ring region is indicated in Figure 2 with the green polygon. These high-resolution images give us a distinct opportunity to study not only the multiwavelength properties of the AGN, but also its host galaxy. The [*HST*]{}  images, however, suffer from one major limitation: their field of view is too small to properly sample the disk component or to reliably measure the sky background.

\[sdssimg\]

Fortunately, UM 625 was imaged with SDSS. Thus, before we discuss the [*HST*]{} images in detail, we first turn to the SDSS images. Our strategy is to use the SDSS $r$-band image, which closely approximates the [*HST*]{} F606W band, to constrain the photometric parameters of the disk component, which is otherwise difficult to determine from the [*HST*]{}  data alone. With the disk thus constrained, we will use the [*HST*]{} F606W image to measure the parameters of the AGN point source and the bulge, which are central to our scientific analysis. The F330W and F160W images provide further photometric points for the nuclear SED, as well as color information to diagnose the stellar population of the bulge.

SDSS Imaging
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UM 625 was observed by SDSS in $ugriz$ on 24 May 2001 UT (Figure 3). Although the 