The study of exoplanets is one of the most dynamic emerging fields of science, and these values may change as new discoveries are made.
[10][11][12][13] An Earth-mass planet claimed to orbit Alpha Centauri B (apparent magnitude = 1.33) was subsequently refuted.
2MASS J04414489+2301513 b is listed as the youngest planet in the NASA Exoplanet Archive, at an age of 1 Myr,[1] but fails the mass ratio criterion of the IAU working definition of an exoplanet; the mass ratio with the primary is larger than the L4/L5 limit of stability ≈ 1/25[56] and 'more likely to have been produced by cloud core fragmentation' (similar to a star).
[58] CI Tauri c would be the youngest radial velocity planet at an age of 2–3 Myr, if confirmed.
[64] A brown dwarf or massive planetary companion was announced around the population II star HE 1523-0901, whose metallicity is −2.65±0.22 dex.
[67] A disputed substellar companion, possibly a Jovian planet, was announced to orbit[92] the B-type subdwarf star HD 149382 with a metallicity of -1.30 dex.
[13] Candidate planets were reported around the cool giants R Leonis (at 3537 L☉)[104], R Fornacis (at 5800 L☉)[101], BD+20°2457 (at 1479 L☉)[113][90], V Hydrae (at 18000 L☉)[114][103] and L2 Puppis (at 1490±150 L☉)[115][24].
The stars R126, R66 and HH 1177 in the Large Magellanic Cloud have luminosities of 1400000 L☉, 320000 L☉ and 19000 L☉[105][97] and have dust discs but no planets have been detected yet.
[102][99] A gas giant planet was found orbiting TVLM 513-46546,[123] which is an ultracool star (2242 K) located close to the brown dwarf/red dwarf mass boundary.
30 Arietis Bb was believed to be either brown dwarf or a massive gas giant in a quadruple star system until later studies revealed a true mass well above 80 MJup.
[131] The quintuple star system GG Tauri has several protoplanetary disks but no planets have been detected yet.
[132] Similarly, the star β3 Tucanae A, located in a sextuple system, was suggested to have a debris disk with no planets having been found.