HD 126614
HD 126614 is a trinary star system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81, it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −33 km/s. The primary is a late G-type star with a stellar classification of G8IV. It is a super metal-rich star; among the most metal -rich stars currently known. Because of its temperature and mass, this is most likely an evolving subgiant star rather than a main sequence star. In 2010, a close stellar companion was resolved and designated component B. This object is a faint red dwarf at an angular separation of , which corresponds to a projected physical separation of . The outer companion, component C, was first reported in 1960 with the W. J. Luyten proper motion catalog. It is a magnitude 17.0 red dwarf with a class of M5.5, located at an angular separation of from the primary along a position angle of  299°, as of 2015. They have a physical projected separation of . The common proper motion of the system has been confirmed, indicating that they are gravitationally bound. A Doppler search for giant planets begun in 1997 at the Keck Observatory provided an 11 year baseline for detecting periodicity in the primary's radial velocity data. In 2010, a Jovian companion was announced with an orbital period of .