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Kepler-14 is a binary star system targeted by the Kepler spacecraft. It is host to one known planet: the Jupiter-like Kepler-14b. The star system was identified by Kepler as a possible planetary host, but when imaging revealed that Kepler-14 was a binary star system and not a single star, the confirmation process became protracted. The stars are separated by at least 280 AU, and the stars complete an orbit around a common center of mass every 2800 years. Both stars are larger than the Sun. They are of similar absolute magnitudes; however, the primary star is brighter as seen from Earth. ==Observational history== Kepler-14 was identified as a possible host to a planet during the first four months of Kepler's operational data, which began when NASA launched the satellite in April 2009. Kepler-14 was provisionally designated KOI-98. Because Kepler-14's transit signal seemed to imply that the possible planet had a short orbit and a clear effect on Kepler-14's brightness, the Kepler science team forwarded the candidate to the Kepler Follow-up Program (KFOP).〔 KFOP used the Fibre-fed Échelle Spectrograph (FIES) on the Nordic Optical Telescope to measure Kepler-14's radial velocity in October 2009. Other radial velocity measurements were collected using W.M. Keck Observatory. The FIES and Keck data, combined with speckle imaging data from WIYN Observatory and near-infrared adaptive optics measurements at Palomar Observatory and the MMT Observatory, revealed that Kepler-14 was actually a close binary star, something that radial velocity data alone could not recognize. Because of this new discovery, further investigation of Kepler-14 was postponed until after the publishing of the first five new Kepler planets (the ones orbiting Kepler-4, Kepler-5, Kepler-6, Kepler-7, and Kepler-8).〔 Analysis of the data revealed that, of the two component stars in the Kepler-14 system, both stars are of nearly equal magnitude, although one of the stars was fainter. The brighter star was designated the "A" component, and the fainter star received the "B" designation. The transit signal was observed in orbit around the A component of the system, meaning that the planetary candidate would be in orbit of the primary star of Kepler-14. This was confirmed on August 7, 2010, when the Infrared Array Camera on the Spitzer Space Telescope observed Kepler-14 to gather photometric data.〔 Analysis of both the Spitzer photometric data and the radial velocity data confirmed the idea of a planet as the source of the transit signal.〔 The planet was designated Kepler-14b, and this was published alongside the data and research on Kepler-14 in a June 2011 paper.〔 Kepler-14's nature as a close binary star was almost missed by the astronomers, and would not have been known if high-resolution imaging of the star had not been undertaken. The Kepler team acknowledged that a number of transiting planets' host stars may have actually been close visual binaries, and that the assumed characteristics of the stars and their planets may be incorrect. As a result of their studies into Kepler-14, the Kepler team suggested the implementation of a high-resolution imaging campaign to re-examine transiting planet hosts, an effort which would require only a modest amount of telescope time.〔 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「Kepler-14」の詳細全文を読む スポンサード リンク
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