  Polar faculae are bright features that can be detected in solar limb
observations and they are related to magnetic field concentrations. Although
there is a large number of works studying them, some questions about their
nature as their magnetic properties at different heights are still open. Thus,
we aim to improve the understanding of solar polar faculae. In that sense, we
infer the vertical stratification of the temperature, gas pressure, line of
sight velocity and magnetic field vector of polar faculae regions. We performed
inversions of the Stokes profiles observed with Hinode/SP after removing the
stray light contamination produced by the spatial point spread function of the
telescope. Moreover, after solving the azimuth ambiguity, we transform the
magnetic field vector to local solar coordinates. The obtained results reveal
that the polar faculae are constituted by hot plasma with low line of sight
velocities and single polarity magnetic fields in the kilogauss range that are
nearly perpendicular to the solar surface. We also found that the spatial
location of these magnetic fields is slightly shifted respect to the continuum
observations towards the disc centre. We believe that this is due to the hot
wall effect that allows detecting photons that come from deeper layers located
closer to the solar limb.
