(1999). We model the starlight component with the stellar templates of Lu et al. (2006), which were built from the simple stellar population spectra (Bruzual & Charlot 2003). The AGN continuum is modeled as a power law. The stellar absorption lines must be subtracted well to ensure reliable measurement of weak emission lines (e.g., Ho et al. 1993, 1997). This is achieved by broadening and shifting the starlight templates to match the stellar velocity dispersion of the galaxy. As shown in Figure 1 (left panel), the fit is good; the absorption features are well matched, and the residuals in the emission line-free regions are consistent with the noise level.

Next, we fit the emission lines with Gaussians, using the code described in detail in Dong et al. (2005). The spectrum of UM 625 is dominated by strong, narrow emission lines such as [\[O[III]{}\]]{}$\lambda\lambda4959,5007$, [H$\beta$]{}, [H$\alpha$]{}, and [\[N[II]{}\]]{}$\lambda\lambda6548,6583$. But even a cursory inspection of the spectrum reveals that [H$\alpha$]{} has a clear broad component, even before continuum subtraction; after continuum subtraction, a broad component to [H$\beta$]{} also emerges. This is reminiscent of the situation of the two prototypal broad-line AGNs with intermediate-mass BHs, namely NGC4395 (Filippenko & Sargent 1989) and POX52 