  It has not been shown so far whether the diffuse Galactic polarized emission
at frequencies relevant for cosmic microwave background (CMB) studies
originates from nearby or more distant regions of our Galaxy. This questions
previous attempts that have been made to constrain magnetic field models at
local and large scales. The scope of this work is to investigate and quantify
the contribution of the dusty and magnetized local interstellar medium to the
observed emission that is polarized by thermal dust. We used stars as distance
candles and probed the line-of-sight submillimeter polarization properties by
comparing the emission that is polarized by thermal dust at submillimeter
wavelengths and the optical polarization caused by starlight. We provide
statistically robust evidence that at high Galactic latitudes ($|b| \geq
60^\circ$), the $353$ GHz polarized sky as observed by \textit{Planck} is
dominated by a close-by magnetized structure that extends between $200$ and
$300$ pc and coincides with the shell of the Local Bubble. Our result will
assist modeling the magnetic field of the Local Bubble and characterizing the
CMB Galactic foregrounds.
