We examine the UV/X-ray properties of 1378 quasars in order to link empirical correlations to theoretical models of the physical mechanisms dominating quasars as a function of mass and accretion rate. The clarity of these correlations is improved when (1) using CIV broad emission line equivalent width (EQW) and blueshift (relative to systemic) values calculated from high signal-to-noise ratio reconstructions of optical/UV spectra and (2) removing quasars expected to be absorbed based on their UV/X-ray spectral slopes. In addition to using the traditional CIV parameter space measures of CIV EQW and blueshift, we define a "CIV_{\parallel} distance" along a best-fit polynomial curve that incorporates information from both CIV parameters. We find that the CIV{\parallel} distance is linearly correlated with both the optical-to-X-ray slope, {alpha}_ox, and broad-line HeII EQW, which are known spectral energy distribution indicators, but does not require X-ray or high spectral resolution UV observations to compute. The CIV_{\parallel}_ distance may be a better indicator of the mass-weighted accretion rate, parameterized by L/LEdd, than the CIV EQW or blueshift alone, as those relationships are known to break down at the extrema. Conversely, there is only a weak correlation with the X-ray energy index ({Gamma}), an alternate L/LEdd indicator. We find no X-ray or optical trends in the direction perpendicular to the CIV distance that could be used to reveal differences in accretion disk, wind, or corona structure that could be widening the CIV EQW-blueshift distribution. A different parameter (such as metallicity) not traced by these data must come into play.

Cone search capability for table J/ApJ/931/154/fig13 (The "Good" that underlies the Bokeh interactive plots in Figure 13)