NICMOS images of the GG Tau Circumbinary Disk

We present deep, near-infrared images of the circumbinary disk surrounding the pre–main-sequence binary star, GG Tau A, obtained with NICMOS aboard the Hubble Space Telescope. The spatially resolved proto-planetary disk scatters ∼1.5% of the stellar flux, with a near-to-far side flux ratio of ∼1.4, independent of wavelength, and colors that are comparable to the central source all of these properties are significantly different from the earlier ground-based observations. New Monte Carlo scattering simulations of the disk emphasize that the general properties of the disk, such as disk flux, near side to far side flux ratio and integrated colors, can be approximately reproduced using ISM-like dust grains, without the presence of either circumstellar disks or large dust grains, as had previously been suggested. A single parameter phase function is fitted to the observed azimuthal variation in disk flux, providing a lower limit on the median grain size of a > 0.23 µm. Our analysis, in comparison to previous simulations, shows that the major limitation to the study of grain growth in T Tauri disk systems through scattered light lies in the uncertain ISM dust grain properties. Without explicit determination of the scattering properties it is not possible to differentiate between geometric, scattering and evolutionary effects. Finally, we use the 9 year baseline of astrometric measurements of the binary to solve the complete orbit, assuming that the binary is coplanar with the circumbinary ring. We find that the estimated 1σ range on disk inner edge to semi-major axis ratio, 3.2 < R in /a < 6.7, is larger than that estimated by previous SPH simulations of binary-disk interactions. Subject headings: