This is a list of Wolf-Rayet stars, in order of their distance from Earth. [1] [2] [3]
Star system ← ← | Nebula | Median distance (ly) | Stars in system | Spectral type | Apparent magnitude (V) | Comments and references |
---|---|---|---|---|---|---|
Gamma² Velorum (WR 11/Suhail al Muhlif/Regor) | 1096+26 −23 | 2 | WC8 | 1.83 | The Closest Wolf-Rayet star to Earth. | |
HD 45166 | 3,232 | 2 | qWR | 9.88 | The primary of HD 45166 is currently the only known example of a qWR star. | |
HD 112313 | 3,377.2±153.6 | 1 | WC | Center star of NGC 4361 Nebula. | ||
WR 142 | 4,000 | 1 | WO2 | 12.94 | ||
HD 151932 (WR 78) | 4,100 | 1 | WN7h | 6.45 - 6.61 | ||
HD 326823 (V1104 Scorpii) | 4,142 | 1 | WNpec | 9.03 | ||
HD 151932 (WR 78) | 4,200 | 1 | WN7h | 6.45 - 6.61 | ||
EZ Canis Majoris (WR 6) | 4,900 | 1 | WN4-s | 6.91 | ||
WR 111 (HD 165763) | 5,316+320 −230 | 1 | WC5 | +7.82 | ||
WR 140 (SBC9 1232) | 5,600 ± 300 | 2 | WC7p | 6.85 | ||
HD 152408 (WR 79a) | 5,600 | 1 | WN9ha | 5.81-5.85 | ||
WR 93 | 5,900 | 1 | WC7 | |||
WR 133 (V1676 Cyg) | 6,100 ± 300 | 2 | WN5o | 6.75 - 6.84 | ||
HD 152408 (WR 79a) | 6,500 | 1 | WN9ha | 5.81-5.85 | ||
WR 25 (HD 93162) | 6,500 | 2 | O2.5If*/WN6 | 8.80 | ||
Apep (WR 70-16) | 6523+400 −300 | 3 | WR + WR | |||
CV Serpentis (WR 113) | 6,700 ± 200 | 2 | WC8d | 9.08 | ||
WR 136 (HD 192163) | 6,700 ± 500 | 1 | WN6(h)-s | 7.50 | ||
WR 86 | 6849 ± 800 | 1 | WR | 9.27 | ||
HD 83535 | 7,270 | 1 | WC3 | Central star of NGC 2867 Nebula. | ||
Theta Muscae (WR 48a) | 7,400 | 4 | WC5/6 | 5.53 | ||
WR 93b | 7,600 ± 500 | 1 | WO3 | 15.2 | ||
WR 2 | 8,186 | 1 | WN2-w | 11.33 | ||
WR 22 (V429 Carinae) | 8,300 ± 700 | 2 | WN7h | 6.42 | ||
WR 104 (V5097 Sgr) | 8,400 | 3 | WC9d | 13.28 + 15.36 | ||
AG Pegasi | 9,000 | 2 | WR | 6.0 - 9.4 | ||
WR 8 | 9,000 | 1 | WR | |||
WR 46 (DI Crucis) | 9,300 ± 900 | 1 | WN3p-w | 10.83 | ||
WR 3 | 9,458+520 −390 | 1 | WN3-hw | 10.69 | ||
WR 102 | 9,500 ± 600 | 1 | WO2 | 14.10 | ||
WR 138 | 10,000 | 1 | WR | |||
WR 1 | 10,500 ± 500 | 1 | WN4-s | 10.54 | ||
WR 157 | 11285.01 | 1 | WN4.5 | Member of Markarian 50 Cluster. | ||
WR 69 | 11,350 | 1 | WC9d | 9.1 | ||
WR 9 | 12,000 ± 600 | 2 | WC4 | 10.50 | ||
WR 142a | 13,000 | 1 | WR | |||
WR 21a | 13,100 ± 700 | 1 | O3/WN5ha + O3Vz((f*)) | 12.661 | ||
CD Crucis (WR 47) | 14,000 | 2 | WN6o | 10.81 | ||
WR 120–6 | 14,000 | 1 | WN4 | It is the central star of Abell 48 Planetary Nebula. | ||
WR 24 (HD 93131) | 14,000 | 1 | WN6ha-w | 6.48 - 6.50 | ||
WR 20a | 14,000 ± 1,000 | 2 | O3If*/WN6 + O3If*/WN6 | 13.28 | ||
WR 142b | 15,000 | 1 | WR | |||
WR 7 (HD 56925) | 16,000 | 1 | WN4-s | 11.56 | ||
AG Carinae | 17,000 ± 1,000 | 2 | WN11 | 6.96 | ||
WR 12 (V378 Velorum) | 19,000 ± 1,000 | 1 | WN8h | 10.78 | ||
OAO 1657-415 | 20,000 | 1 | Ofpe/WN9 | >23 | ||
WR 124 (QR Sagittae) | 21,000 ± 2,000 | 1 | WN8h | 11.50±0.11 | ||
WR 30a | 21,917+1,400 −1,090 | 1 | WO4 | |||
Cygnus X-3 (WR 145a/V1521 Cyg) | 24,135±1,100 | 1 | WN 4–6 | |||
NGC 3603-A1 (WR 43a/HD 97950A1) | 24,800 | 2 | WN6h+WN6h | 11.18 | ||
NGC 3603-B (WR 43b/HD 97950B) | 24,800 | 1 | WN6h | 11.33 | ||
NGC 3603-C (WR 43c/HD 97950C) | 24,800 | 1 | WN6h | 11.89 | ||
HD 97950 (WR 43) | 25,000 | 1 | WR | 9.03 | It is the central core of a super star cluster within the NGC 3603 H II region (similar to R136 within the Tarantula Nebula). | |
Arches-F1 (WR 102ad) | 25,000 | 1 | WN8-9h | |||
Arches-F6 (WR 102ah) | 25,000 | 1 | WN8-9h | |||
Arches-F9 (WR 102ae) | 25,000 | 1 | WN8-9h | |||
WR 42e (2MASS J11144550-115001) | 25,000 | 1 | O3If*/WN6 | 14.53 | ||
G0.059-0.068 | 26,000 | 1 | B0-1Ia+/WNLh | |||
G0.238-0.071 | 26,000 | 1 | WN11h | Present in the Galactic Center region of Milky Way. | ||
WR 102ka (Peony Star) | 26,000 | 1 | Ofpe/WN9 | |||
WR 102c | 26,000 | 1 | WN6 | 11.6 | ||
WR 102ea | 26,000 | 1 | WN9h | 8.8 | ||
GCIRS 13E (WR 101f) | 26,000 | 1 | WR | Located near Galactic Center. | ||
GCIRS 16SW | 26,000 | 1 | Ofpe/WN9 | Located near Galactic Center. | ||
WR 101-2 (CXOGC J174516.1-284909) | 26,092 | 1 | Ofpe/WN9 | |||
WR 31a (Hen 3-519) | 28,000 | 1 | WN11h | 10.85 | ||
WR 102e | 28,000 | 1 | WR | |||
WR 150 | 28,473+1,700 −1,380 | 1 | WC5 | 13.47 | ||
HD 826 | 30,000 | 1 | WC8 | Center Star of NGC 40 Nebula. | ||
WR 102b | 31,000 | 1 | WR | |||
Mercer 30-1 A (WR 46-3 A) | 40,000 | 1 | WR | |||
Mercer 30-7 A | 40,000 | 1 | WR | |||
The Large Magellanic Cloud (LMC) is around 163 kly distant and the Small Magellanic Cloud (SMC) is around 204 kly distant.
Host galaxy | Star system | Median distance (ly) | Stars in system | Spectral type | Apparent magnitude (V) | Comments and references |
---|---|---|---|---|---|---|
LMC | LMC195-1 | 160,000 | 1 | WO2 | 15.15 | |
LMC | LH 41-1042 | 160,000 | 1 | WO4 | 13.95 | |
LMC | R145 (HD 269928) | 163,000 | 2 | WN6h + O3.5If*/WN7 | 12.04 | |
LMC | HD 38282 (BAT99-118/Brey 89) | 163,000 | 2 | WN5-6h + WN6-7h | 11.11 | |
LMC | BAT99-7 | 163,000 | 1 | WN4b | 13.81 | |
LMC | BAT99-123 (Brey 93) | 163,000 | 1 | WO3 | 15.204 | |
LMC | Melnick 34 (BAT99-116) | 163,000 | 2 | WN5h + WN5h | 13.09 | |
LMC | R136a1 (RMC 136a1) | 163,000 | 1 | WN5h | 12.23 | |
LMC | R136a2 (RMC 136a2) | 163,000 | 1 | WN5h | 12.34 | |
LMC | R136a3 | 163,000 | 1 | WN5h | 12.97 | |
LMC | R136c | 163,000 | 1 | WN5h | 12.86 | |
LMC | R71 (HD 269006) | 164,000 | 1 | WR | 8.7 - 9.9 - 11.2 | |
LMC | VFTS 457 | 164,000 | 1 | O3.5If*/WN7 | ||
LMC | VFTS 482 | 164,000 | 1 | O3If*/WN6-A | ||
LMC | VFTS 545 | 164,000 | 1 | O2If*/WN5 | ||
LMC | VFTS 682 | 164,000 | 1 | WN5h | 16.08 | |
LMC | VFTS 1022 | 164,000 | 1 | O3.5If*/WN7 | ||
LMC | R134 | 164,000 | 1 | WR | ||
LMC | R146 | 164,000 | 1 | WN4 | ||
LMC | BAT99-98 | 165,000 | 1 | WN6 | 13.38 | |
LMC | R99 | 165,000 | 1 | Ofpe/WN10 | 11.46 | |
SMC | SMC AB7 | 197,000 | 2 | WN4 | 13.016 | |
SMC | SMC AB8 | 197,000 | 2 | WO4 | 12.83 | |
SMC | HD 5980 | 200,000 | 1 | WN4 | 8.8 - 11.9 | |
The Andromeda Galaxy (M31) is 2.5 Mly distant and the Triangulum Galaxy is around 3.2 Mly distant
Host galaxy | Star system | Median distance (ly) | Stars in system | Spectral type | Apparent magnitude (V) | Comments and references |
---|---|---|---|---|---|---|
Triangulum | [BMS2003] 867 | 2,700,000 | 2 | O4Iab+O4Ia | ||
Triangulum | Romano's Star | 2,700,000 | 2 | WN8h–WN11h | 16.5–18.8 | |
Host Galaxy | Star system | Median distance (ly) | Stars in system | Spectral type | Apparent magnitude (V) | Comments and references |
---|---|---|---|---|---|---|
NGC 6822 | NGC 6822-WR 12 (LGGS J194513.50-144512.9) | 1,540,000 | 1 | WN4 | 18.96 | |
The Large Magellanic Cloud (LMC) is a dwarf galaxy and satellite galaxy of the Milky Way. At a distance of around 50 kiloparsecs (163,000 light-years), the LMC is the second- or third-closest galaxy to the Milky Way, after the Sagittarius Dwarf Spheroidal (c. 16 kiloparsecs (52,000 light-years) away) and the possible dwarf irregular galaxy called the Canis Major Overdensity. Based on the D25 isophote at the B-band (445 nm wavelength of light), the Large Magellanic Cloud is about 9.86 kiloparsecs (32,200 light-years) across. It is roughly one-hundredth the mass of the Milky Way and is the fourth-largest galaxy in the Local Group, after the Andromeda Galaxy (M31), the Milky Way, and the Triangulum Galaxy (M33).
The Tarantula Nebula is a large H II region in the Large Magellanic Cloud (LMC), forming its south-east corner.
S Doradus is one of the brightest stars in the Large Magellanic Cloud (LMC), a satellite galaxy of the Milky Way, located roughly 160,000 light-years away. The star is a luminous blue variable, and one of the most luminous stars known, having a luminosity varying widely above and below 1,000,000 times the luminosity of the Sun, although it is too far away to be seen with the naked eye.
Messier 2 or M2 is a globular cluster in the constellation Aquarius, five degrees north of the star Beta Aquarii. It was discovered by Jean-Dominique Maraldi in 1746, and is one of the largest known globular clusters.
In astronomy, extinction is the absorption and scattering of electromagnetic radiation by dust and gas between an emitting astronomical object and the observer. Interstellar extinction was first documented as such in 1930 by Robert Julius Trumpler. However, its effects had been noted in 1847 by Friedrich Georg Wilhelm von Struve, and its effect on the colors of stars had been observed by a number of individuals who did not connect it with the general presence of galactic dust. For stars lying near the plane of the Milky Way which are within a few thousand parsecs of the Earth, extinction in the visual band of frequencies is roughly 1.8 magnitudes per kiloparsec.
The Magellanic Stream is a stream of high-velocity clouds of gas extending from the Large and Small Magellanic Clouds over 100° through the Galactic south pole of the Milky Way. The stream contains a gaseous feature dubbed the leading arm. The stream was sighted in 1965 and its relation to the Magellanic Clouds was established in 1974.
HD 37974 a variable B[e] hypergiant in the Large Magellanic Cloud. It is surrounded by an unexpected dust disk.
HD 269810 is a blue giant star in the Large Magellanic Cloud. It is one of the most massive and most luminous stars known, and one of only a handful of stars with the spectral type O2.
In astronomy, stellar kinematics is the observational study or measurement of the kinematics or motions of stars through space.
WOH G64 is an unusual red supergiant (RSG) star in the Large Magellanic Cloud (LMC) satellite galaxy in the southern constellation of Dorado. It is the largest known star with a well-defined radius. It is also one of the most luminous and massive red supergiants, with a radius calculated to be around 1,540 times that of the Sun (R☉) and a luminosity around 282,000 times the solar luminosity (L☉).
Mensa is a constellation in the Southern Celestial Hemisphere near the south celestial pole, one of fourteen constellations drawn up in the 18th century by French astronomer Nicolas-Louis de Lacaille. Its name is Latin for table, though it originally commemorated Table Mountain and was known as "Mons Mensae". One of the eighty-eight constellations designated by the International Astronomical Union (IAU), it covers a keystone-shaped wedge of sky 153.5 square degrees in area. Other than the south polar constellation of Octans, it is the most southerly of constellations and is observable only south of the 5th parallel of the Northern Hemisphere.
Classical Cepheids are a type of Cepheid variable star. They are young, population I variable stars that exhibit regular radial pulsations with periods of a few days to a few weeks and visual amplitudes ranging from a few tenths of a magnitude up to about 2 magnitudes. Classical Cepheids are also known as Population I Cepheids, Type I Cepheids, and Delta Cepheid variables.
S Vulpeculae is a variable star located in the constellation Vulpecula. A supergiant star, it is around 382 times the diameter of the Sun.
HV 2112 is a cool luminous variable star in the Small Magellanic Cloud. Until 2018, it was considered to be the most likely candidate for a Thorne–Żytkow object, but it is now thought to be an asymptotic giant branch star.
R Sagittae is an RV Tauri variable star in the constellation Sagitta that varies from magnitude 8.0 to 10.5 in 70.77 days. It is a post-AGB low mass yellow supergiant that varies between spectral types G0Ib and G8Ib as it pulsates. Its variable star designation of "R" indicates that it was the first star discovered to be variable in the constellation. It was discovered in 1859 by Joseph Baxendell, though classified as a semi regular variable until RV Tauri variables were identified as a distinct class in 1905.
NGC 121 is a globular cluster of stars in the southern constellation of Tucana. It is the oldest globular cluster in the Small Magellanic Cloud (SMC), which is a dwarf satellite galaxy of the Milky Way. This cluster was first discovered by English astronomer John Herschel on September 20, 1835. The compiler of the New General Catalogue, Danish astronomer John Louis Emil Dreyer, described this object as "pretty bright, pretty small, little extended, very gradually brighter middle". The cluster is located at a distance of around 200,000 light-years (60 kpc) from the Sun.
HV 11423 is a red supergiant star in the Small Magellanic Cloud. It is about 200,000 light-years away towards the constellation of Tucana.