Since then UM 625 has been classified as a Seyfert 2 galaxy (or occasionally as an H II galaxy) in light of its extremely strong [\[O[III]{}\]]{} $\lambda\lambda 4959,5007$ lines and the apparent absence of broad emission lines (e.g., Salzer et al. 1989; Terlevich et al. 1991). The spectral classification was re-examined critically by Dessauges-Zavadsky et al. (2000); using emission-line measurements from the literature, they classified it as a Seyfert 2 according to the three standard optical line-ratio diagnostic diagrams of Veilleux & Osterbrock (1987). Using a high-quality Sloan Digital Sky Survey (SDSS; York et al. 2000) spectrum with a resolution $R \approx 2000$, we clearly detect both broad [H$\alpha$]{} and [H$\beta$]{} and revise the spectral classification of UM 625 to a Seyfert 1. Combining the broad line width and luminosity, we estimate a BH mass of $1.6 \times 10^{6}$ [$M_{\odot}$]{}, placing UM 625 in our sample of AGNs with low-mass BHs (Dong et al. 2012b).

We assume a cosmology with $H_{0} =70$ km s$^{-1}$ Mpc$^{-1}$, $\Omega_{m} = 
0.3$, and $\Omega_{\Lambda} = 0.7$. At a redshift of $z=0.0250$, UM 625 has a luminosity distance of 109.1 Mpc.

Analysis of the Optical Spectrum
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UM 625 was spectroscopically observed by SDSS on 