  For more than 5000 stars with accurate parallaxes from the Hipparcos and Gaia
DR1 Tycho-Gaia astrometric solution (TGAS), Tycho-2 photometry, interstellar
polarization from eight catalogues and interstellar extinction from eight 3D
maps the largest up to date comparison of the polarization and extinction is
provided. The extinction maps give different estimations of the extinction and
of the polarization efficiency as the polarization divided into extinction
$P/A_V$ as well as of the percentage of the stars with the polarization
efficiency higher than the limit of Serkowski $P/A_V>0.03$. Using the Hipparcos
parallaxes we found about 200 stars (4\%, mainly OB stars) drop higher than the
limit when we use any extinction map. However, the usage of more accurate TGAS
parallaxes decreases them to only 17 stars (0.3\%). The polarization and
extinction are negligible inside the Local Bubble within 80 pc from the Sun. In
the vast Bubble's shell at the distances 80--118 pc from the Sun the
polarization and extinction rapidly grow with the distance whereas the position
angle of the polarization is oriented predominantly along the shell of the
Bubble. Outside the Bubble the polarization and extinction grow with the
distance slowly. In addition, within a radius of 80--300 pc of the Sun a disc
of some filamentary dust clouds (including well-known Markkanen cloud) is
observed as in the polarization map as in the reddening one by Schlegel et al.
In this disc the position angle of polarization is preferably oriented along
the plane of the disk. For the regions further than 300 pc the position angle
of polarization is preferably oriented along the Local spiral arm, i.e. Y
coordinate axis. The polarization and its efficiency is lower in the dust layer
in the Gould belt than in the equatorial dust layer. It may means different
properties of dust in these two layers.
