  Solar pores are active regions with large magnetic field strengths and
apparent simple magnetic configurations. Their properties resemble the ones
found for the sunspot umbra although pores do not show penumbra. Therefore,
solar pores present themselves as an intriguing phenomenon that is not
completely understood. We examine in this work a solar pore observed with
Hinode/SP using two state of the art techniques. The first one is the spatial
deconvolution of the spectropolarimetric data that allows removing the stray
light contamination induced by the spatial point spread function of the
telescope. The second one is the inversion of the Stokes profiles assuming
local thermodynamic equilibrium that let us to infer the atmospheric physical
parameters. After applying these techniques, we found that the spatial
deconvolution method does not introduce artefacts, even at the edges of the
magnetic structure, where large horizontal gradients are detected on the
atmospheric parameters. Moreover, we also describe the physical properties of
the magnetic structure at different heights finding that, in the inner part of
the solar pore, the temperature is lower than outside, the magnetic field
strength is larger than 2 kG and unipolar, and the LOS velocity is almost null.
At neighbouring pixels, we found low magnetic field strengths of same polarity
and strong downward motions that only occur at the low photosphere, below the
continuum optical depth $\log \tau=-1$. Finally, we studied the spatial
relation between different atmospheric parameters at different heights
corroborating the physical properties described before.
