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The quest for a B-mode imprint from primordial gravity waves on thepolarization of the cosmic microwave background (CMB) requires thecharacterization of foreground polarization from Galactic dust. We present astatistical study of the filamentary structure of the 353 GHz Planck Stokesmaps at high Galactic latitude, relevant to the study of dust emission as apolarized foreground to the CMB. We filter the intensity and polarization mapsto isolate filaments in the range of angular scales where the power asymmetrybetween E-modes and B-modes is observed. Using the Smoothed Hessian Major AxisFilament Finder, we identify 259 filaments at high Galactic latitude, withlengths larger or equal to 2\deg\ (corresponding to 3.5 pc in length for atypical distance of 100 pc). These filaments show a preferred orientationparallel to the magnetic field projected onto the plane of the sky, derivedfrom their polarization angles. We present mean maps of the filaments in StokesI, Q, U, E, and B, computed by stacking individual images rotated to align theorientations of the filaments. Combining the stacked images and the histogramof relative orientations, we estimate the mean polarization fraction of thefilaments to be 11 %. Furthermore, we show that the correlation between thefilaments and the magnetic field orientations may account for the E and Basymmetry and the $C_{\ell}^{TE}/C_{\ell}^{EE}$ ratio, reported in the powerspectra analysis of the Planck 353 GHz polarization maps. Future models of thedust foreground for CMB polarization studies will need to take into account theobserved correlation between the dust polarization and the structure ofinterstellar matter.

Planck intermediate results. XXXVIII. E- and B-modes of dust polarization from the magnetized filamentary structure of the interstellar medium