List of exoplanet extremes

The following are lists of extremes among the known exoplanets. The properties listed here are those for which values are known reliably.

Extremes from Earth's viewpoint
Title Planet Star Data Notes
Most distant discovered SWEEPS-11 / SWEEPS-04 SWEEPS J175902.67−291153.5 27,710 light-years.[1]
See also: Extragalactic planet
An analysis of the lightcurve of the microlensing event PA-99-N2 suggests the presence of a planet orbiting a star in the Andromeda Galaxy (2.54 ± 0.11 Mly).[2] In late January 2018,[3] a team of scientists led by Xinyu Dai claimed to have discovered a collection of about 2,000 rogue planets in the quasar microlens RX J1131-1231, which is 3.8 billion light-years distant. The bodies range in mass from that of the Moon to several Jupiter masses.[4][3]

The most distant potentially habitable planet confirmed is Kepler-1606b, at 2870 light-years distant,[5] although the unconfirmed planet KOI-5889.01 is over 5,000 light-years distant.

Least distant Proxima Centauri b and c Proxima Centauri 4.22 light years Proxima Centauri b is the closest rocky exoplanet and closest potentially habitable exoplanet known, and c is the closest super-Earth and potentially-ringed planet. As Proxima Centauri is the closest star to the Sun (and will stay so for the next 25,000 years), this is an absolute record.
Most distant directly visible CVSO 30 c CVSO 30 1,200 light-years Also first directly imaged planet in system with a transiting planet.
Least distant directly visible Proxima Centauri c Proxima Centauri 4.22 light-years Confirmed in 2020 using archival Hubble data from 1995+.
Star with the brightest apparent magnitude with a planet Pollux b Pollux[6] Apparent magnitude is 1.14 The evidence of planets around Vega with an apparent magnitude of 0.03 is strongly suggested by circumstellar disks surrounding it. As of 2018, no planets had yet been confirmed.[7]
Largest angular distance separation from its host star GU Piscium b GU Piscium 42 arc seconds[8] The upper mass limit (13 Jupiter masses) may make this a brown dwarf. WD 0806-661 b has an angular separation of 130.2 arc seconds from WD 0806-661. However, its planetary origin is also unknown. Not counting either of these, DT Virginis b would be the widest-separated definite exoplanet.

Planetary characteristics
Title Planet Star Data Notes
Least massive WD 1145+017 b WD 1145+017 0.00067 M🜨[9]
Least massive in proportion to the mass of the star(s) it revolves around
Most massive The candidate for the most massive planet is contentious, as it is difficult to distinguish between a highly massive planet and a brown dwarf. It is estimated the largest planets are approximately a dozen Jupiter masses.
Most massive in proportion to the mass of the star(s) it revolves around
Largest radius HD 100546 b HD 100546 6.9+2.7
−2.9[10] Jupiter radii		 Largest exoplanet in the NASA Exoplanet Archive, although because of flux from the planet and the disk that are superimposed, the exact size of this planet cannot be determined and the emitting area has this size, composed of the planet and including its disk, not to be mistaken as a single planet radius. Over time, it will shrink to the size of Jupiter. 20 MJ; is likely a brown dwarf.
Smallest radius SDSS J1228+1040 b SDSS J1228+1040 128.6856 km (diameter)[11]
Most dense Kepler-131c Kepler-131 77.7+55
−55 g/cm3[12]		 Highly uncertain
Least dense Kepler-51c, b and/or possibly d[13] Kepler-51[13] ~ 0.03 g/cm3[13] The densities of Kepler-51 b and c have been constrained to be below 0.05 g/cm3 (expected value 0.03 g/cm3 for each). The density of Kepler-51d is determined to be 0.046±0.009 g/cm3.[13]
Hottest Kepler-70b Kepler-70 >7,000 K[14]
Coldest OGLE-2016-BLG-1195Lb OGLE-2016-BLG-1195L 31 K
Highest albedo Kepler-1658b Kepler-1658 0.758[15](geometric albedo)
Lowest albedo TrES-2b GSC 03549-02811 Geometric albedo < 1%[16] Best-fit model for albedo gives 0.04% (0.0004)[14]
Youngest Proplyd 133-353 Proplyd 133-353 0.5 Myr[17][18] The upper mass limit (13 Jupiter masses) may make this a brown dwarf.
Oldest PSR B1620-26 b PSR B1620-26 13 Gyr Orbits in a circumbinary orbit around two stellar remnants – a pulsar and a white dwarf. Kapteyn b is the oldest potentially habitable exoplanet at 11 Gyr.[19]

Orbital characteristics
Title Planet Star Data Notes
Longest orbital period
(Longest year)		 COCONUTS-2b COCONUTS-2A 1,100,000 years[20] 2MASS J2126–8140 previously held record at ~900,000 years.
Shortest orbital period
(Shortest year)		 SWIFT J1756.9-2508 b SWIFT J1756.9-2508 48 minutes, 56.5 seconds[21] K2-137b has the shortest orbit around a main-sequence star (an M dwarf) at 4.31 hours.[22]
Most eccentric orbit HD 20782 b[23] HD 20782 0.956±0.004 [24]Record among confirmed planets. Putative satellite of VB 10 may have higher eccentricity of 0.98.[25]
Largest orbit around a single star 2MASS J2126–8140 TYC 9486-927-1 6900AU (projected separation) The upper mass limit (13 Jupiter masses) may make this a brown dwarf. Next largest are COCONUTS-2b with 6471 AU and HD 106906 b[26] with ~738 AU
Smallest orbit WD 1202-024 B WD 1202-024 0.0021 AU
Smallest orbit around binary star Kepler-47b Kepler-47AB ≃0.3 AU [27]
Smallest ratio of semi-major axis of a planet orbit to binary star orbit Kepler-16b Kepler-16AB 3.14 ± 0.01 [28]
Largest orbit around binary star DT Virginis c DT Virginis 1,168 AU Star system is also known as Ross 458 AB. The planet was eventually confirmed to be below deuterium burning limit but its formation origin is unknown.
Largest orbit around a single star in a multiple star system Fomalhaut b Fomalhaut 115 AU The second stellar component of the system, TW Piscis Austrini, has a semi-major axis of 57,000 AU from Fomalhaut and the third stellar component, LP 876-10 orbits 158,000 AU away from Fomalhaut.
Largest distance between binary stars with a circumbinary planet FW Tauri AB b FW Tau AB ≈11 AU FW Tauri AB b orbits at a distance of 150-300 AU.[29]
Closest orbit between stars with a planet orbiting one of the stars OGLE-2013-BLG-0341LBb OGLE-2013-BLG-0341LB ~12–17 AU
(10 or 14 AU projected distance)[30]		 OGLE-2013-BLG-0341L b's semi-major axis is 0.7 AU.[30]
Smallest semi-major axis difference between consecutive planets Kepler-70b and Kepler-70c[14] Kepler-70 0.0016 AU (about 240,000 km) During closest approach, Kepler-70c would appear 5 times the size of the Moon in Kepler-70b's sky.
Smallest semi-major axis ratio between consecutive planets Kepler-36b and Kepler-36c Kepler-36 11% Kepler-36b and c have semi-major axes of 0.1153 AU and 0.1283 AU respectively, c is 11% further from star than b .
Largest semi-major axis difference between consecutive planets
Largest semi-major axis ratio between consecutive planets

Stellar characteristics
Title Planet Star Data Notes
Highest metallicity HD 126614 Ab HD 126614 A +0.56 dex Located in a triple star system.
Lowest metallicity Kapteyn b Kapteyn's Star −0.99±0.04 dex BD+20°2457 may be the lowest metallicity planet host ([Fe/H]=−1.00), however the proposed planetary system is dynamically unstable.[31] After Kapteyn's Star, the next lowest-metallicity system is Kepler-271, at -0.951 dex. Planets were announced around even the extremely low metallicity stars HIP 13044 and HIP 11952, however these claims have since been disproven.[32]
Highest stellar mass M51-ULS-1b M51-ULS-1[33] 50< M☉ M51-ULS-1b is listed as a candidate planet with 4 sigma confidence, and likely to be confirmed as a planet in the near future. The host is a massive O-class supergiant and a black hole orbiting each other at 0.8 AUs, with a combined system mass of >60 solar masses. The planet is a Saturn sized (0.72 Jupiter radii) object orbiting the black-hole/supergiant binary at 10 AU. The host stars giving a combined 1 million solar luminosities off, the planet receives the equivalent irradiation of 51 Pegasi b, which orbits its star at 0.045 AU. M51-Uls-1b would also be one of the youngest planets ever discovered, with a system age of <10 million years according to evolutionary models

Because M51-ULS-1b requires further confirmation, the object V921 Sco b, a 60 Jupiter mass object orbiting a 20 solar mass 30,000K Herbig Haro B0IV class subgiant at 835 AU, may actually be the record holder. Despite the large distance, V921 Sco b receives a comparable amount of irradiation as Mars, owing to the large mass and luminosity of the host star. At 20 solar masses, V921 Sco is the most massive object to host a substellar object. Normally, V921 Sco b would be considered a brown dwarf, but given the high mass of the host star, and the growing studies that confirm the correlation of more massive planets around more massive stars, it is likely that this object may indeed be a planet. Hatzes and Rauer quote an upper limit of 60 Jupiter masses for a core-accretion formation of high mass gas giants, which is how heavy this object is. Furthermore, the Extrasolar Planets Encyclopedia lists objects up to 65 Jupiter masses as planets if they orbit stars.

[34] the stars R126 and R66 in the LMG have masses of 70 and 30 solar masses and have dust discs but no planets have been detected yet.

Lowest stellar mass (main sequence) 2MASS J1119-1137 2MASS J1119–1137 0.0033 M☉ The system 2MASS J1119-1137 AB is a pair of binary rogue planets approximately 3.7 Jupiter masses each.[35]

The least massive main sequence star with known planets is OGLE-2016-BLG-1195L, at 0.078 M☉.

Lowest stellar mass (main sequence star) VHS 1256-1257 b VHS 1256-1257 0.07 M☉
Lowest stellar mass (brown dwarf) 2M J044144 b[36] 2M J044144[36] 0.02 M☉[36]
Largest stellar radius R Leonis b R Leonis 299 or 320-350 R☉[37][38] Star is a Mira variable.
Smallest stellar radius (main sequence star) VB 10 b VB 10 0.102 R☉[39]
Smallest stellar radius (brown dwarf) 2M 0746+20 b[40] 2M 0746+20 0.089 (± 0.003) R☉ Planet's mass is very uncertain at 30.0 (± 25.0) Mjup.
Smallest stellar radius (pulsar) PSR J1719-1438 b[41] PSR J1719-1438 0.04 R☉
Oldest star HD 164922 b HD 164922[42] 13.4 billion years[42]
Hottest star with a planet M51-ULS-1b M51-ULS-1 40,000 K This system is composed of an O5 class supergiant star and an X-Ray source accreting black hole companion of at least 50 solar masses and potentially up to 80 with a semi-major axis of 0.5 AU. The system has 1 known Saturn sized exoplanet orbiting at 10AU with an estimated irradiation blackbody temperature of 1500K.
Hottest main-sequence star with a planet V921 Sco V921 Sco[43] 30,000 K

Host star is a 20 solar mass B0IV class subgiant

 M51-ULS-1b's supergiant primary is an O5 class supergiant with an estimated surface temperature of 40,000K, but as the star is a supergiant, does not count as on the main-sequence.
Coldest star with a planet TRAPPIST-1b, c, d, e, f, g, and h. TRAPPIST-1 2,511 K Technically Oph 162225-240515, CFBDSIR 1458+10, and WISE 1217+1626 are colder, but are classified as brown dwarfs.

System characteristics
Title System(s) Planet(s) Star(s) Notes
System with most planets Tau Ceti 6-10 1 4 are unconfirmed, but 3 of those are likely planets.
System with most planets in habitable zone TRAPPIST-1 7 1 Four planets in this system (d, e, f and g) orbit within the habitable zone.[44]
System with most stars Kepler-64 PH1b (Kepler-64b) 4 PH1b has a circumbinary orbit.
Multiplanetary system with smallest mean semi-major axis (planets are nearest to their star) Kepler-70 b, c, d? 1 Kepler-42 b, c, and d have a semimajor axis of only 0.0116, 0.006, and 0.0154 AU, respectively.
Kepler-70 b, c, and d (unconfirmed) have a semimajor axis of only 0.006, 0.0076, and ~0.0065 AU, respectively.
Multiplanetary system with largest mean semi-major axis (planets are farthest from their star) HR 8799 b, c, d, e 1 HR 8799 b, c, d, and e have a semimajor axis of 68, 38, 24, and 14.5 AU, respectively.
Multiplanetary system with smallest range of semi-major axis (smallest difference between the star's nearest planet and its farthest planet) Kepler-70 b, c, d? 1 Kepler-70 b, c, and d (unconfirmed) have a semimajor axis of only 0.006, 0.0076, and ~0.0065 AU, respectively. The separation between closest and furthest is only 0.0016 AU.
Multiplanetary system with largest range of semi-major axis (largest difference between the star's nearest planet and its farthest planet) HR 8799 b, c, d, e 1 HR 8799 b, c, d, and e have a semimajor axis of 68, 38, 24, and 14.5 AU, respectively. The separation between closest and furthest is 53.5 AU.
Multiplanetary system with smallest mean difference in semi-major axis between neighboring planets (orbits are most closely spaced to each other)
Multiplanetary system with largest mean semi-major axis between neighboring planets (orbits are most spread out with respect to each other)
System with smallest total planetary mass Kepler-444 b, c, d, e, f 1 The planets in the Kepler-444 system have radii of 0.4, 0.497, 0.53, 0.546, and 0.741 Earth radii respectively. Due to their size and proximity to Kepler-444, these must be rocky planets, with masses close to that of Mars. For comparison, Mars has a mass of 0.105 Earth masses and a radius of 0.53 Earth radii.
System with largest total planetary mass Nu Ophiuchi b, c 1 Nu Ophiuchi b and c have masses of 24 and 27 Jupiter masses, respectively. They may be brown dwarfs.
System with smallest ratio of total planetary mass to stellar mass
System with largest ratio of total planetary mass to stellar mass
Multiplanetary system with smallest mean planetary mass Kepler-444 b, c, d, e, f 1 The planets in the Kepler-444 system have radii of 0.4, 0.497, 0.53, 0.546, and 0.741 Earth radii respectively. Due to their size and proximity to Kepler-444, these must be rocky planets, with masses close to that of Mars. For comparison, Mars has a mass of 0.105 Earth masses and a radius of 0.53 Earth radii.
Multiplanetary system with smallest ratio of mean planetary mass to stellar mass
Multiplanetary system with largest mean planetary mass Kepler-52 b, c, d 1 Kepler-52 b and c have masses of 8.7 and 10.41 Jupiter masses, respectively. The mass of Kepler-52 d is 4.46 Earth masses.[45]
Multiplanetary system with largest ratio of mean planetary mass to stellar mass
Exo-multiplanetary system with smallest range in planetary mass, log scale (smallest proportional difference between the most and least massive planets) Teegarden's Star b, c 1 Teegarden b and c are estimated to have masses of 1.05 and 1.11 Earth masses, respectively.
Exo-multiplanetary system with largest range in planetary mass, log scale (largest proportional difference between the most and least massive planets) Kepler-37 b, d 1 Mercury and Jupiter have a mass ratio of 5,750 to 1. Kepler-37 d and b may have a mass ratio between 500 and 1000, and Gliese 676 c and d have a mass ratio of 491.

See also

References
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