the same profile as broad [H$\alpha$]{}. With the exception of [\[O[III]{}\]]{}$\lambda4959,5007$, 0.1cm we fit the other narrow emission lines simply with a single Gaussian. For [\[O[III]{}\]]{}, we modeled each of its doublet lines with two Gaussians, one accounting for the bulk component (line core) and the other for a weak, yet apparent, blue wing. All the line parameters are listed in Table 1. We make available online the data and the detailed fitting parameters.[^1]

The ratios of the prominent narrow lines, [\[O[III]{}\]]{}$\lambda5007$/[H$\beta$]{} $= 5.5$ and [\[N[II]{}\]]{}$\lambda6583$/[H$\alpha$]{} $= 0.4$, place UM 625 within the regime of AGNs (Baldwin et al. 1981). With a total [H$\beta$]{} to [\[O[III]{}\]]{}$\lambda5007$ ratio of 0.2, UM 625, like NGC 4395 and POX 52, would be considered a Seyfert 1.8 in the classification scheme of Osterbrock (1981). From the best-fit model of broad [H$\alpha$]{} yields FWHM = $1801 \pm 68$ [$\mathrm{km~s^{-1}}$]{} and a line dispersion ($\sigma_{\rm line}$, the second moment of the line profile) of $1583 \pm 59$ [$\mathrm{km~s^{-1}}$]{} (both corrected for the SDSS instrumental resolution of 139 [$\mathrm{km~s^{-1}}$]{} FWHM). The luminosity of broad [H$\alpha$]{} is $2.3 \times 10^{40}$ [erg s$^{-1}$]{}. The observed (not corrected for internal extinction) luminosity of the narrow [H$\alpha$]{} component is 3 times 