broad emission lines. The continuum and line measurements are corrected for Galactic extinction using the extinction map of Schlegel, Finkbeiner, & Davis (1998) and the reddening law of Cardelli, Clayton, & Mathis (1989).

Continuum
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The nonstellar, featureless continuum of Type 1 (broad-line) AGNs is challenging to measure at optical wavelengths because it is entangled with a complex emission-line spectrum and starlight, depending on the relative brightness of the nucleus with respect to the host galaxy. Particularly troublesome are the broad, blended  multiplets, which form a “pseudo-continuum” that litters most of the spectrum, but especially the regions flanking [H$\beta$]{}. Moreover, the intrinsic shape of the featureless continuum itself is not well known. For the objects that have minimal starlight contamination, which, by selection, constitute the majority of our sample, we decompose the spectrum by simultaneously fitting a two-component model consisting of (1) an underlying featureless continuum and (2) an empirical template. In practice, the featureless continuum over the optical region can be approximated well by a double power law, with a spectral break at $\lambda \approx 5000$ Å (Vanden Berk [et al.]{} 2001; M. Kim & L. C. Ho 2005, in preparation). We require that the combined flux of the 