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This paper presents the large-scale polarized sky as seen by Planck HFI at353 GHz, which is the most sensitive Planck channel for dust polarization. Weconstruct and analyse large-scale maps of dust polarization fraction andpolarization direction, while taking account of noise bias and possiblesystematic effects. We find that the maximum observed dust polarizationfraction is high (pmax > 18%), in particular in some of the intermediate dustcolumn density (AV < 1mag) regions. There is a systematic decrease in the dustpolarization fraction with increasing dust column density, and we interpret thefeatures of this correlation in light of both radiative grain alignmentpredictions and fluctuations in the magnetic field orientation. We alsocharacterize the spatial structure of the polarization angle using the angledispersion function and find that, in nearby fields at intermediate latitudes,the polarization angle is ordered over extended areas that are separated byfilamentary structures, which appear as interfaces where the magnetic field skyprojection rotates abruptly without apparent variations in the dust columndensity. The polarization fraction is found to be anti-correlated with thedispersion of the polarization angle, implying that the variations are likelydue to fluctuations in the 3D magnetic field orientation along the line ofsight sampling the diffuse interstellar medium.We also compare the dustemission with the polarized synchrotron emission measured with the Planck LFI,with low-frequency radio data, and with Faraday rotation measurements ofextragalactic sources. The two polarized components are globally similar instructure along the plane and notably in the Fan and North Polar Spur regions.A detailed comparison of these three tracers shows, however, that dust andcosmic rays generally sample different parts of the line of sight and confirmsthat much of the variation observed in the Planck data is due to the 3Dstructure of the magnetic field.

Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust