two power-law components at 5600 Å, a relatively line-free region, be equal to the observed flux at that point. Following Boroson & Green (1992), an effective  template can be generated by a simple velocity-broadening and scaling of the spectrum derived from observations of the “narrow-line” Type 1 AGN [I]{} Zw 1 (kindly provided by T. Boroson). In order to avoid contamination from strong spectral lines, we only include the following regions in our fit: 4170–4260, 4430–4770, 5080–5550, 6050–6200, and 6890–7010 Å. We do not fit the region below 3685 Å, since it is not covered by the [I]{} Zw 1  template of Boroson & Green (1992); consequently, we do not have to model the Balmer continuum (e.g., Wills, Netzer, & Wills 1985).

Approximately 30 objects at the lowest luminosities have sufficient galaxy contamination to warrant removing it. In lieu of more sophisticated methods for starlight decomposition (e.g., Greene & Ho 2004, 2005), we find that for the present sample the galaxy continuum can be modeled adequately using a scaled spectrum of a velocity-broadened K giant star (obtained from the SDSS).

Emission Lines
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The primary challenge in measuring accurate fluxes and profiles of broad emission lines is to properly deblend 