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We present 353 GHz full-sky maps of the polarization fraction $p$, angle$\psi$, and dispersion of angles $S$ of Galactic dust thermal emission producedfrom the 2018 release of Planck data. We confirm that the mean and maximum of$p$ decrease with increasing $N_H$. The uncertainty on the maximum polarizationfraction, $p_\mathrm{max}=22.0$% at 80 arcmin resolution, is dominated by theuncertainty on the zero level in total intensity. The observed inversebehaviour between $p$ and $S$ is interpreted with models of the polarized skythat include effects from only the topology of the turbulent Galactic magneticfield. Thus, the statistical properties of $p$, $\psi$, and $S$ mostly reflectthe structure of the magnetic field. Nevertheless, we search for potentialsignatures of varying grain alignment and dust properties. First, we analysethe product map $S \times p$, looking for residual trends. While $p$ decreasesby a factor of 3--4 between $N_H=10^{20}$ cm$^{-2}$ and $N_H=2\times 10^{22}$cm$^{-2}$, $S \times p$ decreases by only about 25%, a systematic trendobserved in both the diffuse ISM and molecular clouds. Second, we find nosystematic trend of $S \times p$ with the dust temperature, even though in thediffuse ISM lines of sight with high $p$ and low $S$ tend to have colder dust.We also compare Planck data with starlight polarization in the visible at highlatitudes. The agreement in polarization angles is remarkable. Two polarizationemission-to-extinction ratios that characterize dust optical properties dependonly weakly on $N_H$ and converge towards the values previously determined fortranslucent lines of sight. We determine an upper limit for the polarizationfraction in extinction of 13%, compatible with the $p_\mathrm{max}$ observed inemission. These results provide strong constraints for models of Galactic dustin diffuse gas.

Planck 2018 results. XII. Galactic astrophysics using polarized dust emission