Comparison of the model predictions for dust and the Planck data. The columns from left to right are for Stokes I, Q, and U, while the rows are the data followed by the prediction for each model, and lastly the difference between model and data divided by the uncertainty.As for synchrotron emission, the polarization uncertainty is computed as the ensemble variance predicted by the models. Since dust total intensity is not a function of the magnetic field, its uncertainties are computed from the sky rms of the dust map.