be ruled out.

For CH UMa, the [*[FUSE]{}*]{} spectrum is very noisy and underexposed. We took into account our adopted distance of 300 pc in the model fitting, we fixed the WD mass at M$_{wd} = 1.2 M_{\sun}$ (Log $g = 9.0$, with a radius of $\approx 4,000$km), and fixed the disk inclination at the published value of 18 degrees. A single temperature white dwarf fit to CH UMa had $\chi^{2} = 0.227$, and yielded a best fit T$_{eff} = 29,000$K, and a distance of 310pc. This model however did not fit very well in the shorter wavelengths ($<$1020Å). A lowest $\chi^{2}$ fit for this same WD mass was obtained for T=40,000K, with $\chi^{2} = 0.208$, but it yielded a distance of 600pc, twice the adopted estimate of the distance. Since the Ritter catalog give a mass of 1.95$M_{\odot}$ (well above the Chandraskhar mass limit for a WD), we decided to try a larger mass with a correspondingly smaller radius which lead to a smaller emitting surface area and therefore a shorter distance. We assumed $M=1.38M_{\odot}$ ($log {g} = 9.5$, with a radius of $\approx 2,000$km) and found that the best fit was for $T=40,000$K. This model yielded a distance 