Post-common-envelope binary stars and the precataclysmic binary PG 1114+187

We present orbit-resolved spectroscopy and orbit-sampled photometry of the binary system PG 1114+187. Both photometry and radial velocity studies reve al a period P = 1.75992 days, which is taken to be the orbital period of th e binary. Strong modulation of emission-line strength with the same period is also present. A preliminary mass ratio, M-2/M-1 approximate to 0.7, is f ound from primary- and secondary-star radial velocity amplitudes. No eviden ce is seen for either an accretion disk or mass transfer, leading to the co nclusion that PG 1114+187 is not a cataclysmic variable (CV) but is in a pr e-CV state, before the initiation of mass transfer. The short orbital perio d also leads to the conclusion that the system passed through a common-enve lope phase at some time in the past. The current list of known post-common- envelope and precataclysmic binary stars is also reviewed and the general p roperties of this class of star are discussed.