HD 149026 b, formally named Smertrios, is an extrasolar planet approximately 250 light-years from the Sun in the constellation of Hercules.
Chi Virginis is a double star in the constellation Virgo. Based upon parallax measurements, it is approximately 294 light-years from Earth. It has an apparent visual magnitude of 4.65, which is bright enough to be seen with the unaided eye under suitable viewing conditions.
Upsilon Andromedae d (υ Andromedae d, abbreviated Upsilon And d, υ And d), formally named Majriti, is a super-Jupiter exoplanet orbiting within the habitable zone of the Sun-like star Upsilon Andromedae A, approximately 44 light-years (13.5 parsecs, or nearly 4.163×1014 km) away from Earth in the constellation of Andromeda. Its discovery made it the first multiplanetary system to be discovered around a main sequence star, and the first such system known in a multiple star system. The exoplanet was found by using the radial velocity method, where periodic Doppler shifts of spectral lines of the host star suggest an orbiting object.
HD 69830 d is an exoplanet likely orbiting within the habitable zone of the star HD 69830, the outermost of three such planets discovered in the system. It is located approximately 40.7 light-years (12.49 parsecs, or 3.8505×1014 km) from Earth in the constellation of Puppis. The exoplanet was found by using the radial velocity method, from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star.
14 Herculis b or 14 Her b is an extrasolar planet approximately 58.5 light-years away in the constellation of Hercules. The planet was found orbiting the star 14 Herculis, with a mass that would likely make the planet a Jovian planet roughly the same size as Jupiter but much more massive. It was discovered in July 1998 by the Geneva Extrasolar Planet Search team. At the time of discovery it was the extrasolar planet with the longest orbital period, though longer-period planets have subsequently been discovered.
HD 11506 is a star in the equatorial constellation of Cetus. It has a yellow hue and can be viewed with a small telescope but is too faint to be visible to the naked eye, having an apparent visual magnitude of 7.51. The distance to this object is 167 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −7 km/s. It has an absolute magnitude of 3.94.
HD 8574 b is an extrasolar planet discovered in 2001 by a team of European astronomers using Doppler spectroscopy as part of the ELODIE Planet Search Survey, and was published in a paper with five other planets. HD 8574 b is in the orbit of host star HD 8574. The planet is at most two times the mass of Jupiter, orbiting every 227 days at three quarters of the distance between the Earth and Sun. HD 8574 b has a very elliptical orbit, far more than that of Jupiter.
HD 205739 is a yellow-white hued star in the southern constellation of Piscis Austrinus, positioned near the western constellation boundary with Microscopium. It has the proper name Sāmaya, which was selected in the NameExoWorlds campaign by Sri Lanka, during the 100th anniversary of the IAU. Sāmaya means peace in the Sinhalese language.
HD 154672 b is an extrasolar planet located approximately 210 light-years away in the constellation of Ara, orbiting the metal-rich and aged star HD 154672. This planet has a minimum mass five times that of Jupiter and orbits at about 60% the distance between the Earth to the Sun. Its orbit is very elliptical, which causes temperatures on the planet to vary significantly as it proceeds along its orbit. This planet was discovered in Las Campanas Observatory on September 5, 2008 using the radial velocity method. Along with HD 205739 b, the planets were the first to be discovered by the N2K Consortium using the Magellan Telescopes.
HD 205739 b is an extrasolar planet located approximately 350 light-years away
HD 153950 b is an extrasolar planet located approximately 162 light-years awayThis planet was discovered on October 26, 2008 by Moutou et al. using the HARPS spectrograph on ESO's 3.6 meter telescope installed at La Silla Observatory in Atacama desert, Chile.
HD 43848 is a 9th magnitude K-type subgiant star located approximately 123 light-years away in the constellation of Columba. The star is less massive than the Sun.
Pirx (BD+14 4559 b) is an exoplanet orbiting the K-type main sequence star Solaris about 161 light-years (49 parsecs, or nearly 1.5×1015 km) from Earth in the constellation Pegasus. It orbits its star within the habitable zone at a distance of 0.777 AU, close to that of Venus, but its star is less energetic, thus its habitable zone is closer to it than Earth. The exoplanet was found by using the radial velocity method, from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star.
The Magellan Planet Search Program is a ground-based search for extrasolar planets that makes use of the radial velocity method. It began gathering data in December 2002 using the MIKE echelle spectrograph mounted on the 6.5m Magellan II "Clay" telescope located within the Las Campanas Observatory in Chile. In 2010, the program began using the newly commissioned Planet Finder Spectrograph (PFS), an instrument purpose-built for precise radial velocity measurement.
The N2K Consortium is a collaborative multinational effort by American, Chilean and Japanese astronomers to find additional extrasolar planets around stars that are not already being surveyed. The N2K is shorthand for the set of roughly 2,000 of the nearest and most luminous main sequence stars that were selected to be newly surveyed. Target stars have a B - V color index value between 0.4 and 1.2, a visual magnitude brighter than 10.5, and a distance of less than 110 pc from the Sun. They were selected based upon their high metallicity, which is the abundance of elements other than hydrogen and helium.
Gliese 3634 b is a super-Earth exoplanet in the orbit of the nearby red dwarf Gliese 3634 at approximately 64.5 light-years in constellation Hydra. The planet is approximately eight times the mass of Earth, and orbits its star every two and a half days at a distance of 0.0287 AU. The planet was the first to be discovered by a group of astronomers searching for exoplanets in the orbit of very-low-mass stars after the team reorganized their strategy, choosing to search for targets that they could also confirm using the transit method. However, a transit event associated with Gliese 3634 b was not detected. The planet's discovery was published in Astronomy and Astrophysics on February 8, 2011.
Gliese 3634 is a red dwarf star in the Hydra constellation. One planet has been discovered in its orbit, Gliese 3634 b. GJ 3634 is under half the mass and size of the Sun, and is estimated to be at least a billion years younger, and lies near to Earth, with a distance of 19.8 parsecs. It was targeted by astronomers during an over six-year survey of red dwarfs. The astronomers had recently changed their strategy to search for planets with extremely short orbits so they could narrow down candidates that transited, or crossed in front of, their host stars as seen from the Earth. The Super-Earth GJ 3634 b was the first planet discovered using this new strategy. The planet was confirmed using Doppler spectroscopy, or the observation and extrapolation of data from a recorded Doppler effect in the star's light, but later observations found no transiting pattern. The planet was published by its discoverers on February 8, 2011.
WASP-24b is a Hot Jupiter detected in the orbit of the F-type star WASP-24. The planet is approximately the same size and mass of Jupiter, but it orbits at approximately 4% of the mean distance between the Earth and the Sun every two days. WASP-24b was observed by SuperWASP starting in 2008; after two years of observations, follow-ups led to the collection of the information that led to the planet's discovery.
HD 240237 b is a super-Jupiter exoplanet orbiting the K-type giant star HD 240237 about 4,900 light-years (1,500 parsecs, or nearly 4.6×1016 km) away from Earth in the constellation Cassiopeia. It orbits outside of the habitable zone of its star at a distance of 1.9 AU. The exoplanet was found by using the radial velocity method, from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star. The planet has a mildly eccentric orbit.
HD 131399 is a star system in the constellation of Centaurus. Based on the system's electromagnetic spectrum, it is located around 351 light-years away. The total apparent magnitude is 7.07, but because of interstellar dust between it and the Earth, it appears 0.22 ± 0.09 magnitudes dimmer than it should be.
