continuum energy distribution similar to UU Aql. There are definitely some broad emission lines from the source itself. The most prominent one is the O[vi]{} doublet (the right component being strongly attenuated by molecular hydrogen sharp absorption lines), C[iii]{} (both around 977Å and 1175Å) which also seems to be in emission and a tentative identification of N[iv]{} emission in the short wavelengths. The source is also contaminated with sharp emission lines due to air glow. Here too the N[i]{} & N[ii]{} are geocoronal in origin, and the sharp peaks on top of the broad C[iii]{} (977Å) and O[vi]{} emissions are heliocoronal in origin. We note that ISM molecular hydrogen absorption is affecting the continuum.

Since the wavelength range covered by [*[FUSE]{}*]{} overlaps with [*[HST]{}*]{}/STIS or [*[IUE]{}*]{} in the region of C[iii]{} between 1170Å and 1180Å, a much broader FUV wavelength coverage is afforded by combining the spectra when the flux levels of the two spectra in the wavelength overlap region match closely enough. We found archival [*[IUE]{}*]{} spectra matching the [*[FUSE]{}*]{} spectra of two of the three systems (CH UMa and BV Cen) but unfortunately no [*[HST]{}*]{} spectra exist for the three systems.

The [*[FUSE]{}*]{} + [*[IUE]{}*]{} combination of spectra 