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We present the first dynamical determination of the binary parameters of aneclipsing SW Sextantis star in the 3-4 hour orbital period range during a lowstate. We obtained time-resolved optical spectroscopy and photometry of HS0220+0603 during its 2004-2005 low brightness state, as revealed in thecombined SMARTS, IAC80 and M1 Group long-term optical light curve.  The optical spectra taken during primary eclipse reveal a secondary starspectral type of M5.5 $\pm$ 0.5 as derived from molecular band-head indices.The spectra also provide the first detection of a DAB white dwarf in acataclysmic variable. By modelling its optical spectrum we estimate a whitedwarf temperature of 30000 $\pm$ 5000 K.  By combining the results of modelling the white dwarf eclipse from ULTRACAMlight curves with those obtained by simultaneously fitting the emission- andabsorption-line radial velocity curves and I-band ellipsoidal light curves, wemeasure the stellar masses to be M$_1 = 0.87 \pm 0.09$ M$_\odot$ and M$_2 =0.47 \pm 0.05$ M$_\odot$ for the white dwarf and the M dwarf, respectively, andan inclination of the orbital plane of $i \approx 79^\mathrm{o}$. A radius of$0.0103 \pm 0.0007$ R$_\odot$ is obtained for the white dwarf. The secondarystar in HS 0220+0603 is likely too cool and undersized for its mass.

Dynamical masses of a nova-like variable on the edge of the period gap