Local Bubble contribution to the 353-GHz dust polarized emission

To date, it has never been shown whether the diffuse Galactic polarized emission, at frequencies relevant for cosmic microwave background (CMB) studies, originate from nearby or more distant regions of our Galaxy. This questions previous attempts to constrain magnetic field models, both 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 thermal dust polarized emission. We use stars as distance candles and probe the line-of-sight sub-millimeter polarization properties by comparing the dust thermal polarized emission at sub-millimeter wavelengths and the starlight optical polarization. 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 at distances extended up to $200 - 300$ pc, which coincides with the shell of the Local Bubble. Our result should be of assistance for the modeling of the magnetic field of the Local Bubble and for the characterization of the CMB Galactic foregrounds.