux andpolarization fractions from self-scattering using a hot and massive Class 0disk model and compare with observations. We compared new and archivalhigh-resolution observations between 1.3 and 18 mm to a set of syntheticmodels. We have developed a new public tool to automate this process calledSynthesizer. This is an easy-to-use program to generate synthetic observationsfrom numerical simulations. Optical depths are in the range of 130 to 2 from1.3 to 18 mm, respectively. Predictions from significant grain growthpopulations, including millimetric grains are comparable to the observations atall wavelengths. The polarization fraction produced by self-scattering reachesa maximum of $\sim$0.1% at 1.3 mm for a maximum grain size of 100 $\mu$m, beingan order of magnitude lower than that observed with ALMA. From the comparisonof Stokes I fluxes, we conclude that significant grain growth could be presentin the young Class 0 disk IRAS 16293 B, particularly in the inner hot region($<10$ au, $T>$ 300 K) where refractory organics evaporate. The polarizationproduced by self-scattering in our model is not high enough to explain theobservations at 1.3 and 7 mm, and effects like dichroic extinction orpolarization reversal of elongated aligned grains remain other possible butuntested scenarios.

Exploring the dust grain size and polarization mechanism in the hot and massive Class 0 disk IRAS 16293-2422 B