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The Gemini Planet Imager (GPI) is currently in its final Acceptance & Testingstages. GPI is an XAO system based on a tweeter & woofer architecture (43 & 9actuators respectively across the pupil), with the tweeter being a BostonMichromachines $64^2$ MEMS device. The XAO AO system is tightly integrated witha Lyot apodizing coronagraph. Acceptance testing started in February 2013 atthe University of California, Santa Cruz. A conclusive acceptance review washeld in July 2013 and the instrument was found ready for shipment to the GeminiSouth telescope on Cerro Pachon, Chile. Commissioning at the telescope willtake place by the end of 2013, matching the summer window of the southernhemisphere. According to current estimates the 3 year planet finding campaign(890 allocated hours) might discover, image, and spectroscopically analyze 20to 40 new exo-planets. Final acceptance testing of the integrated instrumentcan always bring up surprises when using cold chamber and flexure riginstallations. The latest developments are reported. Also, we will give anoverview of GPI's lab performance, the interplay between subsystems such as thecalibration unit (CAL) with the AO bench. We report on-going optimizations onthe AO controller loop to filter vibrations and last but not least achievedcontrast performance applying speckle nulling. Furthermore, we will give anoutlook of possible but challenging future upgrades as the implementation of apredictive controller or exchanging the conventional 48x48 SH WFS with apyramid. With the ELT era arising, GPI will proof as a versatile andpath-finding testbed for AO technologies on the next generation of ground-basedtelescopes.

Final A&T Stages of the Gemini Planet Finder