  We use polarization observations of a circumbinary disk to investigate how
the polarization properties change at distinct frequency bands. Our goal is to
discern the main mechanism responsible for the polarization through comparison
between our observations and model predictions. We used ALMA to perform full
polarization observations at 97.5 GHz, 233 GHz and 343.5 GHz. The target is the
Class I object BHB07-11, which is the youngest object in the Barnard 59
protocluster. Complementary VLA observations at 34.5 GHz revealed a binary
system within the disk. We detect an extended and structured polarization
pattern remarkably consistent among all three bands. The distribution of
polarized intensity resembles a horseshoe shape with polarization angles
following this morphology. From the spectral index between bands 3 and 7, we
derive a dust opacity index $\beta \sim 1$ consistent with maximum grain sizes
larger than expected to produce self-scattering polarization in each band. The
polarization morphology do not match predictions from self-scattering. On the
other hand, marginal correspondence is seen between our maps and predictions
from radiation field assuming the brightest binary component as main radiation
source. Molecular line data from BHB07-11 indicates disk rotation. We produced
synthetic polarization maps from a rotating magnetized disk model assuming
combined poloidal and toroidal magnetic field components. The magnetic field
vectors (i. e., the polarization vectors rotated by 90$\degr$) are better
represented by a model with poloidal magnetic field strength about 3 times the
toroidal one. The similarity of our polarization patterns among the three bands
provides a strong evidence against self-scattering and radiation fields. On the
other hand, our data are reasonably well reproduced by a model of disk with
toroidal magnetic field components slightly smaller than poloidal ones.
