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The Next-Generation Transit Survey (NGTS) is a ground-based robotic search for exoplanets. The facility is located at Paranal Observatory on the outskirts of the Atacama desert in northern Chile, a few kilometers from ESO's Very Large Telescope and near the VISTA Survey Telescope. Science operations began in early 2015. The aim of NGTS is to discover super-Earths and exo-Neptunes transiting relatively bright and nearby stars with an apparent magnitude of up to 13. The survey uses transit photometry, which precisely measures the dimming of a star to detect the presence of a planet when it crosses in front of it. NGTS consists of an array of twelve commercial 0.2-metre telescopes (f/2.8), each equipped with a red-sensitive CCD camera operating in the visible and near-infrared at 600–900 nm. The array covers an instantaneous field of view of 96 square degrees (8 deg2 per telescope) or around 0.23% of the entire sky.〔 NGTS builds heavily on the experience of its predecessor, SuperWASP, using more sensitive detectors, refined software, and improved optics. Compared to the ''Kepler'' spacecraft with its fixed field of view of 115 square degrees, the sky area covered by NGTS will be sixteen times larger, because the survey intends to scan four different fields every year over a period of four years. As a result, the number of discovered nearby exoplanets will be much larger. NGTS is designed to fill the current gap between Earth-sized planets and gas giants. Although other ground-based surveys could only detect larger, Jupiter-sized exoplanets, ''Keplers Earth-sized planets are often too far away or orbit stars too dim to allow for doppler spectroscopy—a different detection method to determine the planet's mass by the wobble of its host star. NGTS's wider field of view enables it to detect a larger number of more-massive planets around brighter stars. With a detailed follow-up characterization by larger instruments such as HARPS, ESPRESSO and VLT-SPHERE, it will be possible to measure the mass of a large number of targets using this wobble method. This makes it possible to determine the exoplanet's density, and hence whether it is gaseous or rocky. The survey is managed by a consortium of seven European universities and other academic institutions from Chile, Germany, Switzerland, and the United Kingdom.〔(【引用サイトリンク】publisher=Next Generation Transit Survey )〕 Prototypes of the array were tested in 2009 and 2010 on La Palma, and from 2012 to 2014 at the Geneva Observatory.〔 == Science mission == Ground-based surveys for extrasolar planets such as WASP and the HATNet Project have discovered many large exoplanets, mainly Saturn- and Jupiter-sized gas giants. Space-based missions such as CoRoT and the ''Kepler'' survey have extended the results to smaller objects, including rocky super-Earth- and Neptune-sized exoplanets.〔 Orbiting space missions have a higher accuracy of stellar brightness measurement than is possible via ground-based measurements, but they have probed a relatively small region of sky. Unfortunately, most of the smaller candidates orbit stars that are too faint for confirmation by radial-velocity measurements. The masses of these smaller candidate planets are hence either unknown or poorly constrained, such that their bulk composition cannot be estimated.〔 By focusing on super-Earth- to Neptune-sized targets orbiting cool, small, but bright stars of K and early-M spectral type, over an area considerably larger than that covered by space missions, NGTS is intended to provide prime targets for further scrutiny by telescopes such as the Very Large Telescope (VLT), European Extremely Large Telescope (E-ELT), and the James Webb Space Telescope (JWST). Such targets are more readily characterized in terms of their atmospheric composition, planetary structure, and evolution than smaller targets orbiting larger stars.〔 In follow-up observations by larger telescopes, powerful means will be available to probe the atmospheric composition of exoplanets discovered by NGTS. For example, during secondary eclipse, when the star occults the planet, a comparison between the in-transit and out-of-transit flux allows computation of a difference spectrum representing the thermal emission of the planet.〔(【引用サイトリンク】url=http://www.ngtransits.org/science.shtml )〕 Calculation of the transmission spectrum of the planet's atmosphere can be obtained by measuring the small spectral changes in the spectrum of the star that arise during the planet's transit. This technique requires an extremely high signal-to-noise ratio, and has thus far been successfully applied to only a few planets orbiting small, nearby, relatively bright stars, such as HD 189733 b and GJ 1214 b. NGTS is intended to greatly increase the number of planets that are analyzable using such techniques.〔 Simulations of expected NGTS performance reveal the potential of discovering approximately 231 Neptune- and 39 super-Earth-sized planets amenable to detailed spectrographic analysis by the VLT, compared to only 21 Neptune- and 1 super-Earth-sized planets from the ''Kepler'' data.〔 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「Next-Generation Transit Survey」の詳細全文を読む スポンサード リンク
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