As our primary goal for the F330W image is to measure the brightness of the nucleus, we simply set the disk scale length to be identical to that obtained from the F606W fit. The resulting fit yields a bulge with $n=2.64$ and $r_e =$ 102 (515 pc), and a point source flux that is very insensitive to the assumptions of the disk component. The AGN magnitude changes by only $\pm 0.01$ mag depending on whether the disk is included or not. If we further force the bulge to have the same $n$ and $r_e$ as derived from the F606W fit (i.e. allowing only the luminosity to adjust), the resulting AGN magnitude changes by 0.06 mag.

[*HST*]{}: NIR Image
--------------------

The NICMOS/NIC1 F160W image was observed on 31 July 1997 (Proposal ID: 7328), in three 256 s exposures dithered in an “L”-shaped pattern. Each exposure was processed with the standard pipeline [calnica]{} within IRAF/STSDAS. This task corrects for the nonlinearity of the detector and removes the bias value, dark current, amplifier glow, and shading; however, it does not remove the ghost “pedestal” effect produced by the variable quadrant bias (see, e.g., Hunt & Malkan, 2004). To correct for this effect, we 