# HD 129116

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Binary star in the constellation Centaurus

This article is about b Centauri. For B Centauri, see [HD 102964](/source/HD_102964). For β Centauri, see [Beta Centauri](/source/Beta_Centauri). Not to be confused with [Alpha Centauri b](/source/Alpha_Centauri_b_(disambiguation)).

b Centauri Location of b Centauri (circled in red) Observation data Epoch J2000.0 Equinox J2000.0 Constellation Centaurus[1] Right ascension 14h 41m 57.59068s[2] Declination −37° 47′ 36.5940″[2] Apparent magnitude (V) +4.01[1] Characteristics Evolutionary stage Main sequence Spectral type B3V[3] B−V color index −0.157±0.002[1] Variable type Constant[4] Astrometry Radial velocity (Rv) +2.6±1.5[1] km/s Proper motion (μ) RA: −29.828±0.369[5] mas/yr Dec.: −31.914±0.518[5] mas/yr Parallax (π) 10.0339±0.3143 mas[5] Distance 330 ± 10 ly (100 ± 3 pc) Absolute magnitude (MV) −1.07[1] Details Mass 5–6[6] M☉ Radius 2.93±0.12[7] R☉ Luminosity 637.01[1] L☉ Surface gravity (log g) 4.23±0.03[7] cgs Temperature 18,310±320[6] K Rotational velocity (v sin i) 129[8] km/s Age 15±2[6] Myr Other designations b Cen, CD−37°9618, FK5 2985, GC 19779, HD 129116, HIP 71865, HR 5471, SAO 205839[9] Database references SIMBAD data

**HD 129116** is a [binary star](/source/Binary_star) in the northeastern part of [Centaurus](/source/Centaurus), east of [Menkent](/source/Menkent). It is also known by its [Bayer designation](/source/Bayer_designation) of **b Centauri**, while *HD 129116* is the star's identifier in the *[Henry Draper catalogue](/source/Henry_Draper_catalogue)*. This object has a blue-white hue and is faintly visible to the naked eye with an [apparent visual magnitude](/source/Apparent_visual_magnitude) of +4.01.[1] It is located at a distance of approximately 325 [light years](/source/Light_year) (100 [parsecs](/source/Parsec))[5] from the [Sun](/source/Sun) based on [parallax](/source/Stellar_parallax), and has an [absolute magnitude](/source/Absolute_magnitude) of −1.07.[1]

The primary star is a hot type-B star with a [spectral type](/source/Spectral_type) of B3V and a mass of 5 to 6 times the [solar mass](/source/Solar_mass). The secondary star is a close companion separated by approximately 1 [AU](/source/Astronomical_unit), with up to 4.4 times the solar mass. In 2021, a massive [exoplanet](/source/Exoplanet) was discovered by [direct imaging](/source/Direct_imaging) orbiting the pair of stars (a [circumbinary planet](/source/Circumbinary_planet)) at a distance of about 560 AU.[6]

## Star system

This is a young stellar system, belonging to the Upper Centaurus–Lupus subgroup of the [Scorpius–Centaurus association](/source/Scorpius%E2%80%93Centaurus_association), the nearest [OB association](/source/OB_association) to the Sun. This is an association of stars with common origin and movement.[10] The region inside Upper Centaurus–Lupus where b Centauri is located seems to have a uniform age of 15 million years, which is therefore the age of this system (with an uncertainty of about 2 million years).[6] From its [stellar parallax](/source/Stellar_parallax) measured by the [Gaia](/source/Gaia_(spacecraft)) spacecraft, b Centauri is located at a distance of 325 [light years](/source/Light_year) (100 [parsecs](/source/Parsec)).[5] It has been noted that the secondary star may interfere with the parallax measurements, so this distance value may not be completely accurate. In any case, b Centauri seems to be located on the closer side of the Scorpius–Centaurus association, as seen from Earth, which is also indicated by its higher [proper motion](/source/Proper_motion) compared to the mean of the association.[6]

The primary star is a [B-type main-sequence star](/source/B-type_main-sequence_star) with a [stellar classification](/source/Stellar_classification) of B3V,[3] which indicates it is engaged in [core](/source/Stellar_core) [hydrogen fusion](/source/Hydrogen_fusion) to generate energy. The object has been used as a "standard star" in several [photometric systems](/source/Photometry_(astronomy)), and it appears to be non-[variable](/source/Variable_star).[4] It has a high rate of spin, showing a [projected rotational velocity](/source/Projected_rotational_velocity) of 129 km/s.[8] The star has 5 to 6[6] times the [mass of the Sun](/source/Mass_of_the_Sun) and 2.9[7] times the [Sun's radius](/source/Sun's_radius). It is radiating 637[1] times the [luminosity of the Sun](/source/Luminosity_of_the_Sun) from its [photosphere](/source/Photosphere) at an [effective temperature](/source/Effective_temperature) of 18,445 K.[7]

In 1968 the primary was found to have variable [radial velocity](/source/Radial_velocity), which is evidence of a second star in the system, but no orbit was published.[11] The existence of the secondary star was confirmed in 2010 with an [interferometric](/source/Interferometry) observation, which revealed it at a separation of 9.22 [mas](/source/Milliarcsecond), or 1.0 [AU](/source/Astronomical_unit) at the system's distance.[12] The difference in magnitude between the stars is 1.06,[12] from which a mass of 4.4 M☉ is calculated for the secondary. However this value for the magnitude difference is uncertain, since it was based on a single observation and the detection is close to the instrument performance limit, the mass of 4.4 M☉ is considered an upper estimate.[6] Given all uncertainties, the total mass of the system is estimated at 6 to 10 M☉.[6]

## Planetary system

Artist's impression showing b Centauri and its giant planet b Centauri b.

b Centauri imaged by [VLT](/source/Very_Large_Telescope)/[SPHERE](/source/Spectro-Polarimetric_High-Contrast_Exoplanet_Research). The planet b Centauri b is indicated by an arrow. **Credit**: *ESO/Janson et al.*

The b Centauri system was included in the BEAST survey, which uses the [SPHERE](/source/SPHERE) instrument at the [Very Large Telescope](/source/Very_Large_Telescope) to search for planets around B-type stars in the Scorpius–Centaurus association. SPHERE is equipped with a sophisticated [coronagraph](/source/Coronagraph) that blocks out the light from a star and allows exoplanets around it to be [directly imaged](/source/Direct_imaging).[13] The first observation of the system in 2019 revealed an object at a 5.3 arcseconds separation that had infrared colors consistent with a massive planet. A second observation in 2021 confirmed that the object has common proper motion with b Centauri and therefore is physically bound to the system.[6] The authors of this study also looked for old observations of b Centauri and found that the planet had been imaged by the [ESO 3.6 m Telescope](/source/ESO_3.6_m_Telescope) in 2000, but was considered a background star at the time.[6][14] With a primary star mass of 5–6 M☉ and a total system mass of 6–10 M☉, b Centauri is the most massive system around which a planet has been found; previously, the most massive star with a known planet was 3 M☉. The discovery was published in December 2021 on the scientific journal *[Nature](/source/Nature_(journal))* and was led by [Stockholm University](/source/Stockholm_University) astronomer Markus Janson.[6]

Named b Centauri (AB)b (shortened as 'b Cen (AB)b'), this is a [circumbinary planet](/source/Circumbinary_planet) that orbits the stellar pair at a projected separation of 560 AU. The three epochs of observations show evidence of the orbital motion of the planet around the central stars, but the orbit is still not well constrained. The data are consistent with an [orbital period](/source/Orbital_period) between 2650 and 7170 years, inclination between 128 and 157 degrees, and [eccentricity](/source/Orbital_eccentricity) smaller than 0.4.[6]

The SPHERE images show the planet has approximately 0.01% the solar luminosity, a relic of its recent formation. From this luminosity and the age of the system, cooling models predict it has a mass of about 11 times the [mass of Jupiter](/source/Mass_of_Jupiter). The mass ratio between b Cen (AB)b and the central binary star is 0.10—0.17%, which is similar to the Sun-Jupiter system and is consistent to the expectations that more massive stars tend to have more massive planets.[6]

The formation mechanism for b Cen (AB)b is uncertain. It is believed that most giant planets are formed via [core accretion](/source/Core-accretion_theory), in which a rocky core, after growing to a critical mass, starts rapidly [accreting](/source/Accretion_(astrophysics)) the surrounding gas of the [circumstellar disc](/source/Circumstellar_disc). This mechanism cannot explain b Cen (AB)b, because core accretion becomes less efficient at large distances from the star, and massive stars like b Centauri A cause the disc to dissipate much quicker. It's more probable that the planet formed directly from the circumstellar gas, through a mechanism known as gravitational instability. This process is much faster than core accretion and can act even at separations of hundreds of astronomical units. Another possibility is that the planet formed closer to the central stars and was subsequently ejected to its current orbit through interactions with another body, but this is disfavored by the lack of evidence of other planets in the system and by the low eccentricity of b Cen (AB)b.[6]

The discovery of b Cen (AB)b showed that planets can exist even around massive stars. Previous studies had shown that planet occurrence rate starts to drop for stars over 2 M☉ and reaches almost zero for 3 M☉ stars, but this result is valid only for close in planets, which the [radial velocity method](/source/Radial_velocity_method) can detect. The discovers of b Cen (AB)b argued that the short lifetime of the circumstellar discs around massive stars may prevent planets from [migrating](/source/Planetary_migration) closer to their stars, but allows the existence of distant planets like b Cen (AB)b.[6]

The b Centauri planetary system[6] Companion (in order from star) Mass Semimajor axis (AU) Orbital period (years) Eccentricity Inclination (°) Radius (AB)b 10.9±1.6 MJ 556±17 7170±2650 0.4 157°±128° 1.11 RJ

## References

1. ^ [***a***](#cite_ref-Anderson2012_1-0) [***b***](#cite_ref-Anderson2012_1-1) [***c***](#cite_ref-Anderson2012_1-2) [***d***](#cite_ref-Anderson2012_1-3) [***e***](#cite_ref-Anderson2012_1-4) [***f***](#cite_ref-Anderson2012_1-5) [***g***](#cite_ref-Anderson2012_1-6) [***h***](#cite_ref-Anderson2012_1-7) [***i***](#cite_ref-Anderson2012_1-8) Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". *[Astronomy Letters](/source/Astronomy_Letters)*. **38** (5): 331. [arXiv](/source/ArXiv_(identifier)):[1108.4971](https://arxiv.org/abs/1108.4971). [Bibcode](/source/Bibcode_(identifier)):[2012AstL...38..331A](https://ui.adsabs.harvard.edu/abs/2012AstL...38..331A). [doi](/source/Doi_(identifier)):[10.1134/S1063773712050015](https://doi.org/10.1134%2FS1063773712050015). [XHIP record for this object](https://vizier.cds.unistra.fr/viz-bin/VizieR-4?-ref=VIZ681510a8389ecb&-out.src=V%2F137D%2FXHIP&-nav=cat%3AV%2F137D%26tab%3A{V%2F137D%2FXHIP}%26key%3Asource%3DV%2F137D%2FXHIP%26HTTPPRM%3A&-source=V%2F137D%2FXHIP&-out=HIP&HIP=71865&-out=Comp&-out=Gr&-out=RAJ2000&-out=DEJ2000&-out=Dist&-out=X&-out=Y&-out=Z&-out=SpType&-out=Simbad&-out=Hpmag&-out=Lum&-out=Cst) at [VizieR](/source/VizieR).

1. ^ [***a***](#cite_ref-vanLeeuwen2007_2-0) [***b***](#cite_ref-vanLeeuwen2007_2-1) van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". *Astronomy and Astrophysics*. **474** (2): 653–664. [arXiv](/source/ArXiv_(identifier)):[0708.1752](https://arxiv.org/abs/0708.1752). [Bibcode](/source/Bibcode_(identifier)):[2007A&A...474..653V](https://ui.adsabs.harvard.edu/abs/2007A&A...474..653V). [doi](/source/Doi_(identifier)):[10.1051/0004-6361:20078357](https://doi.org/10.1051%2F0004-6361%3A20078357). [S2CID](/source/S2CID_(identifier)) [18759600](https://api.semanticscholar.org/CorpusID:18759600).

1. ^ [***a***](#cite_ref-Hiltner1969_3-0) [***b***](#cite_ref-Hiltner1969_3-1) Hiltner, W. A.; et al. (July 1969). ["MK Spectral Types for Bright Southern OB Stars"](https://doi.org/10.1086%2F150069). *Astrophysical Journal*. **157**: 313–326. [Bibcode](/source/Bibcode_(identifier)):[1969ApJ...157..313H](https://ui.adsabs.harvard.edu/abs/1969ApJ...157..313H). [doi](/source/Doi_(identifier)):[10.1086/150069](https://doi.org/10.1086%2F150069).

1. ^ [***a***](#cite_ref-Paunzen2017_4-0) [***b***](#cite_ref-Paunzen2017_4-1) Paunzen, E.; Rode-Paunzen, M. (2017). "BRITE photometry of seven B-type stars". *Second Brite-Constellation Science Conference: Small Satellites – Big Science*. **5**: 180. [arXiv](/source/ArXiv_(identifier)):[1612.04714](https://arxiv.org/abs/1612.04714). [Bibcode](/source/Bibcode_(identifier)):[2017sbcs.conf..180P](https://ui.adsabs.harvard.edu/abs/2017sbcs.conf..180P).

1. ^ [***a***](#cite_ref-EDR3_5-0) [***b***](#cite_ref-EDR3_5-1) [***c***](#cite_ref-EDR3_5-2) [***d***](#cite_ref-EDR3_5-3) [***e***](#cite_ref-EDR3_5-4) [Brown, A. G. A.](/source/Anthony_Brown_(scientist)); et al. (Gaia collaboration) (2021). ["*Gaia* Early Data Release 3: Summary of the contents and survey properties"](https://doi.org/10.1051%2F0004-6361%2F202039657). *[Astronomy & Astrophysics](/source/Astronomy_%26_Astrophysics)*. **649**: A1. [arXiv](/source/ArXiv_(identifier)):[2012.01533](https://arxiv.org/abs/2012.01533). [Bibcode](/source/Bibcode_(identifier)):[2021A&A...649A...1G](https://ui.adsabs.harvard.edu/abs/2021A&A...649A...1G). [doi](/source/Doi_(identifier)):[10.1051/0004-6361/202039657](https://doi.org/10.1051%2F0004-6361%2F202039657). [S2CID](/source/S2CID_(identifier)) [227254300](https://api.semanticscholar.org/CorpusID:227254300). (Erratum: [doi](/source/Doi_(identifier)):[10.1051/0004-6361/202039657e](https://doi.org/10.1051%2F0004-6361%2F202039657e)). [Gaia EDR3 record for this source](https://vizier.u-strasbg.fr/viz-bin/VizieR-S?Gaia%20EDR3%206105713692544123520) at [VizieR](/source/VizieR).

1. ^ [***a***](#cite_ref-Janson2021_6-0) [***b***](#cite_ref-Janson2021_6-1) [***c***](#cite_ref-Janson2021_6-2) [***d***](#cite_ref-Janson2021_6-3) [***e***](#cite_ref-Janson2021_6-4) [***f***](#cite_ref-Janson2021_6-5) [***g***](#cite_ref-Janson2021_6-6) [***h***](#cite_ref-Janson2021_6-7) [***i***](#cite_ref-Janson2021_6-8) [***j***](#cite_ref-Janson2021_6-9) [***k***](#cite_ref-Janson2021_6-10) [***l***](#cite_ref-Janson2021_6-11) [***m***](#cite_ref-Janson2021_6-12) [***n***](#cite_ref-Janson2021_6-13) [***o***](#cite_ref-Janson2021_6-14) [***p***](#cite_ref-Janson2021_6-15) [***q***](#cite_ref-Janson2021_6-16) Janson, Markus; Gratton, Raffaele; Rodet, Laetitia; Vigan, Arthur; Bonnefoy, Mickaël; Delorme, Philippe; Mamajek, Eric E.; Reffert, Sabine; Stock, Lukas; Marleau, Gabriel-Dominique; Langlois, Maud; Chauvin, Gaël; Desidera, Silvano; Ringqvist, Simon; Mayer, Lucio; Viswanath, Gayathri; Squicciarini, Vito; Meyer, Michael R.; Samland, Matthias; Petrus, Simon; Helled, Ravit; Kenworthy, Matthew A.; Quanz, Sascha P.; Biller, Beth; Henning, Thomas; Mesa, Dino; Engler, Natalia; Carson, Joseph C. (2021). "A wide-orbit giant planet in the high-mass b Centauri binary system". *Nature*. **600** (7888): 231–234. [arXiv](/source/ArXiv_(identifier)):[2112.04833](https://arxiv.org/abs/2112.04833). [Bibcode](/source/Bibcode_(identifier)):[2021Natur.600..231J](https://ui.adsabs.harvard.edu/abs/2021Natur.600..231J). [doi](/source/Doi_(identifier)):[10.1038/s41586-021-04124-8](https://doi.org/10.1038%2Fs41586-021-04124-8). [PMID](/source/PMID_(identifier)) [34880428](https://pubmed.ncbi.nlm.nih.gov/34880428). [S2CID](/source/S2CID_(identifier)) [245005994](https://api.semanticscholar.org/CorpusID:245005994).

1. ^ [***a***](#cite_ref-Fitzpatrick2005_7-0) [***b***](#cite_ref-Fitzpatrick2005_7-1) [***c***](#cite_ref-Fitzpatrick2005_7-2) [***d***](#cite_ref-Fitzpatrick2005_7-3) Fitzpatrick, E. L.; Massa, D. (March 2005). "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry". *The Astronomical Journal*. **129** (3): 1642–1662. [arXiv](/source/ArXiv_(identifier)):[astro-ph/0412542](https://arxiv.org/abs/astro-ph/0412542). [Bibcode](/source/Bibcode_(identifier)):[2005AJ....129.1642F](https://ui.adsabs.harvard.edu/abs/2005AJ....129.1642F). [doi](/source/Doi_(identifier)):[10.1086/427855](https://doi.org/10.1086%2F427855). [S2CID](/source/S2CID_(identifier)) [119512018](https://api.semanticscholar.org/CorpusID:119512018).

1. ^ [***a***](#cite_ref-Wolff2007_8-0) [***b***](#cite_ref-Wolff2007_8-1) Wolff, S. C.; Strom, S. E.; Dror, D.; Venn, K. (2007). "Rotational Velocities for B0-B3 Stars in Seven Young Clusters: Further Study of the Relationship between Rotation Speed and Density in Star-Forming Regions". *[The Astronomical Journal](/source/The_Astronomical_Journal)*. **133** (3): 1092–1103. [arXiv](/source/ArXiv_(identifier)):[astro-ph/0702133](https://arxiv.org/abs/astro-ph/0702133). [Bibcode](/source/Bibcode_(identifier)):[2007AJ....133.1092W](https://ui.adsabs.harvard.edu/abs/2007AJ....133.1092W). [doi](/source/Doi_(identifier)):[10.1086/511002](https://doi.org/10.1086%2F511002). [S2CID](/source/S2CID_(identifier)) [119074863](https://api.semanticscholar.org/CorpusID:119074863).

1. **[^](#cite_ref-SIMBAD_9-0)** ["b Cen"](http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=b+Cen). *[SIMBAD](/source/SIMBAD)*. [Centre de données astronomiques de Strasbourg](/source/Centre_de_donn%C3%A9es_astronomiques_de_Strasbourg). Retrieved 2020-03-05.

1. **[^](#cite_ref-deZeeuw1999_10-0)** De Zeeuw, P. T.; Hoogerwerf, R.; De Bruijne, J. H. J.; Brown, A. G. A.; Blaauw, A. (1999). "A HIPPARCOS Census of the Nearby OB Associations". *The Astronomical Journal*. **117** (1): 354–399. [arXiv](/source/ArXiv_(identifier)):[astro-ph/9809227](https://arxiv.org/abs/astro-ph/9809227). [Bibcode](/source/Bibcode_(identifier)):[1999AJ....117..354D](https://ui.adsabs.harvard.edu/abs/1999AJ....117..354D). [doi](/source/Doi_(identifier)):[10.1086/300682](https://doi.org/10.1086%2F300682). [S2CID](/source/S2CID_(identifier)) [16098861](https://api.semanticscholar.org/CorpusID:16098861).

1. **[^](#cite_ref-Gutierrez-Moreno1968_11-0)** Gutierrez-Moreno, Adelina; Moreno, Hugo (1968). ["A Photometric Investigation of the SCORPIUS-CENTAURUS Association"](https://doi.org/10.1086%2F190168). *The Astrophysical Journal Supplement Series*. **15**: 459. [Bibcode](/source/Bibcode_(identifier)):[1968ApJS...15..459G](https://ui.adsabs.harvard.edu/abs/1968ApJS...15..459G). [doi](/source/Doi_(identifier)):[10.1086/190168](https://doi.org/10.1086%2F190168).

1. ^ [***a***](#cite_ref-Rizzuto2013_12-0) [***b***](#cite_ref-Rizzuto2013_12-1) Rizzuto, A. C.; Ireland, M. J.; Robertson, J. G.; Kok, Y.; Tuthill, P. G.; Warrington, B. A.; Haubois, X.; Tango, W. J.; Norris, B.; Ten Brummelaar, T.; Kraus, A. L.; Jacob, A.; Laliberte-Houdeville, C. (2013). ["Long-baseline interferometric multiplicity survey of the Sco-Cen OB association"](https://doi.org/10.1093%2Fmnras%2Fstt1690). *Monthly Notices of the Royal Astronomical Society*. **436** (2): 1694. [arXiv](/source/ArXiv_(identifier)):[1309.3811](https://arxiv.org/abs/1309.3811). [Bibcode](/source/Bibcode_(identifier)):[2013MNRAS.436.1694R](https://ui.adsabs.harvard.edu/abs/2013MNRAS.436.1694R). [doi](/source/Doi_(identifier)):[10.1093/mnras/stt1690](https://doi.org/10.1093%2Fmnras%2Fstt1690).

1. **[^](#cite_ref-Janson2021beast_13-0)** Janson, Markus; Squicciarini, Vito; Delorme, Philippe; Gratton, Raffaele; Bonnefoy, Mickaël; Reffert, Sabine; Mamajek, Eric E.; Eriksson, Simon C.; Vigan, Arthur; Langlois, Maud; Engler, Natalia; Chauvin, Gaël; Desidera, Silvano; Mayer, Lucio; Marleau, Gabriel-Dominique; Bohn, Alexander J.; Samland, Matthias; Meyer, Michael; d'Orazi, Valentina; Henning, Thomas; Quanz, Sascha; Kenworthy, Matthew; Carson, Joseph C. (2021). "BEAST begins: Sample characteristics and survey performance of the B-star Exoplanet Abundance Study". *Astronomy and Astrophysics*. **646**: A164. [arXiv](/source/ArXiv_(identifier)):[2101.02043](https://arxiv.org/abs/2101.02043). [Bibcode](/source/Bibcode_(identifier)):[2021A&A...646A.164J](https://ui.adsabs.harvard.edu/abs/2021A&A...646A.164J). [doi](/source/Doi_(identifier)):[10.1051/0004-6361/202039683](https://doi.org/10.1051%2F0004-6361%2F202039683). [S2CID](/source/S2CID_(identifier)) [230770142](https://api.semanticscholar.org/CorpusID:230770142).

1. **[^](#cite_ref-Shatsky2002_14-0)** Shatsky, N.; Tokovinin, A. (2002). "The mass ratio distribution of B-type visual binaries in the Sco OB2 association". *Astronomy and Astrophysics*. **382**: 92. [arXiv](/source/ArXiv_(identifier)):[astro-ph/0109456](https://arxiv.org/abs/astro-ph/0109456). [Bibcode](/source/Bibcode_(identifier)):[2002A&A...382...92S](https://ui.adsabs.harvard.edu/abs/2002A&A...382...92S). [doi](/source/Doi_(identifier)):[10.1051/0004-6361:20011542](https://doi.org/10.1051%2F0004-6361%3A20011542). [S2CID](/source/S2CID_(identifier)) [16697655](https://api.semanticscholar.org/CorpusID:16697655).

## External links

- ["ESO telescope images planet around most massive star pair to date"](https://www.eso.org/public/news/eso2118/). [European Southern Observatory](/source/European_Southern_Observatory). 8 December 2021. Retrieved 8 December 2021.

v t e Constellation of Centaurus List of stars in Centaurus Centaurus in Chinese astronomy Stars Bayer α A (Rigil Kentaurus) B (Toliman) C (Proxima Centauri) β (Hadar) γ δ ε ζ (Leepwal) η θ (Menkent) ι (Kulou) κ λ μ ν (Heng) ξ1 ξ2 ο1 ο2 π ρ σ τ υ1 υ2 φ χ ψ x1 x2 C3 D E F G H J K M N Q Flamsteed 1 (i) 2 (g) 3 (k) 4 (h) Variable R T V Y RR SV SX BV DY UY V346 V553 V744 V752 V761 (a) V763 (C1) V766 V779 (Krzemiński's star) V803 V810 V816 (Przybylski's Star) V831 V842 V885 V886 V863 V1032 V1369 V1400 V1935 HR 4460 (A) 4466 (C2) 4499 4522 4523 4537 (j) 4546 (B) 4721 4748 (u) 4796 4817 (l) 4831 (w) 4874 (p) 4888 (e) 4889 (n) 4940 (f) 4979 4989 5006 (r) 5041 (m) 5089 (d) 5174 (z) 5222 (y) 5224 5241 5297 5358 (v) 5371 5471 (b) 5485 (c1) 5489 (c2) HD 97413 98176 100453 101581 101930 102117 (Uklun) 103197 107914 108236 109749 110113 113538 113766 114386 114729 115600 116434 (Matza) 117207 117618 (Dofida) 117939 120411 121228 121504 124448 (Popper's Star) 125072 125595 131399 Other 2MASS J1126−5003 2M1207 Gaia BH2 HD 131399 Ab PSR B1259−63 PSR J1311−3430 TOI-763 WASP-15 (Nyamien) WASP-41 WASP-42 WASP-167/KELT-13 Exoplanets 2M1207b b Centauri b HD 101930 b HD 102117 b (Leklsullun) HD 103197 b HD 109749 b HD 113538 b c HD 114386 b HD 114729 b HD 117207 b HD 117618 b (Noifasui) HD 121504 b HIP 65426 b (Najsakopajk) HIP 67522 b NGTS-13b Proxima Centauri b c d WASP-15b (Asye) Star clusters NGC 3766 4230 4507 5281 5286 5316 5460 5617 5662 Other IC 2944 ω Centauri Scorpius–Centaurus association Stock 16 Nebulae NGC 3918 5307 Other Boomerang Nebula Fleming 1 G292.0+1.8 G306.3-0.9 Gum 41 IC 2944 IRAS 13208−6020 RCW 79 RCW 86 Southern Crab Nebula SuWt 2 Galaxies NGC 3557 3568 3749 3783 4444 4603 4622 4650A 4683 4696 4706 4709 4729 4730 4743 4744 4909 4930 4945 4976 5011 A 5026 5064 5082 5090 5091 5102 5114 5121 5128 (Centaurus A) 5161 5206 5253 5266 5291 5398 5408 5419 5483 5516 Other ESO 269-57 ESO 325-4 ESO 383-76 ESO 444-46 Fourcade-Figueroa Object IC 3370 IC 4214 IC 4329A IRAS 13224−3809 J1144−4308 LEDA 677373 PKS 1144−379 PKS 1353−341 PKS 1424−418 Galaxy clusters Abell S740 Centaurus Cluster Shapley Supercluster Astronomical events GW190521 SN 185 SN 1895B (Z) SN 1972E SN 1986G J1407b SN 2019so Category

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Adapted from the Wikipedia article [HD 129116](https://en.wikipedia.org/wiki/HD_129116) by Wikipedia contributors ([contributor history](https://en.wikipedia.org/wiki/HD_129116?action=history)). Available under [Creative Commons Attribution-ShareAlike 4.0 International](https://creativecommons.org/licenses/by-sa/4.0/). Changes may have been made.