OGLE-TR-111 b is an extrasolar planet orbiting star OGLE-TR-111.
In 2002 the Optical Gravitational Lensing Experiment (OGLE) survey detected that the light from the star periodically dimmed very slightly every 4 days, indicating a planet-sized body transiting the star. But since the mass of the object had not been measured, it was not clear if it was a true planet, low-mass red dwarf or something else. In 2004 radial velocity measurements showed unambiguously that the transiting body is indeed a planet.
The planet is probably very similar to the other "hot Jupiters" orbiting nearby stars. Its mass is about half that of Jupiter and it orbits the star at a distance less than 1/20th that of Earth from the Sun.
OGLE-TR-111 b has similar mass and orbital distance as the first transiting planet, HD 209458 b (dubbed "Osiris"). But unlike it, the planet has a radius comparable to Jupiter which is typical to other transiting planets detected by OGLE. However, those other planets tend to be more massive and orbit even closer than typical "hot Jupiters". Therefore this planet is an important "missing link" between the different types of transiting planets.
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