  Post-shock regions (PSR) of polar cataclysmic variables produce most of their
luminosity and give rise to high circular polarization in optical wavelengths
and strong variability on the white dwarf rotation period, which are
distinctive features of these systems. To investigate the polar candidate V348
Pav, we obtained a comprehensive observational set including photometric,
polarimetric, and spectroscopic data, which was used to constrain the
post-shock properties of the system. The object presents high circular
polarization ($\sim30$ per cent) and high He II 4686A to H$~\beta$ line ratio,
confirming it is a polar. From both radial velocities and light curves, we
determined an orbital period of 79.98~min, close to the orbital period minimum
of CVs. The H$~\beta$ radial velocity curve has a semi-amplitude of
$141.4\pm1.5$ km s$^{-1}$. Doppler tomography showed that most of the spectral
line emission in this system is originated in the region of the companion star
facing the WD, possibly irradiated by the emission related to the PSR. We
modelled the PSR using the Cyclops code. The PSR density and temperature
profiles, obtained by a proper solution of the hydro-thermodynamic equations,
were used in a 3D radiative transfer solution that takes into account the
system geometry. We could reproduce the V348 Pav \textit{B, V, R}, and
\textit{I} photometric and polarimetric data using a model with a WD magnetic
field of $\sim28$ MG, a WD mass of $\sim0.85$~M$_{\odot}$ and a low
($\sim25^{\circ}$) orbital inclination. These values for the WD mass and
orbital inclination are consistent with the measured radial velocities.
