Accurate Masses for the Primary and Secondary in the Eclipsing White Dwarf Binary NLTT 11748

We measure the radial velocity curve of the eclipsing detached white dwarf binary NLTT 11748. The primary exhibits velocity variations with a semi-amplitude of 273 km s⁻¹ and an orbital period of 5.641 hr. We do not detect any spectral features from the secondary star or any spectral changes during the secondary eclipse. We use our composite spectrum to constrain the temperature and surface gravity of the primary to be T_eff = 8690 ± 140 K and log g = 6.54 ± 0.05, which correspond to a mass of 0.18 M ☉. For an inclination angle of 89.°9 derived from the eclipse modeling, the mass function requires a 0.76 M ☉ companion. The merger time for the system is 7.2 Gyr. However, due to the extreme mass ratio of 0.24, the binary will most likely create an AM CVn system instead of a merger