List of supernova candidates

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Map showing various supernova candidates, most of which are within one kiloparsec from the Solar System. Supernova candidates.jpg
Map showing various supernova candidates, most of which are within one kiloparsec from the Solar System.

This is a list of supernova candidates, or stars that are believed to soon become supernovae. Type II supernova progenitors include stars with at least 8~10 solar masses that are in the final stages of their evolution. Prominent examples of stars in this mass range include Antares, Spica, Gamma Velorum, [2] Mu Cephei, and members of the Quintuplet Cluster. [3] Type Ia supernova progenitors are white dwarf stars that are close to the Chandrasekhar limit of about 1.44 solar masses and are accreting matter from a binary companion star.

The list includes massive Wolf–Rayet stars, which may become Type Ib/Ic supernovae, particularly oxygen-sequence (Wolf-Rayet WO) stars. As of 2023, most of these candidates are in the Milky Way galaxy, however five oxygen-sequence Wolf-Rayet stars are also known in other galaxies.

This is a dynamic list and may never be able to satisfy particular standards for completeness. You can help by adding missing items with reliable sources.
Identifier Epoch J2000 Constellation Distance

(light years)

 Spectral

class

Evolutionary stage Possible supernova

type

Notes
R. A. Dec.
IK Pegasi 21h 26m 26.7s+19° 22′ 32″ Pegasus 154.4±1.0 [4] A8m:/DA White dwarf Ia
Spica 13h 25m 11.6s−11° 09′ 40.8″ Virgo 250+14
−13 [5] 		B1 Subgiant [6]
Acrux 12h 26m 35.9s–63° 05′ 56″ Crux 320±20 [5] B0.5 IV Main sequence (blue dwarf)II [7]
Alpha-2 Crucis 12h 26m 36.4s–63° 05′ 58″ Crux 320±20 [5] B1 V Main sequence (blue dwarf)II [7]
Zeta Ophiuchi 16h 37m 09.5s−10° 34′ 02″ Ophiuchus 365±6.52 [1] O9.5V Main sequence (blue dwarf) [6]
Betelgeuse 05h 55m 10.3s+07° 24′ 25″ Orion ~400–500 [8] M2Iab Red supergiant IIP [9]
Alpha Lupi 14h 41m 55.8s–47° 23′ 17″ Lupus 465+12
−11 [5] 		B1.5 Blue giant II [6]
Antares 16h 29m 24.5s–26° 25′ 55″ Scorpius 554+113
−80 [5] 		M1.5Iab-b Red supergiant IIP [6]
Pi Puppis 07h 17m 08.6s–37° 05′ 51″ Puppis 807+72
−61 [5] 		K3 Ib Red supergiant II? [1] [10]
S Monocerotis A06h 40m 58.7s+09° 53′ 44″ Monoceros 920+150
−110 [5] 		O7V Main sequence (blue dwarf)II [1]
S Monocerotis B06h 40m 58.7s+09° 53′ 44″ Monoceros 920+150
−110 [5] 		O9.5V Main sequence (blue dwarf)II [1]
Rigel 05h 14m 32.3s–08° 12′ 06″ Orion 1118+30
−28 [4] 		B8Ia Blue supergiant IIn(pec?) [11]
Gamma2 Velorum 08h 09m 32.0s−47° 20′ 12″ Vela 1120+130
−100 [5] 		WC8 Wolf–Rayet star Ib/Ic [12] [2]
Alnitak 05h 40m 45.5s−01° 56′ 34.3″ Orion 1260±180O9.5Iab Blue supergiant [13]
119 Tauri 05h 32m 12.8s+18° 35′ 40″ Taurus 1790+300
−220 [5] 		M2Iab-Ib Red supergiant IIb [1] [10]
Deneb 20h 41m 25.9s+45° 16′ 49″ Cygnus 2615±215 [1] A2la Blue supergiant IIL [1]
T Coronae Borealis 15h 59m 30.2s+25° 55′ 13″ Corona Borealis 2690+110
−100 [4] 		M3III/D White dwarf Ia [14]
KPD 1930+2752 19h 32m 14.9s+27° 58′ 35″ Cygnus 2860+130
−120 [4] 		sdB/D White dwarf Ia [nb 1] [15] [16]
Mu Cephei 21h 43m 30.5s+58° 46′ 48″ Cepheus 3060+456
−130 [17] 		M2Ia Red hypergiant IIn/IIb [18]
Rho Cassiopeiae 23h 54m 23.0s+57° 29′ 58″ Cassiopeia 3440+930
−610 [4] 		G2Ia0e Yellow hypergiant IIL [19]
VY Canis Majoris 07h 22m 58.3s−25° 46′ 03″ Canis Major 3930+420
−350 [20] 		M5eIa Red hypergiant II [9] [21]
IRAS 17163-3907 17h 19m 49.3s−39° 10′ 37.9″ Scorpius 3930+990
−660 [4] 		late B/early A Yellow hypergiant II [22]
Wray 17-96 17h 41m 35.4s–30° 06′ 39″ Scorpius 3940+1110
−710 [4] 		B3 Luminous blue variable
VV Cephei A21h 56m 39.1s+63° 37′ 32″ Cepheus 4900 [23] M2Iab Red hypergiant [1]
P Cygni 20h 17m 47.2s+38° 01′ 59″Cygnus5250±590 [24] B1Ia+ Luminous blue variable IIb [25]
HD 168625 18h 21m 19.5s−16° 22′ 26″ Sagittarius 5250+600
−490 [4] 		B6Ia Luminous blue variable II [26]
NML Cygni 20h 46m 25.6s+40° 06′ 59.4″ Cygnus 5250+420
−360 [27] 		M6I Red hypergiant II [28]
IRC +10420 19h 26m 48.1s+11° 21′ 17″Aquila5600+2200
−1200 [4] 		F8Ia+ Yellow hypergiant IIb [29] [30]
WR 142 20h 21m 44.3s+37° 22′ 31″ Cygnus 5670+290
−270 [4] 		WO2 Wolf–Rayet star Ib/Ic
WR 136 20h 12m 06.5s+38° 21′ 18″ Cygnus 6700+500
−430 [4] 		WN6(h)-s Wolf–Rayet star Ic
RS Ophiuchi 17h 50m 13.2s–06° 42′ 28″ Ophiuchus 7380+1000
−790 [4] 		M2III/D White dwarf Ia
Eta Carinae 10h 45m 03.6s−59° 41′ 04″Carina8630+69
−68 [4] 		LBV/O Luminous blue variable Ib [31] [32]
WR 93b 17h 32m 03.3s−35° 04′ 32″ Scorpius 8700+1900
−1300 [4] 		WO3 Wolf–Rayet star Ib/Ic
WR 102 17h 45m 47.5s−26° 10′ 27″ Sagittarius 9410+840
−710 [4] 		WO2 Wolf–Rayet star Ib/Ic
HD 179821 19h 13m 58.6s+00° 07′ 32″Aquila10500+2100
−1500 [4] 		G5Ia Yellow hypergiant IIL [33] [34]
T Pyxidis 09h 04m 41.5s−32° 22′ 48″ Pyxis 10700+1700
−1300 [4] 		White dwarf Ia [35] [36]
WR 104 18h 02m 04.1s–23° 37′ 41″Sagittarius13400+9200
−3900 [4] 		WC9d/OB Wolf–Rayet star Ib/Ic with Grb? [37] [38]
V445 Puppis 07h 37m 56.9s–25° 56′ 59″ Puppis 16000+5200
−4600 [39] 		White dwarf Ia [40]
WR 30a 10h 51m 38.9s−60° 56′ 35.2″ Carina 38900+18500
−9500 [4] 		WO4/O5((f)) Wolf–Rayet star
Sher 25 11h 15m 07.8s−61° 15′ 17″ Carina 43500+5200
−4200 [4] 		B1.5Iab Blue supergiant [41]
U Scorpii 16h 22m 30.7s–17° 52′ 42″ Scorpius 63900+68500
−17300 [42] 		White dwarf Ia [43]
LMC195-1 05h 18m 10.3s−69° 13′ 03″ Dorado 160000 [4] WO2 Wolf–Rayet star Ib/Ic
S Doradus 05h 18m 14.4s−69° 15′ 01″ Dorado 169000LBV Luminous blue variable [44]
SMC AB8 01h 31m 04.1s−73° 25′ 04″ Hydrus 200000 [4] WO4/O4 Wolf–Rayet star Ib/Ic

Notes

  1. ↑ The Kitt Peak Downes star.

Related Research Articles

<span class="mw-page-title-main">Supernova</span> Explosion of a star at its end of life

A supernova is a powerful and luminous explosion of a star. A supernova occurs during the last evolutionary stages of a massive star, or when a white dwarf is triggered into runaway nuclear fusion. The original object, called the progenitor, either collapses to a neutron star or black hole, or is completely destroyed to form a diffuse nebula. The peak optical luminosity of a supernova can be comparable to that of an entire galaxy before fading over several weeks or months.

<span class="mw-page-title-main">Red supergiant</span> Stars with a supergiant luminosity class with a spectral type of K or M

Red supergiants (RSGs) are stars with a supergiant luminosity class and a stellar classification K or M. They are the largest stars in the universe in terms of volume, although they are not the most massive or luminous. Betelgeuse and Antares A are the brightest and best known red supergiants (RSGs), indeed the only first magnitude red supergiant stars.

<span class="mw-page-title-main">Blue supergiant</span> Hot, luminous star with a spectral type of A9 or earlier

A blue supergiant (BSG) is a hot, luminous star, often referred to as an OB supergiant. They are usually considered to be those with luminosity class I and spectral class B9 or earlier, although sometimes A-class supergiants are also deemed blue supergiants.

Solar radius is a unit of distance used to express the size of stars in astronomy relative to the Sun. The solar radius is usually defined as the radius to the layer in the Sun's photosphere where the optical depth equals 2/3:

<span class="mw-page-title-main">Luminous blue variable</span> Type of star that is luminous, blue, and variable in brightness

Luminous blue variables (LBVs) are rare, massive and evolved stars that show unpredictable and sometimes dramatic variations in their spectra and brightness. They are also known as S Doradus variables after S Doradus, one of the brightest stars of the Large Magellanic Cloud.

<span class="mw-page-title-main">Yellow hypergiant</span> Class of massive star with a spectral type of A to K

A yellow hypergiant (YHG) is a massive star with an extended atmosphere, a spectral class from A to K, and, starting with an initial mass of about 20–60 solar masses, has lost as much as half that mass. They are amongst the most visually luminous stars, with absolute magnitude (MV) around −9, but also one of the rarest, with just 20 known in the Milky Way and six of those in just a single cluster. They are sometimes referred to as cool hypergiants in comparison with O- and B-type stars, and sometimes as warm hypergiants in comparison with red supergiants.

<span class="mw-page-title-main">Westerlund 1</span> Super star cluster in the Milky Way Galaxy

Westerlund 1 is a compact young super star cluster about 3.8 kpc away from Earth. It is thought to be the most massive young star cluster in the Milky Way, and was discovered by Bengt Westerlund in 1961 but remained largely unstudied for many years due to high interstellar absorption in its direction. In the future, it will probably evolve into a globular cluster.

<span class="mw-page-title-main">Hypergiant</span> Rare star with tremendous luminosity and high rates of mass loss by stellar winds

A hypergiant (luminosity class 0 or Ia+) is a very rare type of star that has an extremely high luminosity, mass, size and mass loss because of its extreme stellar winds. The term hypergiant is defined as luminosity class 0 (zero) in the MKK system. However, this is rarely seen in literature or in published spectral classifications, except for specific well-defined groups such as the yellow hypergiants, RSG (red supergiants), or blue B(e) supergiants with emission spectra. More commonly, hypergiants are classed as Ia-0 or Ia+, but red supergiants are rarely assigned these spectral classifications. Astronomers are interested in these stars because they relate to understanding stellar evolution, especially star formation, stability, and their expected demise as supernovae. Notable examples of hypergiants include the Pistol Star, a blue hypergiant located close to the Galactic Center and one of the most luminous stars known; Rho Cassiopeiae, a yellow hypergiant that is one of the brightest to the naked eye; and Mu Cephei (Herschel's "Garnet Star"), one of the largest and brightest stars known.

<span class="mw-page-title-main">Cygnus OB2</span> Cluster of massive and luminous stars

Cygnus OB2 is an OB association that is home to some of the most massive and most luminous stars known, including suspected Luminous blue variable Cyg OB2 #12. It also includes one of the largest known stars, NML Cygni. The region is embedded within a wider one of star formation known as Cygnus X, which is one of the most luminous objects in the sky at radio wavelengths. The region is approximately 1,570 parsecs from Earth in the constellation of Cygnus.

<span class="mw-page-title-main">PZ Cassiopeiae</span> Star in the constellation Cassiopeia

PZ Cassiopeiae is a red supergiant star located in the constellation of Cassiopeia, and a semi-regular variable star.

In astronomy, a calcium-rich supernova is a subclass of supernovae that, in contrast to more well-known traditional supernova classes, are fainter and produce unusually large amounts of calcium. Since their luminosity is located in a gap between that of novae and other supernovae, they are also referred to as "gap" transients. Only around 15 events have been classified as a calcium-rich supernova – a combination of their intrinsic rarity and low luminosity make new discoveries and their subsequent study difficult. This makes calcium-rich supernovae one of the most mysterious supernova subclasses currently known.

<span class="mw-page-title-main">NGC 753</span> Galaxy in the constellation Andromeda

NGC 753 is a spiral galaxy located 220 million light-years away in the constellation Andromeda. The galaxy was discovered by astronomer by Heinrich d'Arrest on September 16, 1865 and is a member of Abell 262.

<span class="mw-page-title-main">NGC 4061</span> Galaxy in the constellation Coma Berenices

NGC 4061 is an elliptical galaxy located 310 light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 27, 1785. It was rediscovered by John Herschel on April 29, 1832. It is listed both as NGC 4061 and NGC 4055. NGC 4061 is a member of the NGC 4065 Group and forms an interacting pair with its companion, NGC 4065 as evidenced by distortions in their optical isophotes.

<span class="mw-page-title-main">NGC 4076</span> Galaxy in the constellation Coma Berenices

NGC 4076 is a spiral galaxy located 290 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 27, 1785 and is a member of the NGC 4065 Group.

<span class="mw-page-title-main">NGC 4302</span> Galaxy in the constellation Coma Berenices

NGC 4302 is an edge-on spiral galaxy located about 55 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

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  42. ↑ Schaefer, Bradley E. (2018-09-01). "The Distances to Novae As Seen By Gaia". arXiv.org. Retrieved 2024-09-10.
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  44. ↑ Kalari, V. M.; Vink, J. S.; Dufton, P. L.; Fraser, M. (2018-10-01). "How common is LBV S Doradus variability at low metallicity?". Astronomy & Astrophysics. 618: A17. doi:10.1051/0004-6361/201833484. ISSN   0004-6361.
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