of spectral indices in quasars and since there is a degeneracy between $E(B-V)$ and $\alpha$. Although there is a true $\chi^2$-minimizing pair of spectral index and reddening values for the $RP$-fits, the degeneracy between $E(B-V)$ and $\alpha$ means that the two-parameter $RP$ fitting method cannot be used to determine unique, physical spectral indices and reddening values. As such, the $RP$ spectral indices and reddening values must be considered only mathematical values to reproduce the continua. Nevertheless, we can clearly see that [*at a given value of $\alpha_{RP}$*]{}, BALQSOs (LoBALs in particular) are redder than nonBALQSOs as measured by $E(B-V)_{RP}$; this result cannot be caused by the degeneracy between the two parameters of the $RP$-fit. A two-dimensional K-S test ([Fasano]{} & [Franceschini]{} 1987) shows that the nonBALQSO and BALQSO distributions in the \[$E(B-V)_{RP},\alpha_{RP}$\] plane are different at the 99.9999% confidence level ($\simeq5\sigma$). The HiBAL and LoBAL (including FeLoBAL) distributions are different at the 99.56% confidence level ($\simeq2.8\sigma$). Finally, as we shall discuss in § \[sec:colortrends\], we have reason to believe that the $RP$-fit values may still be useful in a relative sense.

The Form of the Reddening\[sec:red\]
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Having shown that both LoBALs [*and*]{} HiBALs are redder than nonBALQSOs and that 