${\ensuremath{\chi^2}}= 7$ and 23, respectively, for the [H$\beta$]{} and [H$\alpha$]{}–[\[N[II]{}\]]{} regions.

The extinction of the broad-line region (BLR) can be derived

\[galfit\]

from the observed Balmer decrement [H$\alpha$]{}/[H$\beta$]{} for normal AGNs (Dong et al. 2008). Assuming the extinction curve of the Small Magellanic Cloud (Hopkins et al. 2004; Wang et al. 2005) and an intrinsic broad-line [H$\alpha$]{}/[H$\beta$]{} = 3.1 (Dong et al. 2008), we get $E(B-V)=0.57$ mag for the BLR. Likewise, the observed narrow [H$\alpha$]{} and [H$\beta$]{} gives $E(B-V)=0.25$ mag for the NLR.

Analysis of the Images
======================

There are archival [*HST*]{} images in three bands for UM 625: F330W (roughly the $U$ band of the Johnson system), F606W ($R$), and F160W ($H$), observed through ACS, WFPC2, and NICMOS, respectively. From these images, we can see clearly that there is a bright point-like source present in the center of UM 625, and that the galaxy is almost round in shape and has no spiral arms, indicating an elliptical/spheroidal or a face-on S0 galaxy. Closer inspection reveals that there is, in addition, a nuclear semi-ring on scales of $\sim 
150-400$ pc; this feature, most conspicuous in the F330W image, is resolved into several knots, presumably sites of intense star formation. The 