We present ATCA interferometric observations of the old ( 13 Myr ) , nearby ( 86pc ) classical T Tauri star , PDS 66 .
Unresolved 3 and 12 mm continuum emission is detected towards PDS 66 , and upper limits are derived for the 3 and 6 cm flux densities .
The mm-wave data show a spectral slope flatter than that expected for ISM-sized dust particles , which is evidence of grain growth .
We also present HST/NICMOS 1.1 micron PSF-subtracted coronagraphic imaging observations of the circumstellar environment of PDS 66 .
The HST observations reveal a bilaterally symmetric circumstellar region of dust scattering \sim 0.32 % of the central starlight , declining in surface brightness as r ^ { -4.53 } .
The light-scattering disk of material is inclined 32 \pm 5 ^ { \circ } from a face-on viewing geometry , and extend to a radius of 170 AU .
These data are combined with published optical and longer wavelength observations to make qualitative comparisons between the median Taurus and PDS 66 spectral energy distributions ( SEDs ) .
By comparing the near-infrared emission to a simple model , we determine that the location of the inner disk radius is consistent with the dust sublimation radius ( \sim 1400 K at 0.1 AU ) .
We place constraints on the total disk mass using a flat-disk model and find that it is probably too low to form gas giant planets according to current models .
Despite the fact that PDS 66 is much older than a typical classical T Tauri star ( \leq 5 Myr ) , its physical properties are not much different .