noise for the three [*[FUSE]{}*]{} spectra. We binned the data by 0.1Å for which the S/N of UU Aql, BV Cen, and CH UMa is 5.15, 5.9, and 3.6, respectively.

For UU Aql, Fig. 1 reveals a rich line spectrum with numerous lines of molecular hydrogen, interstellar species and possible accretion disk or photospheric absorption features. The spectrum reveals a downturn in the continuum shortward of 1000Å. The spectrum does not exhibit any evidence of emission lines from the source, the only emission lines are from air glow and heliocoronal (e.g. sharp emissions lines from C[iii]{} (around 977Å) and the O[vi]{} doublet).

In figure 2, the [*[FUSE]{}*]{} spectrum of BV Cen has a variety of interstellar and stellar features but has a continuum shape distinctly different from UU Aql. The broad C[iii]{} absorption feature around 1175Å  is definitely from the source, and the C[iii]{} (around 977Å) and the O[vi]{} doublet broad emission features could also possibly be associated with one of the FUV components in BV Cen. All the other sharp emission features are either heliocoronal or geocoronal in origin.

In figure 3, CH UMa reveals numerous absorption lines due to highly ionized and singly ionized metals. It has a 