Spectral Fitting
==========================================

Our data analysis and modeling involves the full suite of multi-component (accretion disk, white dwarf photosphere, accretion belt) synthetic spectral codes, which we have utilized in our spectral fitting of [*[FUSE]{}*]{} and [*[IUE]{}*]{} data. Based upon our expectation that the accreting white dwarf is an important source of FUV flux in these systems during quiescence, we carried out a high gravity photosphere synthetic spectral analysis first. The model atmosphere (TLUSTY200; @hub88), and spectrum synthesis codes (SYNSPEC48 and ROTIN4 @hub95) and details of our $\chi^{2}_{\nu}$ ($\chi^2$ per degree of freedom) minimization fitting procedures are discussed in detail in @sio95 and will not be repeated here. To estimate physical parameters, we generally took the white dwarf photospheric temperature T$_{eff}$, log $g$, and rotational velocity $v_{rot}$ and chemical abundances as free parameters.

We normalize our fits to 1 solar radius and 1 kiloparsec such that the distance of a source is computed from $d = 
1000(pc)*(R_{wd}/R_{\sun})/\sqrt{S}$, or equivalently the scale factor $S 
= \left( \frac{R_{wd}}{R_{\odot}} \right)^{2} \left( \frac{d}{kpc} 
\right)^{-2}$, is the factor by which the theoretical flux (integrated over the entire wavelength range) has to be multiplied to equal the observed (integrated) flux.

The grid of WD models extended over 