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Gemini Planet Imager
The Gemini Planet Imager (GPI) is a high contrast imaging instrument that was built for the Gemini South Telescope in Chile. The instrument achieves high contrast at small angular separations, allowing for the direct imaging and integral field spectroscopy of extrasolar planets around nearby stars.〔Macintosh ''et al.'' (2006), p. 1.〕 The collaboration involved in planning and building the Gemini Planet imager includes the American Museum of Natural History (AMNH), Dunlap Institute, Gemini Observatory, Herzberg Institute of Astrophysics (HIA), Jet Propulsion Laboratory, Lawrence Livermore National Lab (LLNL), Lowell Observatory, SETI Institute, The Space Telescope Science Institute (STSCI), the University of Montreal, University of California, Berkeley, University of California, Los Angeles (UCLA), University of California, Santa Cruz (UCSC), University of Georgia.〔(【引用サイトリンク】 GPI: Gemini Planet Imager )〕
==Specifications==
The Gemini Planet Imager is being used at the Gemini South Telescope, located in Cerro Pachon, Chile. It saw the first light in November 2013, and entered regular operations in November 2014.〔 It is designed to directly detect young gas giants via their thermal emission. It will operate at near-infrared wavelengths (Y - K bands), where planets will be reasonably bright, but thermal emission from the Earth's atmosphere is not too strong.〔Graham ''et al.'' (2007), p 2.〕
The system consist of multiple components, including a high-order adaptive optics system, a coronagraph, a calibration interferometer, and an integral field spectrograph. The adaptive optics system, being built at LLNL, uses a MEMS deformable mirror from Boston Micromachines Corporation to correct wavefront errors induced by motion of air in the atmosphere and the optics in the telescope. The coronagraph, being built at AMNH, blocks out the light from the star being observed, which is necessary in order to see a much dimmer companion. Before sending the GPI at Gemini South it was essential to test the coronagraph by reproducing the exact experimental conditions in which it was going to be used. Photon etc. tunable laser source was use for this matter and helped determine that at its efficiency peak of wavelength, the imager could detect a planet only slightly more massive than Jupiter around a 100-million-year-old Sun-like star. The spectrograph, developed by UCLA and Montreal, images and takes spectra of any detected companion to the star, with a spectral resolving power of 34 - 83, depending on wavelength. The expected instrument performance will allow for detection of companions one ten millionth as bright as their hosts at angular separations of roughly 0.2-1 arcseconds, down to an H band magnitude of 23.〔Macintosh ''et al.'' (2006), p. 3.〕
抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』
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