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We present Gemini Planet Imager (GPI) adaptive optics near-infrared images ofthe giant planet-forming regions of the protoplanetary disk orbiting the nearby(D = 54 pc), pre-main sequence (classical T Tauri) star TW Hydrae. The GPIimages, which were obtained in coronagraphic/polarimetric mode, exploitstarlight scattered off small dust grains to elucidate the surface densitystructure of the TW Hya disk from 80 AU to within 10 AU of the star at 1.5 AUresolution. The GPI polarized intensity images unambiguously confirm thepresence of a gap in the radial surface brightness distribution of the innerdisk. The gap is centered near 23 AU, with a width of 5 AU and a depth of 50%.In the context of recent simulations of giant planet formation in gaseous,dusty disks orbiting pre-main sequence stars, these results indicate that atleast one young planet with a mass 0.2 M_J could be present in the TW Hya diskat an orbital semi-major axis similar to that of Uranus. If this (proto)planetis actively accreting gas from the disk, it may be readily detectable by GPI ora similarly sensitive, high-resolution infrared imaging system.

Peering into the Giant Planet Forming Region of the TW Hydrae Disk with the Gemini Planet Imager