rests on the assumptions that (1) differences between the two spectra in orbital phase and (2) in time after the last outburst can be ignored. Given the long exposure times of the [*[FUSE]{}*]{} and [*[IUE]{}*]{} spectra, the questionable reliability of the orbital ephemerides, including UU Aql’s and (3) the limited S/N of the quiescent spectra, the influence of phase-dependent variations is not considered. However, the time since the last outburst as well as the brightness state of the system at the times of the [*[FUSE]{}*]{} and [*[IUE]{}*]{} observations for the three systems is considered in detail using AAVSO archival light curve data. For UU Aql, the [*[FUSE]{}*]{} spectrum was obtained approximately 50 days after its last major dwarf nova outburst, however, the [*[IUE]{}*]{} spectrum was obtained during the transition to a brightening that appeared not to be a major outburst. Therefore, we have excluded the [*[IUE]{}*]{} spectrum from use in combination with the [*[FUSE]{}*]{} data for UU Aql. For BV Cen both the [*[FUSE]{}*]{} and [*[IUE]{}*]{} spectra were obtained during quiescence but the [*[FUSE]{}*]{} spectrum was acquired approximately 159 days after the last outburst while the [*[IUE]{}*]{} spectrum was taken roughly 50 days after the last outburst. Thus, the [*[FUSE]{}*]{} 