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List of exoplanets detected by microlensing

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This is a list of exoplanets detected by gravitational microlensing. The phenomenon results in the background star's light being warped around a foreground object, causing a distorted image. If the foreground object is a star with an orbiting planet, we would observe an abnormally bright image. By comparing the luminosity and light distortion of the background star to theoretical models, we can estimate the planet's mass and the distance from its star.

The least massive planet detected by microlensing is KMT-2020-BLG-0414Lb, which has a mass about 0.960 times the mass of earth, or OGLE-2016-BLG-0007Lb, which has a mass about 1.32 times the mass of earth.[1][2] The widest separation between a planet and a star is OGLE-2008-BLG-092Lb, which is 15 AU; the shortest separation is KMT-2020-BLG-0414Lc, which is 0.12 AU.[3][4] There are 7 known multi-planetary systems detected by microlensing, all of which have two planets.[5]

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Yellow rows denote the members of multi-planet systems. Green rows denote the members of multi-star systems.

More information Planet, Mass (MJ) ...

Candidate rogue planets

A number of candidate rogue planets have been detected by microlensing.

More information Planet, Mass ...

Unconfirmed detections

Some microlensing events, such as MACHO-98-BLG-35 and PA-99-N2, suggest the possible presence of a planetary companion to the lensing star, but this is unconfirmed. Since microlensing relies on a one-time chance alignment, it is likely not possible to confirm these detections.

In some cases, a planetary interpretation for a microlensing event was proposed, but has been disproven. MACHO-1997-BLG-41 was initially interpreted as a binary star system orbited by a circumbinary planet, but a different model with two stars and no planet was later found to be a better fit to the data. Similarly, OGLE-2013-BLG-0723L was initially interpreted as a binary system of a star and a brown dwarf, with a low-mass planet orbiting the brown dwarf, but a model where the system consists of two low-mass stars with no planet was found to be a better fit to the data.[186]

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Notes

  1. The nature of the observed system is unclear. It is either a rogue planet with about 3.2 MJ masses and a 0.5 M🜨 exomoon or a red dwarf with 18 M🜨 planet.

References

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