and Canadian institutions, funded by the Gemini Observatory, which is an international partnership comprising the U.S.A., U.K., Canada, Australia, Argentina, Brazil & Chile. WHEN: First light and science operations are planned for mid-2012. GPI successfully held its preliminary design review (PDR) in May 2007 and critical design review (CDR) in May 2008. A delta CDR was successful in March, 2009.
GPI is currently in a phase of procurement and fabrication with testing and integration through 2011. The readiness review will be held in Spring 2011 and will be followed by delivery around June 2012. WHERE: Initial deployment at Gemini South, a telescope with an 8-meter diameter mirror located on Cerro Pachon (Chilean Andes) at an altitude of 2715 meters (9000 feet). Later, GPI may also be used at the twin facility Gemini North, which is located on Mauna Kea, Hawaii. WHY: We want to directly detect the light from an extrasolar planet to determine its mass and composition, with an ultimate goal of determining the nature of our own planetary system. More than 200 extrasolar planets are now known, but mostly through indirect Doppler techniques that indicate the planet's mass and orbit. If we can directly pick out a planet from the star's glare, we can use spectroscopy to measure the planet's size, temperature, gravity, and even the composition of its atmosphere. By targeting many stars we will understand how common or unusual our own planetary system may be. HOW: We will create advanced adaptive optics using silicon microchip deformable mirrors to remove atmospheric turbulence, and coronagraphic masks to block the diffracted light from the parent star. WHAT: GPI will provide diffraction limited images between 0.9 and 2.4 microns. Bright natural guide stars (I
