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We present polarimetric data of CW Tau and DG Tau, two well-known Class IIdisk/jet systems, obtained with the Atacama Large Millimeter/submillimeterArray at 870 $\mu$m and 0."2 average resolution. In CW Tau, the total andpolarized emission are both smooth and symmetric, with polarization anglesalmost parallel to the minor axis of the projected disk. In contrast, DG Taudisplays a structured polarized emission, with an elongated brighter region inthe disk's near side and a belt-like feature beyond about 0."3 from the source.At the same time the total intensity is spatially smooth, with no features. Thepolarization pattern, almost parallel to the minor axis in the inner region,becomes azimuthal in the outer belt, possibly because of a drop in opticaldepth. The polarization fraction has average values of 1.2% in CW Tau and 0.4%in DG Tau. Our results are consistent with polarization from self-scattering ofthe dust thermal emission. Under this hypothesis, the maximum size of thegrains contributing to polarization is in the range 100 - 150 $\mu$m for CW Tauand 50 - 70 $\mu$m for DG Tau. The polarization maps combined with dust opacityestimates indicate that these grains are distributed in a geometrically thinlayer in CW Tau, representing a settling in the disk midplane. Meanwhile, suchsettling is not yet apparent for DG Tau. These results advocate polarizationstudies as a fundamental complement to total emission observations, ininvestigations of the structure and the evolution of protoplanetary disks.

ALMA observations of polarized emission toward the CW Tau and DG Tau protoplanetary disks: constraints on dust grain growth and settling