from the subtraction of the elliptical isophote model from the image were consistent with sky noise, as expected for a good fit.

We also fitted profiles to the distribution of surface brightness of G as a function of the mean semi-major axis of its elliptical isophotes. We convolved the model profiles with the azimuthally-averaged profile of the PSF that we created with Tiny Tim v. 4.0, as above, for the $I$ data. Because we used only an azimuthal average of the PSF, the procedure is not significantly sensitive to the details of the PSF wings. We found a good fit ($\chi^2/DOF \sim 1.7$, where $DOF=38$ is the number of degrees of freedom for the fit), for an “$r^{1/4}$” De Vaucouleurs law ($I = I_e\times {\rm exp}(-7.67 [(r/r_e)^{1/4} - 1])$) with parameters $r_e = 1\farcs5 \pm 0\farcs7$ and $I_e = 24.9 \pm 0.4$ mag/arcsec$^2$. Figure 6 is a comparison of our profile data with our DeVaucouleurs profile. We found a better fit ($\chi^2/DOF \sim 0.8$) for a Hubble-law profile ($I = I_0/(1+(r/r_0)^2)$), and a worse fit ($\chi^2/DOF \sim 2.7$) for an isothermal profile ($I = I_0/(1+(r/r_0)^2)^{1/2}$). These results are similar to those obtained by van Dokkum & Franx (1996) for E 