List of nearest exoplanets

Last updated

Fomalhaut b (Dagon), 25 light-years away, with its parent star Fomalhaut blacked out, as pictured by Hubble in 2012. In 2020 this object was determined to be an expanding debris cloud from a collision of asteroids rather than a planet. NASA's Hubble Reveals Rogue Planetary Orbit For Fomalhaut B.jpg
Fomalhaut b (Dagon), 25 light-years away, with its parent star Fomalhaut blacked out, as pictured by Hubble in 2012. In 2020 this object was determined to be an expanding debris cloud from a collision of asteroids rather than a planet.
Distribution of nearest known exoplanets as of March 2018 Distances to nearest confirmed exoplanets in light years.png
Distribution of nearest known exoplanets as of March 2018

There are 5,653 known exoplanets, or planets outside the Solar System that orbit a star, as of April 1, 2024; only a small fraction of these are located in the vicinity of the Solar System. [3] Within 10 parsecs (32.6 light-years ), there are 104 exoplanets listed as confirmed by the NASA Exoplanet Archive. [note 1] [4] Among the over 500 known stars and brown dwarfs within 10 parsecs, [5] [note 2] around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye, [note 3] [7] eight of which have planetary systems.

Contents

The first report of an exoplanet within this range was in 1998 for a planet orbiting around Gliese 876 (15.3 light-years (ly) away), and the latest as of 2023 are two around Gliese 367 (30.7 ly). The closest exoplanets are those found orbiting the star closest to the Solar System, which is Proxima Centauri 4.25 light-years away. The first confirmed exoplanet discovered in the Proxima Centauri system was Proxima Centauri b, in 2016. HD 219134 (21.6 ly) has six exoplanets, the highest number discovered for any star within this range.

Most known nearby exoplanets orbit close to their stars. A majority are significantly larger than Earth, but a few have similar masses, including planets around YZ Ceti, Gliese 367, and Proxima Centauri which may be less massive than Earth. Several confirmed exoplanets are hypothesized to be potentially habitable, with Proxima Centauri b and GJ 1002 b (15.8 ly) considered among the most likely candidates. [8] The International Astronomical Union has assigned proper names to some known extrasolar bodies, including nearby exoplanets, through the NameExoWorlds project. Planets named in the 2015 event include the planets around Epsilon Eridani (10.5 ly) and Fomalhaut, [note 4] [11] while planets named in the 2022 event include those around Gliese 436, Gliese 486, and Gliese 367. [12]

Exoplanets within 10 parsecs

Key to colors
° Mercury, Earth and Jupiter (for comparison purposes)
#Confirmed multiplanetary systems
↑Exoplanets believed to be potentially habitable [8]
Confirmed exoplanets [4]
Host star system Companion exoplanet (in order from star)Notes and additional planetary observations
Name Distance
(ly)
Apparent
magnitude
(V)		 Mass
(M☉)
Label
[note 5] 		Mass
(ME) [note 6]
Radius
(R🜨)
Semi-major axis
(AU)
Orbital period
(days)
Eccentricity
Inclination
(°)
Discovery
method 		Discovery year
Sun °0.000016−26.71 Mercury 0.0550.38290.38788.0 0.205————
Earth 111365.30.0167———
Jupiter 317.810.9735.204,3330.0488———
Proxima Centauri #4.246511.130.123 d ≥0.26—0.02895.1220.04— RV 2022 [14] [15] one disputed candidate (c) [16] [17] [18] [19]
b ↑≥1.07—0.048611.190.02— RV 2016
Lalande 21185 #8.3047.520.46 b ≥2.69—0.078812.940.06— RV 20191 candidate [20]
c ≥13.6—2.942,9460.13— RV 2021
Epsilon Eridani 10.4893.730.781 Ægir 242—3.532,6890.26166.5 RV 20001 inferred planet, 1 or possibly 2 inner debris discs, and an outer disc [21] [22]
Lacaille 9352 #10.7247.340.489 b ≥4.2—0.0689.2620.03— RV 20191 candidate [23] [24]
c ≥7.6—0.12021.790.03— RV 2019
Ross 128 11.00711.10.168 b ↑≥1.40—0.04969.8660.12— RV 2017 [25]
Groombridge 34 A#11.6198.10.38 b ≥3.03—0.07211.440.09~54? RV 2014 [26] [27]
c ≥36—5.47,6000.27~54? RV 2018
Epsilon Indi A11.8674.830.762 b 941—11.0815,7000.4298.7 RV 2018 [28] [22]
Tau Ceti #11.9123.500.78 g ≥1.75—0.13320.00.06~35? RV 20174 candidates
[29] [30] [8] [31] [32] [33]
h ≥1.8—0.24349.40.23~35? RV 2017
e ≥3.9—0.5381630.18~35? RV 2017
f ≥3.9—1.336400.16~35? RV 2017
GJ 1061 #11.9847.520.113 b ≥1.37—0.0213.204<0.31— RV 2019two solutions for d's orbit [34]
c ↑≥1.74—0.0356.689<0.29— RV 2019
d ↑≥1.64—0.05413.03<0.53— RV 2019
YZ Ceti #12.12212.10.130 b ≥0.70—0.01632.0210.06— RV 2017 [35]
c ≥1.14—0.02163.0600.0— RV 2017
d ≥1.09—0.02854.6560.07— RV 2017
Luyten's Star #12.34811.940.29 c ≥1.18—0.03654.7230.10— RV 2017 [36] [23]
b ↑≥2.89—0.091118.650.17— RV 2017
d ≥10.8—0.7124140.17— RV 2019
e ≥9.3—0.8495420.03— RV 2019
Teegarden's Star #12.49715.400.08 b ↑≥1.05—0.02524.9100— RV 2019 [37]
c ↑≥1.11—0.044311.410— RV 2019
Wolf 1061 #14.05010.10.25 b ≥1.91—0.03754.8870.15— RV 2015 [36]
c ↑≥3.41—0.089017.870.11— RV 2015
d ≥7.7—0.4702170.55— RV 2015
TZ Arietis 14.57812.300.14 b ≥67—0.887710.46— RV 20192 refuted candidates [23] [38] [39]
Gliese 687 #14.8399.150.41 b ≥17.2—0.16338.140.17— RV 2014 [23] [38]
c ≥16.0—1.1657280.40— RV 2019
Gliese 674 14.8499.380.35 b ≥11.1—0.0394.6940.20— RV 2007 [40]
Gliese 876 #15.23810.20.33 d 6.68—0.02101.9380.0456.7 RV 2005 [41]
c 235—0.130930.100.2656.7 RV 2000
b 749—0.209861.100.0356.7 RV 1998
e 16—0.3355123.60.0556.7 RV 2010
GJ 1002 #15.80613.840.12 b ↑≥1.08—0.045710.35—— RV 2022 [42]
c ↑≥1.36—0.073821.2—— RV 2022
Gliese 832 16.2008.670.45 b 315—3.73,8530.0551 or 134 RV 20081 refuted candidate [43] [44]
GJ 3323 #17.53112.20.164 b ≥2.0—0.03285.360.2— RV 2017 [45]
c ≥2.3—0.12640.50.2— RV 2017
Gliese 251 18.2159.650.372 b ≥4.0—0.081814.20.10— RV 2020 [46]
Gliese 229 A#18.7918.140.58 c ↑≥7.3—0.3391220.19— RV 2020Ab not confirmed until 2020. [47]
b ≥8.5—0.8985260.10— RV 2014
Gliese 752 A19.2929.130.46 b ≥13.6—0.3381060.03— RV 2018 [48] [23]
82 G. Eridani #19.7044.260.85 b ≥2.7—0.12118.3~0— RV 20112 candidates
[49] [50] [51]
c ≥2.4—0.20440.1~0— RV 2011
d ≥4.8—0.35090~0— RV 2011
e ≥4.8—0.509147 0.29— RV 2017
EQ Pegasi A20.40010.380.436 b 718—0.6432840.3569.2 Astrometry 2022 [52]
Gliese 581 #20.54910.50.31 e ≥1.7—0.02823.150.0~45? RV 20093 refuted candidates and a disc
[53] [54] [55] [56]
b ≥16—0.04065.370.0~45? RV 2005
c ≥5.5—0.07212.90.0~45? RV 2007
Gliese 338 B20.6587.00.64 b ≥10.3—0.14124.50.11— RV 2020 [57]
Gliese 625 21.13110.20.30 b ≥2.8—0.078414.6~0.1— RV 2017 [58]
HD 219134 #21.3365.570.78 b 4.71.600.03883.09~085.05 RV 2015 [59] [60] [61]
c 4.41.510.0656.770.06287.28 RV 2015
d ≥16—0.23746.90.138~87? RV 2015
f ≥7.3—0.14622.70.148~87? RV 2015
g ≥11—0.37594.20~87? RV 2015
h (e)≥108—3.112,2470.06~87? RV 2015
LTT 1445 A#22.38710.530.26 c 1.541.150.02663.12<0.2287.43 Transit 2021 [62] [63]
b 2.871.300.03815.36<0.1189.68 Transit 2019
Gliese 393 22.9538.650.41 b ≥1.71—0.05407.030.00— RV 2019 [23] [64]
Gliese 667 C#23.62310.20.33 b ≥5.4—0.0497.200.13~52? RV 20095 dubious candidates
[65] [8] [66] [67] [23]
c ↑≥3.9—0.125128.20.03~52? RV 2011
Gliese 514 24.8789.030.53 b ≥5.2—0.4211400.45— RV 2022 [68]
Gliese 486 26.35111.3950.32 Su 2.81.310.01731.47<0.0588.4 Transit 2021 [69]
Gliese 686 26.6139.580.42 b ≥7.1—0.09715.50.04— RV 2019 [70] [23]
61 Virginis #27.8364.740.95 b ≥5.1—0.05024.22~0.1~77? RV 2009a debris disc, [71] 1 disputed candidate [72]
c ≥18—0.21838.00.14~77? RV 2009
CD Ceti 28.05214.0010.161 b ≥3.95—0.01852.290— RV 2020 [73]
Gliese 785 #28.7396.130.78 b ≥17—0.32750.13— RV 2010 [74]
c ≥24—1.18530~0.3— RV 2011
Gliese 849 #28.75010.40.49 b ≥270—2.261,9100.05— RV 2006 [75] [23]
c ≥300—4.82 5,5200.087— RV 2006
Gliese 433 #29.6059.790.48 b ≥6.0—0.0627.370.04— RV 2009 [76] [23] [47]
d ≥5.2—0.17836.10.07— RV 2020
c ≥32—4.825,0900.12— RV 2012
HD 102365 A30.3964.890.85 b ≥16—0.461220.34— RV 2010 [77]
Gliese 367 30.7199.980.45 Tahay 0.550.720.00710.32080.75 Transit 2021 [78]
Gliese 357 #30.77610.90.34 b 6.11.170.0353.930.0288.92 Transit 2019 [79] [23]
c ≥3.6—0.0619.130.04~89? RV 2019
d ↑≥7.7—0.20455.70.03~89? RV 2019
Gliese 176 30.93710.10.45 b ≥8.0—0.0668.770.08— RV 20071 disputed candidate [80] [81] [23]
GJ 3512 #30.97613.110.123 b ≥147—0.3382040.44— RV 2019 [82]
c ≥54—>1.2>1390—— RV 2019
Wolf 1069 31.22913.990.167 b ↑≥1.26—0.067215.6—— RV 2023 [83]
AU Microscopii #31.6838.630.50 b 174.380.06458.4630.1089.03 Transit 2020 [84] [85]
c <283.510.110118.86088.62 Transit 2020
Gliese 436 31.88210.670.41 Awohali 21.44.330.02802.640.1585.8 RV 2004 [86] [87]
Gliese 49 32.1588.90.57 b ≥16.4—0.10617.30.03— RV 2019 [88]
HD 260655 #32.6089.770.439 b 2.141.2400.02932.7800.03987.35 Transit 2022 [89]
c 3.091.5330.04755.7060.03887.79 Transit 2022

Excluded objects

Unlike for bodies within the Solar System, there is no clearly established method for officially recognizing an exoplanet. According to the International Astronomical Union, an exoplanet should be considered confirmed if it has not been disputed for five years after its discovery. [90] There have been examples where the existence of exoplanets has been proposed, but even after follow-up studies their existence is still considered doubtful by some astronomers. Such cases include Wolf 359 (7.9 ly, in 2019), [23] LHS 288 (15.8 ly, in 2007), [91] Gliese 682 (16.3 ly, in 2014), [47] 40 Eridani A (16.3 ly, in 2018), [92] [72] and GJ 1151 (26.2 ly, in 2021). [93] [94] [95] There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly), [96] Barnard's Star (5.96 ly), [97] [98] Kapteyn's Star (12.8 ly), [99] Van Maanen 2 (14.1 ly), [100] Groombridge 1618 (15.9 ly), [101] AD Leonis (16.2 ly), [102] VB 10 (19.3 ly), [103] and Fomalhaut (25.1 ly). [2]

In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed. [104] Another candidate planet, Candidate 1, was directly imaged around Alpha Centauri A, though it may also be a clump of asteroids or an artifact of the discovery mechanism. [105]

The Working Group on Extrasolar Planets of the International Astronomical Union adopted in 2003 a working definition on the upper limit for what constitutes a planet: not being massive enough to sustain thermonuclear fusion of deuterium. Some studies have calculated this to be somewhere around 13 times the mass of Jupiter, and therefore objects more massive than this are usually classified as brown dwarfs. [106] Some proposed candidate exoplanets have been shown to be massive enough to fall above the threshold, and thus are likely brown dwarfs, as is the case for: SCR 1845-6357 B (13.1 ly), [107] SDSS J1416+1348 B (30.3 ly), [108] and WISE 1217+1626 B (30 ly). [109]

Excluded from the current list are known examples of potential free-floating sub-brown dwarfs, or "rogue planets", which are bodies that are too small to undergo fusion yet they do not revolve around a star. Known such examples include: WISE 0855−0714 (7.4 ly), [110] UGPS 0722-05, (13.4 ly) [111] WISE 1541−2250 (18.6 ly), [112] and SIMP J01365663+0933473 (20.0 ly). [113]

See also

Notes

  1. ↑ Listed values are primarily taken from NASA Exoplanet Archive , [4] but other databases include a few additional exoplanet entries tagged as "Confirmed" that have yet to be compiled into the NASA archive. Such databases include:
    "Exoplanet Catalog". Extrasolar Planets Encyclopaedia . 1995. Full table.
    "Exoplanets Data Explorer". Exoplanet Orbit Database. California Planet Survey. Click the "+" button to visualize additional parameters.
    "Open Exoplanet Catalogue". Click the "Show options" to visualize additional parameters. Archived from the original on 2017-09-02. Retrieved 2015-02-14.
  2. ↑ For reference, the 100th closest known star system in April 2021 was EQ Pegasi (20.4 ly). [5]
  3. ↑ According to the Bortle scale, an astronomical object is visible to the naked eye under "typical" dark-sky conditions in a rural area if it has an apparent magnitude smaller than +6.5. To the unaided eye, the limiting magnitude is +7.6 to +8.0 under "excellent" dark-sky conditions (with effort). [6]
  4. ↑ The star Epsilon Eridani was named Ran (after Rán, the Norse goddess of the sea), and the planet Epsilon Eridani b was named AEgir (after Ægir, Rán's husband), [9] while the planet Fomalhaut b was named Dagon (after Dagon, an ancient Syrian “fish god” [10] ). [11]
  5. ↑ Exoplanet naming convention assigns uncapitalized letters starting from b to each planet based on chronological order of their initial report, and in increasing order of distance from the parent star for planets reported at the same time. Omitted letters signify planets that have yet to be confirmed, or planets that have been retracted altogether.
  6. ↑ Most reported exoplanet masses have very large error margins (typically, between 10% and 30%). The mass of an exoplanet has generally been inferred from measurements on changes in the radial velocity of the host star, but this kind of measurement only allows for an estimate on the exoplanet's orbital parameters, but not on their orbital inclination (i). As such, most exoplanets only have an estimated minimum mass (Mreal*sin(i)), where their true masses are statistically expected to come close to this minimum, with only about 13% chance for the mass of an exoplanet to be more than double its minimum mass. [13]

Related Research Articles

<span class="mw-page-title-main">Gliese 876</span> Star in the constellation Aquarius

Gliese 876 is a red dwarf star 15.2 light-years away from Earth in the constellation of Aquarius. It is one of the closest known stars to the Sun confirmed to possess a planetary system with more than two planets, after GJ 1061, YZ Ceti, Tau Ceti, and Wolf 1061; as of 2018, four extrasolar planets have been found to orbit the star. The planetary system is also notable for the orbital properties of its planets. It is the only known system of orbital companions to exhibit a near-triple conjunction in the rare phenomenon of Laplace resonance. It is also the first extrasolar system around a normal star with measured coplanarity. While planets b and c are located in the system's habitable zone, they are giant planets believed to be analogous to Jupiter.

<span class="mw-page-title-main">Gliese 436</span> Star in the constellation Leo

Gliese 436 is a red dwarf located 31.9 light-years away in the zodiac constellation of Leo. It has an apparent visual magnitude of 10.67, which is much too faint to be seen with the naked eye. However, it can be viewed with even a modest telescope of 2.4 in (6 cm) aperture. In 2004, the existence of an extrasolar planet, Gliese 436 b, was verified as orbiting the star. This planet was later discovered to transit its host star.

Gliese 849, or GJ 849, is a small, solitary star in the equatorial constellation of Aquarius. It has a reddish hue and is invisible to the naked eye with an apparent visual magnitude of 10.41. The distance to this star is 28.8 light-years based on parallax, but it is drifting closer to the Sun with a radial velocity of −15.3 km/s. It has a pair of confirmed gas giant companions.

Gliese 832 is a red dwarf of spectral type M2V in the southern constellation Grus. The apparent visual magnitude of 8.66 means that it is too faint to be seen with the naked eye. It is located relatively close to the Sun, at a distance of 16.2 light years and has a high proper motion of 818.16 milliarcseconds per year. Gliese 832 has just under half the mass and radius of the Sun. Its estimated rotation period is a relatively leisurely 46 days. The star is roughly 6 billion years old.

Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.

GJ 3512 is a nearby star in the northern circumpolar constellation of Ursa Major. It is invisible to the naked eye but can be observed using a telescope, having an apparent visual magnitude of +15.05. The star is located at a distance of 31 light-years from the Sun based on parallax. It has a high proper motion, traversing the celestial sphere at the rate of 1.311″ yr−1. The measurement of the star's radial velocity is poorly constrained, but it appears to be drifting further away at a rate of ~8 km/s.

<span class="mw-page-title-main">Gliese 357</span> Red dwarf with low starspot activity in the Hydra constellation

GJ 357 is an M-type main sequence star with an unusually low starspot activity. It is located 31 light-years from the Solar System. The system is part of the Hydra constellation.

GJ 3470 is a red dwarf star located in the constellation of Cancer, 96 light-years away from Earth. With a faint apparent magnitude of 12.3, it is not visible to the naked eye. It hosts one known exoplanet.

References

  1. ↑ Harrington, J. D.; Villard, Ray (2013-08-01). "NASA's Hubble Reveals Rogue Planetary Orbit For Fomalhaut". NASA. Archived from the original on 2015-11-06. Retrieved 2015-09-18.
  2. 1 2 Gáspár, András; Rieke, George H. (April 20, 2020). "New HST data and modeling reveal a massive planetesimal collision around Fomalhaut". PNAS . 117 (18): 9712–9722. arXiv: 2004.08736 . Bibcode:2020PNAS..117.9712G. doi: 10.1073/pnas.1912506117 . PMC   7211925 . PMID   32312810. S2CID   215827666.
  3. ↑ Schneider, Jean. "Interactive Extra-solar Planets Catalog". Extrasolar Planets Encyclopaedia . Archived from the original on 2012-02-12. Retrieved 2018-03-20.
  4. 1 2 3 "NASA Exoplanet Archive—Confirmed Planetary Systems". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2023-08-18.
  5. 1 2 Reylé, Céline; Jardine, Kevin; Fouqué, Pascal; Caballero, Jose A.; Smart, Richard L.; Sozzetti, Alessandro (30 April 2021). "The 10 parsec sample in the Gaia era". Astronomy & Astrophysics . 650: A201. arXiv: 2104.14972 . Bibcode:2021A&A...650A.201R. doi:10.1051/0004-6361/202140985. S2CID   233476431. Data available at https://gruze.org/10pc/
  6. ↑ Bortle, John E. (2001). "Light Pollution And Astronomy: The Bortle Dark-Sky Scale". Sky & Telescope. Archived from the original on 2009-03-23. Retrieved 2014-05-20.
  7. ↑ Powell, Richard (2006). "Stars within 50 light years". An Atlas of the Universe. Archived from the original on 2014-06-27. Retrieved 2014-05-17.
  8. 1 2 3 4 "The Habitable Exoplanets Catalog". Planetary Habitability Laboratory. University of Puerto Rico in Arecibo. 2015-09-01. Archived from the original on 2016-01-09. Retrieved 2015-09-17.
  9. ↑ "epsilon Eridani". NameExoWorlds. International Astronomical Union. Archived from the original on 2018-02-15. Retrieved 2018-05-14.
  10. ↑ "Fomalhaut (alpha Piscis Austrini)". Nameexoworlds. International Astronomical Union. Archived from the original on 2017-04-30. Retrieved 2018-05-14.
  11. 1 2 "Final Results of NameExoWorlds Public Vote Released" (Press release). International Astronomical Union. 2015-12-15. Archived from the original on 2018-05-15. Retrieved 2018-03-17.
  12. ↑ "2022 Approved Names". nameexoworlds.iau.org. IAU . Retrieved 7 June 2023.
  13. ↑ Cumming, Andrew; Butler, R. Paul; Marcy, Geoffrey W.; et al. (2008). "The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets". Publications of the Astronomical Society of the Pacific. 120 (867): 531–554. arXiv: 0803.3357 . Bibcode:2008PASP..120..531C. doi:10.1086/588487. S2CID   10979195.
  14. ↑ Anglada-Escudé, Guillem; Amado, Pedro J.; Barnes, John; et al. (2016). "A terrestrial planet candidate in a temperate orbit around Proxima Centauri". Nature. 536 (7617): 437–440. arXiv: 1609.03449 . Bibcode:2016Natur.536..437A. doi:10.1038/nature19106. PMID   27558064. S2CID   4451513.
  15. ↑ Faria, J. P.; Suárez Mascareño, A.; et al. (January 4, 2022). "A candidate short-period sub-Earth orbiting Proxima Centauri" (PDF). Astronomy & Astrophysics. 658. European Southern Observatory: 17. arXiv: 2202.05188 . Bibcode:2022A&A...658A.115F. doi: 10.1051/0004-6361/202142337 .
  16. ↑ Damasso, Mario; Del Sordo, Fabio; Anglada-Escudé, Guillem; et al. (15 January 2020). "A low-mass planet candidate orbiting Proxima Centauri at a distance of 1.5 AU". Science Advances . 6 (3). eaax7467. Bibcode:2020SciA....6.7467D. doi:10.1126/sciadv.aax7467. PMC   6962037 . PMID   31998838.
  17. ↑ Kervella, Pierre; Arenou, Frédéric; Schneider, Jean (2020). "Orbital inclination and mass of the exoplanet candidate Proxima c". Astronomy & Astrophysics. 635: L14. arXiv: 2003.13106 . Bibcode:2020A&A...635L..14K. doi:10.1051/0004-6361/202037551. ISSN   0004-6361. S2CID   214713486.
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  19. ↑ Artigau, Étienne; Cadieux, Charles; Cook, Neil J.; Doyon, René; Vandal, Thomas; Donati, Jean-Françcois; Moutou, Claire; Delfosse, Xavier; Fouqué, Pascal; Martioli, Eder; Bouchy, François; Parsons, Jasmine; Carmona, Andres; Dumusque, Xavier; Astudillo-Defru, Nicola; Bonfils, Xavier; Mignon, Lucille (2022). "Line-by-line Velocity Measurements: An Outlier-resistant Method for Precision Velocimetry". The Astronomical Journal. 164 (3): 84. arXiv: 2207.13524 . Bibcode:2022AJ....164...84A. doi: 10.3847/1538-3881/ac7ce6 . S2CID   251105120.
  20. ↑ Hurt, Spencer A.; Fulton, Benjamin; Isaacson, Howard; Rosenthal, Lee J.; Howard, Andrew W.; Weiss, Lauren M.; Petigura, Erik A. (2021), "Confirmation of the Long-Period Planet Orbiting Gliese 411 and the Detection of a New Planet Candidate", The Astronomical Journal, 163 (5): 218, arXiv: 2107.09087 , Bibcode:2022AJ....163..218H, doi: 10.3847/1538-3881/ac5c47 , S2CID   236134034
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