UG denoting a U Gem-type system; (3) orbital period in days; (4) the recurrence time of dwarf nova outbursts in days; (6) the apparent magnitude at minimum (quiescence); (7) the apparent magnitude in outburst; (8) secondary spectral type; (9) orbital inclination in degrees; (10) white dwarf mass in solar masses; (11) secondary star mass in solar masses; (12) adopted reddening value and ; (13) distance in parsecs.

Observations and Data Reduction
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The instrumental setup and exposure details of the [*[FUSE]{}*]{} spectra of BV Cen, CH UMa and UU Aql in quiescence are provided in Table 2. The LWRS was used in all cases since it is least prone to slit losses due to the misalignment of the four [*[FUSE]{}*]{} telescopes. All the spectra were obtained in time tag (TTAG) mode, and each one of them consists of 7 individual exposures (corresponding to 7 [*[FUSE]{}*]{} orbits). It is clear that the relatively poor [*[FUSE]{}*]{} spectral quality of the spectra speaks to the requirement for more observing time. Nevertheless, we deemed that there was sufficient S/N to warrant a first attempt multi-component FUV analysis of each system

All the data were reduced using CalFUSE version 3.0.7. In this version of CalFUSE 