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

We present the first dynamical determination of the binary parameters of an eclipsing SW Sextantis star in the 3-4 h orbital period range during a low state. We obtained time-resolved optical spectroscopy and photometry of HS 0220+0603 during its 2004-2005 low-brightness state, as revealed in the combined Small & Moderate Aperture Research Telescope System, IAC80 and M1 Group long-term optical light curve. The optical spectra taken during primary eclipse reveal a secondary star spectral type of M5.5 +/- 0.5 as derived from molecular bandhead indices. The spectra also provide the first detection of a DAB white dwarf in a cataclysmic variable. By modelling its optical spectrum we estimate a white dwarf temperature of 30 000 +/- 5000 K. By combining the results of modelling the white dwarf eclipse from ULTRACAM light curves with those obtained by simultaneously fitting the emission-and absorption-line radial velocity curves and I-band ellipsoidal light curves, we measure the stellar masses to be M-1 = 0.87 +/- 0.09 M-circle dot and M-2 = 0.47 +/- 0.05 M-circle dot for the white dwarf and the M dwarf, respectively, and an inclination of the orbital plane of i approximate to 79 degrees. A radius of 0.0103 +/- 0.0007 R-circle dot is obtained for the white dwarf. The secondary star in HS 0220+0603 is likely too cool and undersized for its mass.