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Post-shock regions (PSR) of polar cataclysmic variables produce most of theirluminosity and give rise to high circular polarization in optical wavelengthsand strong variability on the white dwarf rotation period, which aredistinctive features of these systems. To investigate the polar candidate V348Pav, we obtained a comprehensive observational set including photometric,polarimetric, and spectroscopic data, which was used to constrain thepost-shock properties of the system. The object presents high circularpolarization ($\sim30$ per cent) and high He II 4686A to H$~\beta$ line ratio,confirming it is a polar. From both radial velocities and light curves, wedetermined an orbital period of 79.98~min, close to the orbital period minimumof 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 spectralline emission in this system is originated in the region of the companion starfacing the WD, possibly irradiated by the emission related to the PSR. Wemodelled the PSR using the Cyclops code. The PSR density and temperatureprofiles, obtained by a proper solution of the hydro-thermodynamic equations,were used in a 3D radiative transfer solution that takes into account thesystem geometry. We could reproduce the V348 Pav \textit{B, V, R}, and\textit{I} photometric and polarimetric data using a model with a WD magneticfield of $\sim28$ MG, a WD mass of $\sim0.85$~M$_{\odot}$ and a low($\sim25^{\circ}$) orbital inclination. These values for the WD mass andorbital inclination are consistent with the measured radial velocities.

Optical observations and cyclops post-shock region modelling of the polar V348 Pav