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OGLE-TR-111 is a yellow dwarf star approximately 5,000 light-years away in the constellation of Carina. Having an apparent magnitude of about 17, this distant and dim star has not yet been cataloged. Because its apparent brightness changes when one of its planets transits, the star has been given the variable star designation V759 Carinae.
Gravitational microlensing is an astronomical phenomenon due to the gravitational lens effect. It can be used to detect objects that range from the mass of a planet to the mass of a star, regardless of the light they emit. Typically, astronomers can only detect bright objects that emit much light (stars) or large objects that block background light. These objects make up only a minor portion of the mass of a galaxy. Microlensing allows the study of objects that emit little or no light.
OGLE-2005-BLG-390Lb is a super-Earth exoplanet orbiting OGLE-2005-BLG-390L, a star 21,500 ± 3,300 light years from Earth near the center of the Milky Way, making it one of the most distant planets known. On 25 January 2006, Probing Lensing Anomalies NETwork/Robotic Telescope Network (PLANET/Robonet), Optical Gravitational Lensing Experiment (OGLE), and Microlensing Observations in Astrophysics (MOA) made a joint announcement of the discovery. The planet does not appear to meet conditions presumed necessary to support life.
OGLE-2005-BLG-390L is a star thought to be a spectral type M. This dim magnitude 16 galactic bulge star is located in the Scorpius constellation at a far distance of about 21,500 light years.
OGLE-2003-BLG-235/MOA 2003-BLG-53 was a gravitational microlensing event which occurred in the constellation of Sagittarius during July 2003. The event was observed both as part of the Optical Gravitational Lensing Experiment (OGLE) and by the Microlensing Observations in Astrophysics group (MOA), hence the double designation. The source star in the gravitational lens is a main sequence star of spectral type G located around 8.8 kiloparsecs away in the galactic bulge. The lens star is an orange dwarf star of spectral type K, which is accompanied by a giant planet.
MACHO-1997-BLG-41, commonly abbreviated as 97-BLG-41 or MACHO-97-BLG-41, was a gravitational microlensing event located in Sagittarius which occurred in July 1999. The source star is likely a giant or subgiant star of spectral type K located at a distance of around 8 kiloparsecs. The lens star is a binary system approximately 10,000 light-years away in the constellation Sagittarius. The two stars are separated from each other by about 0.9 AU and have an orbital period of around 1.5 years. The most likely mass of the system is about 0.3 times that of our Sun. Star A and star B are both red dwarfs.
OGLE-2005-BLG-169Lb is an extrasolar planet located approximately 2700 parsecs away in the constellation of Sagittarius, orbiting the star OGLE-2005-BLG-169L. This planet was discovered by the OGLE project using the gravitational microlensing method. Based on a most likely mass for the host star of 0.49 solar mass (M☉), the planet has a mass of 13 times that of Earth (MEarth). Its mass and estimated temperature are close to those of Uranus. It is speculated that this planet may either be an ice giant like Uranus, or a "naked super-Earth" with a solid icy or rocky surface.
OGLE-TR-113 is a dim, distant magnitude 16 binary star in the star fields of the constellation Carina. Because of its distance of about 1170 light years, and location in a crowded field it was not notable in any way. Its apparent brightness changes when one of its planets transits, so the star has been given the variable star designation V752 Carinae. Spectral type of the star is type K dwarf star, slightly cooler and less luminous than the Sun.
OGLE-2005-BLG-071L is a distant, magnitude 19.5 galactic bulge star located in the constellation Scorpius, approximately 11000 light years away from the Solar System. The star is probably a red dwarf with a mass 46% of that of our Sun.
OGLE-2006-BLG-109L is a dim magnitude 17 M0V galactic bulge star approximately 4,920 light-years away in the constellation of Scorpius.
OGLE-2006-BLG-109Lc is an extrasolar planet approximately 4,920 light-years away in the constellation of Sagittarius. The planet was detected orbiting the star OGLE-2006-BLG-109L in 2008 by a research team using Microlensing. The host star is about 50% the mass of the Sun and the planet is about 90% the mass of Saturn.
OGLE-2005-BLG-071Lb is a planet discovered by the Optical Gravitational Lensing Experiment (OGLE) and others in 2005, using gravitational microlensing. According to the best fit model, it has about 3.5 times the mass of Jupiter and a projected separation of 3.6 astronomical units from the star. This would result in an effective temperature around 50 K, similar to that of Neptune. However, an alternative model which gives a slightly lower mass of 3.3 times that of Jupiter and a projected separation of 2.1 AU is only slightly less likely. It may be the most massive planet currently known around a red dwarf star.
MOA-2007-BLG-192L is a low-mass red dwarf star or brown dwarf, approximately 3,000 light-years away in the constellation of Sagittarius. It is estimated to have a mass approximately 6% of the Sun's. In 2008, an Earth-sized extrasolar planet was announced to be orbiting this object.
OGLE-TR-111b is an extrasolar planet approximately 5,000 light-years away in the constellation of Carina. The planet is currently the only confirmed planet orbiting the star OGLE-TR-111.
OGLE-2007-BLG-368Lb is an extrasolar planet located approximately 19,230 light-years away in the constellation of Scorpius, orbiting the star OGLE-2007-BLG-368L. This planet was detected on December 8, 2009 by the gravitational microlensing by Sumi. It has mass 6.94% of Jupiter and is located 3.3 AU from the star when observed. Based on those properties it would classify as a Cold Neptune. It is the second Cold Neptune to be observed, the first being OGLE-2005-BLG-169Lb. This planet is most likely be similar to Uranus and Neptune in the Solar System in terms of atmospheric and internal properties.
The Microlensing Follow-Up Network is an informal group of observers who monitor high magnification gravitational microlensing events in the Milky Way's Galactic Bulge. Its goal is to detect extrasolar planets via microlensing of the parent star by the planet. μFUN is a follow-up network - they monitor microlensing events identified by survey groups such as OGLE and Microlensing Observations in Astrophysics (MOA).
OGLE-2007-BLG-349(AB)b is a circumbinary extrasolar planet about 8,000 light-years away in the constellation of Sagittarius. It is the first circumbinary exoplanet to be discovered using the microlensing method of detecting exoplanets.
OGLE-2016-BLG-1195Lb is an extrasolar planet located nearly 13,000 light-years from Earth, orbiting the star OGLE-2016-BLG-1195L, which is only 7.8 percent the size of the Sun. This planet was detected in 2017 using gravitational microlensing techniques managed by the Korea Astronomy and Space Science Institute and the Spitzer Space Telescope. It has a mass similar to Earth and is located about the same distance from its host star as the Earth is from the Sun. However, the host star is so small that it may not be a star at all. It may be "a brown dwarf or an ultracool dwarf" instead, so the planet is likely far too cold to be habitable. Based on its currently observed properties, the 'iceball' planet may be described as a very cold Earth-like exoplanet.
OGLE-2016-BLG-1190Lb is an extremely massive exoplanet, with a mass about 13.4 times that of Jupiter (MJ), or is, possibly, a low mass brown dwarf, orbiting the G-dwarf star OGLE-2016-BLG-1190L, located about 22,000 light years from Earth, in the constellation of Sagittarius, in the galactic bulge of the Milky Way.
References
- 1 2 3 4 5 "SIMBAD query result: NAME OGLE 2005-BLG-169 -- Star". Centre de Données astronomiques de Strasbourg . Retrieved 2009-04-30.
- ↑ Gould, A.; et al. (2006). "Microlens OGLE-2005-BLG-169 Implies That Cool Neptune-like Planets Are Common". The Astrophysical Journal Letters. 644 (1): L37–L40. arXiv: astro-ph/0603276 . Bibcode:2006ApJ...644L..37G. doi:10.1086/505421. S2CID 14270439.
