  We have detected substructure within the smooth scattering disk of the
celebrated Galactic Center radio source Sagittarius A* (SgrA*). We observed
this structure at 1.3 cm wavelength with the Very Long Baseline Array together
with the Green Bank Telescope, on baselines of up to 3000 km, long enough to
completely resolve the average scattering disk. Such structure is predicted
theoretically, as a consequence of refraction by large-scale plasma
fluctuations in the interstellar medium. Along with the much-studied
$\theta_\mathrm{d}\propto \lambda^2$ scaling of angular broadening
$\theta_\mathrm{d}$ with observing wavelength $\lambda$, our observations
indicate that the spectrum of interstellar turbulence is shallow, with an inner
scale larger than 300 km. The substructure is consistent with an intrinsic size
of about 1 mas at 1.3 cm wavelength, as inferred from deconvolution of the
average scattering. Further observations of the substructure can set stronger
constraints on the properties of scattering material and on the intrinsic size
of SgrA*. These constraints will guide understanding of effects of
scatter-broadening and emission physics of the black hole, in images with the
Event Horizon Telescope at millimeter wavelengths.
