List of nearest exoplanets

Last updated

Epsilon Indi Ab, 12 light-years away, with its parent star Epsilon Indi A blacked out, as pictured by JWST in 2023. Epsilon Indi Ab (MIRI Image).png
Epsilon Indi Ab, 12 light-years away, with its parent star Epsilon Indi A blacked out, as pictured by JWST in 2023.
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 7,026 known exoplanets, or planets outside the Solar System that orbit a star, as of July 24, 2024; only a small fraction of these are located in the vicinity of the Solar System. [2] Within 10 parsecs (32.6 light-years ), there are 106 exoplanets listed as confirmed by the NASA Exoplanet Archive. [note 1] [3] Among the over 500 known stars and brown dwarfs within 10 parsecs, [4] [note 2] around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye, [note 3] [6] 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 2024 is one around Struve 2398 A (11.5 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, Proxima Centauri, and Barnard's Star 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. [7] 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] [10] while planets named in the 2022 event include those around Gliese 436, Gliese 486, and Gliese 367. [11]

Exoplanets within 10 parsecs

Key to colors
° Mercury, Earth and Jupiter (for comparison purposes)
#Confirmed multiplanetary systems
↑Exoplanets believed to be potentially habitable [7]
Confirmed exoplanets [3]
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 0.0550.38290.38788.00.205————
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 [13] [14] one disputed candidate (c) [15] [16] [17] [18]
b ↑≥1.07—0.048611.190.02— RV 2016
Barnard's Star 5.96299.510.162b≥0.37—0.02293.1530.16— RV 2024 [19] [20]
Lalande 21185 #8.3047.520.46 b ≥2.69—0.078812.940.06— RV 20191 candidate [21]
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 [22] [23]
Lacaille 9352 #10.7247.340.489 b ≥4.2—0.0689.2620.03— RV 20191 candidate [24] [25]
c ≥7.6—0.12021.790.03— RV 2019
Ross 128 11.00711.10.168 b ↑≥1.40—0.04969.8660.12— RV 2017 [26]
Gliese 725 A11.4918.940.330 b ≥2.78—0.06811.22010.0— RV 2024 [27]
Groombridge 34 A#11.6198.10.38 b ≥3.03—0.07211.440.09~54? RV 2014 [28] [29]
c ≥36—5.47,6000.27~54? RV 2018
Epsilon Indi A11.8674.830.762 b 2005—28.463,4000.40103.7 RV 2018nearest exoplanet directly imaged [30] [31]
Tau Ceti #11.9123.500.78 g ≥1.75—0.13320.00.06~35? RV 20174 disputed candidates
[32] [33] [7] [34] [35] [36]
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 [37]
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 [38]
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 [39] [24]
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 ↑≥1.16—0.02594.9060.03— RV 2019 [40] [41]
c ↑≥1.05—0.045511.420.04— RV 2019
d ≥0.82—0.079126.130.07— RV 2024
Wolf 1061 #14.05010.10.25 b ≥1.91—0.03754.8870.15— RV 2015 [39]
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 [24] [42] [43]
Gliese 687 #14.8399.150.41 b ≥17.2—0.16338.140.17— RV 2014 [24] [42]
c ≥16.0—1.1657280.40— RV 2019
Gliese 674 14.8499.380.35 b ≥11.1—0.0394.6940.20— RV 2007 [44]
Gliese 876 #15.23810.20.33 d 6.68—0.02101.9380.0456.7 RV 2005 [45]
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 [46]
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 [47] [48]
GJ 3323 #17.53112.20.164 b ≥2.0—0.03285.360.2— RV 2017 [39]
c ≥2.3—0.12640.50.2— RV 2017
Gliese 251 18.2159.650.372 b ≥4.0—0.081814.20.10— RV 2020 [49]
Gliese 229 A#18.7918.140.58 c ↑≥7.3—0.3391220.19— RV 2020Ab not confirmed until 2020 [50]
b ≥8.5—0.8985260.10— RV 2014
Gliese 752 A19.2929.130.46 b ≥12.2—0.3431060.10— RV 2018 [51] [52]
82 G. Eridani #19.7044.260.85 b ≥2.0—0.1318.30.09— RV 20115 disputed candidates
[53] [54] [55] [56]
d ≥4.7—0.3789.60.13— RV 2011
Gliese 555 20.39511.320.29 b ≥5.5—0.14236.10.08— RV 20231 candidate [57]
EQ Pegasi A20.40010.380.436 b 718—0.6432840.3569.2 Astrometry 2022 [58]
Gliese 581 #20.54910.50.295 e 2.5—0.02803.150.0147 RV 20093 refuted candidates and a disc [59]
b 20.5—0.03995.370.0347 RV 2005
c 6.8—0.071812.90.0347 RV 2007
Gliese 338 B20.6587.00.64 b ≥10.3—0.14124.50.11— RV 2020 [60]
Gliese 625 21.13110.20.30 b ≥2.8—0.078414.6~0.1— RV 2017 [61]
HD 219134 #21.3365.570.78 b 4.71.600.03883.09~085.05 RV 2015 [62] [63] [64]
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 20211 candidate [65] [66] [67]
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 [24] [68]
Gliese 667 C#23.62310.20.33 b ≥5.4—0.0497.200.13~52? RV 20095 dubious candidates
[69] [7] [70] [71] [24]
c ↑≥3.9—0.125128.20.03~52? RV 2011
Gliese 514 24.8789.030.53 b ≥5.2—0.4211400.45— RV 2022 [72]
GJ 1151 26.23114.010.164 c ≥10.6—0.571390—— RV 20231 refuted candidate [73] [74] [75] [76]
Gliese 486 26.35111.3950.32 Su 2.81.310.01731.47<0.0588.4 Transit 2021 [77]
Gliese 686 26.6139.580.42 b ≥7.1—0.09715.50.04— RV 2019 [78] [24]
GJ 1289 27.27512.67 [79] 0.21 b ≥6.3—0.271120— RV 2024 [80]
61 Virginis #27.8364.740.95 b ≥6.1—0.054.220.05~77? RV 2009a debris disc [56]
c ≥17.9—0.2238.10.06~77? RV 2009
d ≥10.5—0.471230.12~77? RV 2009
CD Ceti 28.05214.0010.161 b ≥3.95—0.01852.290— RV 2020 [81]
Gliese 785 #28.7396.130.78 b ≥17—0.32750.13— RV 2010 [82]
c ≥24—1.18530~0.3— RV 2011
Gliese 849 #28.75010.40.49 b ≥270—2.261,9100.05— RV 2006 [83] [24]
c ≥300—4.825,5200.087— RV 2006
Gliese 433 #29.6059.790.48 b ≥6.0—0.0627.370.04— RV 2009 [84] [24] [50]
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 [85]
Gliese 367 #30.7199.980.45 Tahay 0.630.700.00710.3220.0679.89 Transit 2021 [86] [87]
c ≥4.1—0.07711.50.09~80? RV 2023
d ≥6.0—0.15934.40.14~80? RV 2023
Gliese 357 #30.77610.90.34 b 6.11.170.0353.930.0288.92 Transit 2019 [88] [24]
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 [89] [90] [24]
GJ 3512 #30.97613.110.123 b ≥147—0.3382040.44— RV 2019 [91]
c ≥54—>1.2>1390—— RV 2019
Wolf 1069 31.22913.990.167 b ↑≥1.26—0.067215.6—— RV 2023 [92]
AU Microscopii #31.6838.630.50 b 174.380.06458.4630.1089.03 Transit 20202 candidates [93] [94] [95] [96]
c <283.510.110118.86088.62 Transit 2020
Gliese 436 31.88210.670.41 Awohali 21.44.330.02802.640.1585.8 RV 2004 [97] [98]
Gliese 49 32.1588.90.57 b ≥16.4—0.10617.30.03— RV 2019 [99]
GJ 3988 32.31613.60.184 b ≥3.7—0.04056.9440— RV 2023 [100]
HD 260655 #32.6089.770.439 b 2.141.2400.02932.7800.03987.35 Transit 2022 [101]
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. [102] 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), [24] LHS 288 (15.8 ly, in 2007), [103] and Gliese 682 (16.3 ly, in 2014). [50] There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly), [104] Barnard's Star (5.96 ly), [105] [106] Kapteyn's Star (12.8 ly), [107] Van Maanen 2 (14.1 ly), [108] Groombridge 1618 (15.9 ly), [109] AD Leonis (16.2 ly), [110] 40 Eridani A (16.3 ly), [111] [112] VB 10 (19.3 ly), [113] and Fomalhaut (25.1 ly). [114]

In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed. [115] 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. [116] Candidate planets around Luyten 726-8 (8.77 ly) [117] and GJ 3378 (25.2 ly) were reported in 2024. [80]

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. [118] 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), [119] SDSS J1416+1348 B (30.3 ly), [120] and WISE 1217+1626 B (30 ly). [121]

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), [122] UGPS 0722-05, (13.4 ly) [123] WISE 1541−2250 (18.6 ly), [124] and SIMP J01365663+0933473 (20.0 ly). [125]

See also

Notes

  1. ↑ Listed values are primarily taken from NASA Exoplanet Archive , [3] 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). [4]
  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). [5]
  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), [8] while the planet Fomalhaut b was named Dagon (after Dagon, an ancient Syrian “fish god” [9] ). [10]
  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. [12]

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.

<span class="mw-page-title-main">Groombridge 34</span> Binary star system in the constellation of Andromeda

Groombridge 34 is a binary star system in the northern constellation of Andromeda. It was listed as entry number 34 in A Catalogue of Circumpolar Stars, published posthumously in 1838 by British astronomer Stephen Groombridge. Based upon parallax measurements taken by the Gaia spacecraft, the system is located about 11.6 light-years from the Sun. This positions the pair among the nearest stars to the Solar System.

TZ Arietis is a red dwarf in the northern constellation of Aries. With a normal apparent visual magnitude of 12.3, it is too faint to be seen by the naked eye, although it lies relatively close to the Sun at a distance of 14.6 light-years. It is a flare star, which means it can suddenly increase in brightness for short periods of time.

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.

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 star spot activity. It is located 31 light-years from the Solar System, in the Hydra constellation.

<span class="mw-page-title-main">Gliese 15 Ac</span> Subjovian planet orbiting Gliese 15 A

Gliese 15 Ac is an exoplanet orbiting the nearby red dwarf star Gliese 15 A, which is part of a binary star system located about 11.6 light-years from the Sun. The planet was first proposed in October 2017 using radial velocity data from the CARMENES spectrograph, combined with measurements from the HARPS and HIRES spectrographs, and its existence was confirmed in April 2018 using HARPS-N data. It has a minimum mass 36 times that of Earth and orbits at around 5.4 astronomical units with a period of 7,600 days, an orbit which may have been sculpted by interaction with the companion star, Gliese 15 B. As of 2020, Gliese 15 Ac is the longest-period sub-Jovian planet discovered by radial velocity.

References

  1. ↑ "NASA's Webb Images Cold Exoplanet 12 Light-Years Away". nasa.gov. NASA Webb Mission Team. Retrieved Jul 24, 2024.
  2. ↑ Schneider, Jean (1995). "Interactive Extra-solar Planets Catalog". Extrasolar Planets Encyclopaedia . Archived from the original on 2012-02-12. Retrieved 2018-03-20.
  3. 1 2 3 "NASA Exoplanet Archive—Confirmed Planetary Systems". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2023-08-18.
  4. 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/
  5. ↑ 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.
  6. ↑ 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.
  7. 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.
  8. ↑ "epsilon Eridani". NameExoWorlds. International Astronomical Union. Archived from the original on 2018-02-15. Retrieved 2018-05-14.
  9. ↑ "Fomalhaut (alpha Piscis Austrini)". Nameexoworlds. International Astronomical Union. Archived from the original on 2017-04-30. Retrieved 2018-05-14.
  10. 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.
  11. ↑ "2022 Approved Names". nameexoworlds.iau.org. IAU . Retrieved 7 June 2023.
  12. ↑ 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.
  13. ↑ 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.
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  15. ↑ 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.
  16. ↑ 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.
  17. ↑ Benedict, G. Fritz; McArthur, Barbara E. (16 June 2020). "A Moving Target—Revising the Mass of Proxima Centauri c". Research Notes of the AAS . 4 (6): 86. Bibcode:2020RNAAS...4...86B. doi: 10.3847/2515-5172/ab9ca9 . S2CID   225798015.
  18. ↑ 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.
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