List of most luminous stars

Below is a list of stars arranged in order of decreasing luminosity (increasing bolometric magnitude). Accurate measurement of stellar luminosities is quite difficult in practice, even when the apparent magnitude is measured accurately, for four reasons:

  1. The distance d to the star must be known, to convert apparent to absolute magnitude. Absolute magnitude is the apparent magnitude a star would have if it were 10 parsecs away from the viewer. Since apparent brightness decreases as the square of the distance (i.e. as 1/d2), a small error (e.g. 10%) in determining d implies an error ~2× as large (thus 20%) in luminosity. Stellar distances are only directly measured accurately out to d ~1,000 lt-yrs.
  2. The observed magnitudes must be corrected for the absorption or extinction of intervening interstellar or circumstellar dust and gas. This correction can be enormous and difficult to determine precisely. For example, until accurate infrared observations became possible ~50 years ago, the Galactic Center of the Milky Way was totally obscured to visual observations.
  3. The magnitudes at the wavelengths measured must be corrected for those not observed. "Absolute bolometric magnitude" (which term is redundant, practically speaking, since bolometric magnitudes are nearly always "absolute", i.e. corrected for distance) is a measure of the star's luminosity, summing over its emission at all wavelengths, and thus the total amount of energy radiated by a star every second. Bolometric magnitudes can only be estimated by correcting for unobserved portions of the spectrum that have to be modelled, which is always an issue, and often a large correction. The list is dominated by hot blue stars which produce the majority of their energy output in the ultraviolet, but these may not necessarily be the brightest stars at visual wavelengths.
  4. A large proportion of stellar systems discovered with very high luminosity have later been found to be binary. Usually, this results in the total system luminosity being reduced and spread among several components. These binaries are common both because the conditions that produce high mass high luminosity stars also favour multiple star systems, but also because searches for highly luminous stars are inevitably biased towards detecting systems with multiple more normal stars combining to appear luminous.
This article is about luminosity. For apparent magnitude, see List of brightest stars.

Because of all these problems, other references may give very different values for the most luminous stars (different ordering or different stars altogether). Data on different stars can be of somewhat different reliability, depending on the attention one particular star has received as well as largely differing physical difficulties in analysis (see the Pistol Star for an example). The last stars in the list are familiar nearby stars put there for comparison, and not among the most luminous known. It may also interest the reader to know that the Sun is more luminous than approximately 95% of all known stars in the local neighbourhood (out to, say, a few hundred light years), due to enormous numbers of somewhat less massive stars that are cooler and often much less luminous. For perspective, the overall range of stellar luminosities runs from dwarfs less than 1/10,000th as luminous as the Sun to supergiants over 1,000,000 times more luminous.

Data

This list is currently limited mostly to objects in our galaxy and the Magellanic Clouds, but a few stars in other local group galaxies can now be examined in enough detail to determine the luminosities. Some suspected binaries in this magnitude range are excluded because there is insufficient information about the luminosity of the individual components. Selected fainter stars are also shown for comparison. Despite their extreme luminosity, many of these stars are nevertheless too distant to be observed with the naked eye. Stars that are at least sometimes visible to the unaided eye have their apparent magnitude (6.5 or brighter) highlighted in blue.

The first list show a few of the known stars with an estimated luminosity of 1 million L☉ or greater, including the stars in open cluster, OB association and H II region. The majority of stars thought to be more than 1 million L☉ are shown, but the list is incomplete.

The second list gives some notable stars for the purpose of comparison.

This list is incomplete; you can help by adding missing items with reliable sources.
Legend
Milky Way
Large Magellanic Cloud
Small Magellanic Cloud
Andromeda Galaxy
Triangulum Galaxy
Kinman's dwarf
Stars with 1 million L☉ or greater
Star name Bolometric
luminosity
(L☉, Sun = 1)		 Absolute
bolometric
magnitude		 Approx. distance
from earth
(in light-years)		 Apparent
visible magnitude		 Effective
temperature (K)		 Reference
R136a1 (in Tarantula Nebula of LMC) 6,166,000 -12.235 163,000 12.23 46,000 [1]
R136a2 (in Tarantula Nebula of LMC) 5,623,000 -12.135 160,000 12.34 50,000 [1]
BAT99-98 (in Tarantula Nebula of LMC) 5,012,000 -12.01 165,000 13.38 45,000 [2]
G0.238-0.071 (in Galactic Center) 5,012,000 -12.01 26,000 14.37 (J band) [3]
M33-013406.63 (in M33) 4,677,000 -11.935 3,000,000 16.084 30,000 [4][lower-alpha 1]
Eta Carinae A (in Trumpler 16 of Carina Nebula) 4,600,000 -11.917 7,500 4.3 (combined) 9,400-35,200 [5][lower-alpha 2]
R136a3 (in Tarantula Nebula of LMC) 4,266,000 -11.835 160,000 12.97 50,000 [1]
V4998 Sagittarii (near Quintuplet Cluster) 3,981,000 -11.76 25,000 12.534 (J band) 12,000 [6]
R136c (in Tarantula Nebula of LMC) 3,802,000 -11.71 160,000 12.86 51,000 [7]
Melnick 42 (in Tarantula Nebula of LMC) 3,631,000 -11.66 160,000 12.78 47,300 [8]
G0.070+0.025 (in Galactic Center) 3,311,000 -11.56 26,000 14.799 (J band) [3]
Pistol Star (V4647 Sagittarii in Quintuplet cluster) 3,300,000 -11.556 25,100 11.79 (J band) 11,800 [9]
VFTS 682 (in Tarantula Nebula of LMC) 3,236,000 -11.535 160,000 16.75 52,200 [8]
WR 42e (in HD 97950 of NGC 3603) 3,200,000 -11.523 25,000 14.53 43652 [10][lower-alpha 3]
Peony Star (WR 102ka near Galactic Center) 3,162,000 -11.51 26,100 12.978 (J band) 25,100 [11]
R99 (in N41 of LMC) 3,162,000 -11.51 160,000 11.46 28,000 [2]
Var A-1 (in M31) 3,133,000 -11.5 2,450,000 17.143 20,400-28,100 [12]
VFTS 1022 (in Tarantula Nebula of LMC) 3,020,000 -11.46 164,000 13.44 42,200 [8]
WR 24 (in Collinder 228 of Carina Nebula) 2,951,000 -11.435 8,200 6.48 50,100 [13]
G0.059-0.068 (in Galactic Center) 2,884,000 -11.41 26,000 13.337 (J band) [3]
HD 97950 B (WR 43b in HD 97950 of NGC 3603) 2,884,000 -11.41 24,000 11.33 42,000 [14]
Melnick 34 A (in Tarantula Nebula of LMC) 2,692,000 -11.335 160,000 13.09 (combined) 53,000 [15]
WR 102hb (in Quintuplet Cluster) 2,630,000 -11.31 26,000 13.9 (J band) 25,100 [16]
R146 (in Tarantula Nebula of LMC) 2,512,000 -11.26 160,000 13.116 [2]
VFTS 482 (in Tarantula Nebula of LMC) 2,512,000 -11.26 164,000 13 42,200 [8]
PHL 293B (in PHL 293B) 2,500,000 -11.255 74,000,000 16.87 6,000-6,800 [17]
HD 97950 A1a (WR 43a A in HD 97950 of NGC 3603) 2,455,000 -11.235 24,000 11.18 (combined) 42,000 [14]
WR 102ea (in Quintuplet Cluster) 2,455,000 -11.235 26,000 25,100 [16]
WR 25 A (in Trumpler 16 of Carina Nebula) 2,399,000 -11.21 6,800 8.8 50,100 [13][lower-alpha 4]
LGGS J004444.52+412804.0 (in M31) 2,377,000 -11.2 2,550,000 7,000-18,000 [12]
WR 93 (in Pismis 24 of NGC 6357) 2,377,000 -11.2 [18]
Melnick 34 B (in Tarantula Nebula of LMC) 2,344,000 -11.185 [15]
HD 5980 A (in NGC 346 of SMC) 2,239,000 -11.135 200,000 11.7 21,000-53,000 [19][lower-alpha 5]
HD 97950 C1 (WR 43c A in HD 97950 of NGC 3603) 2,239,000 -11.135 [14][lower-alpha 4]
R136b (in Tarantula Nebula of LMC) 2,239,000 -11.135 165,000 13.24 35,000 [1]
R145 A (in Tarantula Nebula of LMC) 2,239,000 -11.135 163,000 11.94 (combined) 50,000 [20]
Var 83 (in M33) 2,239,000 -11.135 3,000,000 16.4 18,000-37,000 [21]
WR 102ae (in Arches Cluster) 2,239,000 -11.135 25,000 36,600 [22]
WR 102ah (in Arches Cluster) 2,239,000 -11.135 25,000 33,900 [22]
HD 269810 (in NGC 2032 of LMC) 2,188,000 -11.11 170,000 12.28 52,500 [23]
VFTS 1021 (in Tarantula Nebula of LMC) 2,188,000 -11.11 164,000 13.31 39,800 [8]
G0.058+0.014 (in Galactic Center) 2,138,000 -11.085 26,000 [3]
HSH95-36 (in Tarantula Nebula of LMC) 2,138,000 -11.085 163,000 14.39 48,000 [1]
R145 B (in Tarantula Nebula of LMC) 2,138,000 -11.085 163,000 11.94 (combined) 43,000 [20]
WR 89 (in HM 1) 2,138,000 -11.085 9,400 11.02 39,800 [13]
AFGL 2298 (near Galactic plane) 2,000,000 -11.013 33,000 [24][lower-alpha 6]
LBV 1806-20 (in G10.0–0.3 of Galactic Center) 1,995,000 -11.01 28,000 18,000-32,000 [25]
VFTS 545 (in Tarantula Nebula of LMC) 1,995,000 -11.01 164,000 13.4 47,300 [8]
WR 102ad (in Arches Cluster) 1,995,000 -11.01 25,000 33,200 [22]
WR 102aj (in Arches Cluster) 1,995,000 -11.01 25,000 32,900 [22]
WR 102al (in Arches Cluster) 1,995,000 -11.01 25,000 36,800 [22]
WR 147S (in Cygnus OB2) 1,995,000 -11.01 2,100 14.89 39,800 [13][lower-alpha 4]
WR 102aaa (in Galactic Center) 1,950,000 -10.985 26,000 [3]
R136a5 (in Tarantula Nebula of LMC) 1,950,000 -10.985 165,000 13.71 46,000 [1]
AB6 A (in N76 of SMC) 1,905,000 -10.96 [19]
R136a8 (in Tarantula Nebula of LMC) 1,905,000 -10.96 165,000 14.42 51,000 [26]
WR 22 A (in Bochum 10 of Carina Nebula) 1,905,000 -10.96 8,200 6.42 44,700 [13]
R136a6 (in Tarantula Nebula of LMC) 1,862,000 -10.935 165,000 13.35 53,000 [1]
WR 31a (in Blue Bubble Nebula) 1,820,000 -10.91 26,000 10.85 30,200 [27]
LGGS J004051.59+403303.0 (in M31) 1,803,000 -10.9 2,550,000 16.99 [12]
MSX5C G358.5391+00.1305 (in Wray 17-96) 1,800,000 -10.898 15,000 17.8 13,000 [28]
HD 5980 B (in NGC 346 of SMC) 1,778,000 -10.885 200,000 11.9 45,000 [19]
R136a7 (in Tarantula Nebula of LMC) 1,778,000 -10.885 165,000 13.97 49,000 [1]
WR 130 (in Cygnus OB3) 1,778,000 -10.885 8,800 12.14 44,700 [13]
WR 21a A (Runaway star from Westerlund 2) 1,778,000 -10.885 [29]
V4650 Sagittarii (in Quintuplet cluster) 1,770,000 -10.88 25,000 11,300 [30]
R136a4 (in Tarantula Nebula of LMC) 1,738,000 -10.86 160,000 13.96 48,000 [1]
VFTS 506 (in Tarantula Nebula of LMC) 1,738,000 -10.86 160,000 13.31 47,300 [8]
R147 (in Tarantula Nebula of LMC) 1,698,000 -10.835 160,000 12.75 [2]
VFTS 16 (in Tarantula Nebula of LMC) 1,698,000 -10.835 160,000 13.55 53,100 [8]
Cygnus OB2 #12 A (in Cygnus OB2) 1,660,000 -10.81 5,000 11.4 13,700 [31][lower-alpha 4]
VFTS 1017 (in Tarantula Nebula of LMC) 1,622,000 -10.785 164,000 14.5 50,100 [8]
WR 87 (in HM 1) 1,622,000 -10.785 9,400 11.95 44,700 [13]
AF Andromedae (in M31) 1,585,000 -10.76 2,500,000 17.325 28,000 [21]
VFTS 457 (in Tarantula Nebula of LMC) 1,585,000 -10.76 164,000 13.74 39,800 [8]
WR 102af (in Arches Cluster) 1,585,000 -10.76 25,000 36,900 [22]
WR 102df (in Quintuplet cluster) 1,585,000 -10.76 26,000 25,100 [16]
WR 107 (in Sagittarius OB1) 1,585,000 -10.76 13,400 14.1 50,100 [13]
WR 148 A (Runaway star from Galactic plane) 1,585,000 -10.76 27,100 10.3 39,800 [13]
SK -68 137 (in KMK88-92 of LMC) 1,549,000 -10.735 [23]
WR 102i (in Quintuplet cluster) 1,549,000 -10.735 26,000 31,600 [16]
HD 97950 A1b (WR 43a B in HD 97950 of NGC 3603) 1,514,000 -10.71 24,000 11.18 (combined) 40,000 [14]
HM 1-6 (in HM 1) 1,500,000 -10.7 [18]
LGGS J013245.41+303858.3 (in M33) 1,500,000 -10.7 2,700,000 34,000 [32]
HD 93129 Aa (in Trumpler 14 of Carina Nebula) 1,479,000 -10.685 7,500 7.31 42,500 [33]
HSH95-46 (in Tarantula Nebula of LMC) 1,445,000 -10.66 163,000 14.67 49,000 [1]
VFTS 542 (in Tarantula Nebula of LMC) 1,445,000 -10.66 164,000 13.47 44,700 [8]
AB8 A (in NGC 602 of SMC) 1,413,000 -10.635 200,000 12.9 (combined) 141,000 [19]
Arches-F15 (in Arches Cluster) 1,413,000 -10.635 25,000 35,600 [22]
LGGS J013235.25+303017.6 (in M33) 1,413,000 -10.635 [4]
R134 (in Tarantula Nebula of LMC) 1,413,000 -10.635 160,000 12.02 47,000 [2]
S Doradus (in NGC 1910 of LMC) 1,413,000 -10.635 169,000 20,000 [34]
WR 66 (in Circinus OB1) 1,413,000 -10.635 10,700 11.34 44,700 [13]
HD 37974 (in N135 of LMC) 1,400,000 -10.625 160,000 10.91 22,500 [35]
VFTS 621 (in Tarantula Nebula of LMC) 1,380,000 -10.61 160,000 15.39 54,000 [8]
WR 131 (in Cygnus OB3) 1,380,000 -10.61 38,600 12.08 44,700 [13]
VFTS 427 (in Tarantula Nebula of LMC) 1,349,000 -10.585 164,000 13.76 39,800 [8]
WR 18 (in Carinae OB1 of Carina Nebula) 1,288,000 -10.535 [13]
AB7 A (in NGC 371 of SMC) 1,259,000 -10.51 197,000 13.016 105,000 [19]
HD 50064 (in NGC 2301) 1,259,000 -10.51 9,500 8.21 13,500 [36]
R139 A (in Tarantula Nebula of LMC) 1,259,000 -10.51 160,000 12.0 (combined) [37]
VFTS 259 (in Tarantula Nebula of LMC) 1,259,000 -10.51 160,000 13.65 [8]
VFTS 642 (in Tarantula Nebula of LMC) 1,259,000 -10.51 [38]
WR 102ag (in Arches Cluster) 1,259,000 -10.51 25,000 32,900 [22]
WR 102bb (in Arches Cluster) 1,259,000 -10.51 25,000 29,600 [22]
Trumpler 27-27 (in Trumpler 27) 1,247,000 -10.5 8,200 [18]
HSH95-47 (in Tarantula Nebula of LMC) 1,230,000 -10.485 163,000 14.63 47,000 [1]
VFTS 1028 (in Tarantula Nebula of LMC) 1,230,000 -10.485 160,000 13.82 47,300 [8]
LH 10-3601 (in N11 of LMC) 1,202,000 -10.46 [23]
AB1 (in DEM S10 of SMC) 1,175,000 -10.435 [39]
BI 253 (Runaway star from Tarantula Nebula of LMC) 1,175,000 -10.435 [7]
LGGS J013248.26+303950.4 (in M33) 1,175,000 -10.435 [4]
NGC 346-W3 (in NGC 346 of SMC) 1,175,000 -10.435 [23]
WR 102df (in Quintuplet cluster) 1,175,000 -10.435 26,000 10.5 35,100 [16]
WR 126 (in Vulpecula OB2) 1,175,000 -10.435 [40]
WR 20a A (in Westerlund 2) 1,150,000 -10.412 [41]
WR 20a B (in Westerlund 2) 1,150,000 -10.412 [41]
BAT99-104 (in Tarantula Nebula of LMC) 1,148,000 -10.41 160,000 12.5 63,000 [2]
WR 102-16 (in Galactic Center) 1,148,000 -10.41 26,000 [3]
G359.797+0.037 (in Galactic Center) 1,148,000 -10.41 26,000 [3]
HD 93205 A (in Trumpler 16 of Carina Nebula) 1,148,000 -10.41 [42]
WR 158 (in Cassiopeia OB1) 1,148,000 -10.41 26,000 11.24 44,700 [13]
WR 28 (in FSR 1555) 1,148,000 -10.41 [13]
HD 303308 (in Trumpler 16 of Carina Nebula) 1,138,000 -10.4 [18]
M33C-15235 (in M33) 1,138,000 -10.4 2,700,000 29,200 [32]
AB9 (in DEM S80 of SMC) 1,122,000 -10.385 [39]
Arches-F18 (in Arches Cluster) 1,122,000 -10.385 25,000 [22]
HSH95-48 (in Tarantula Nebula of LMC) 1,122,000 -10.385 163,000 14.72 49,000 [1]
Var B (in M33) 1,122,000 -10.385 3,000,000 16.208 [21]
VFTS 562 (in Tarantula Nebula of LMC) 1,122,000 -10.385 160,000 13.66 42,200 [8]
WR 37 (in SFC 27 of G291.27-0.71) 1,122,000 -10.385 [13]
VFTS 512 (in Tarantula Nebula of LMC) 1,096,000 -10.36 [8]
VFTS 3 (in Tarantula Nebula of LMC) 1,072,000 -10.335 [7]
VFTS 151 (in Tarantula Nebula of LMC) 1,072,000 -10.335 160,000 14.28 42,200 [8]
VFTS 603 (in Tarantula Nebula of LMC) 1,060,000 -10.323 [43]
HD 93403 A (in Trumpler 16 of Carina Nebula) 1,047,000 -10.31 10,000 7.3 39,300 [44]
R133 (in Tarantula Nebula of LMC) 1,047,000 -10.31 160,000 12.49 37,600 [8]
HD 229059 (in Berkeley 87) 1,038,000 -10.3 3,200 8.7 26,300 [18]
M33C-10788 (in M33) 1,038,000 -10.3 2,700,000 32,000 [32]
HD 93250 A (in Trumpler 16 of Carina Nebula) 1,023,000 -10.285 7,500 7.5 46,000 [45][lower-alpha 4]
HSH95-31 (in Tarantula Nebula of LMC) 1,023,000 -10.285 163,000 14.35 48,000 [1]
VFTS 267 (in Tarantula Nebula of LMC) 1,023,000 -10.285 160,000 13.49 44,700 [8]
VFTS 599 (in Tarantula Nebula of LMC) 1,023,000 -10.285 [7]
WR 156 (in Cepheus OB1) 1,023,000 -10.285 [13]
BAT99-68 (in Tarantula Nebula of LMC) 1,000,000 -10.26 160,000 14.13 45,000 [2]
VFTS 64 (in Tarantula Nebula of LMC) 1,000,000 -10.26 160,000 14.62 39,800 [8]
VFTS 602 (in Tarantula Nebula of LMC) 1,000,000 -10.26 [38]
VFTS 687 (in Tarantula Nebula of LMC) 1,000,000 -10.26 [38]
WR 102aa (in Arches Cluster) 1,000,000 -10.26 25,000 33,500 [22]
WR 102ba (in Arches Cluster) 1,000,000 -10.26 25,000 34,500 [22]
A few notable stars of luminosity less than 1 million L☉ are kept here for the purpose of comparison.
P Cygni 610000 -9.7 5900 4.8 18700
ζ Puppis 550000 -9 1090 2.21 40000
ρ Cassiopeiae 500000 -9.6 3400 4.1 to 6.2 5777
Alnilam 389000 -9.2 1300 1.7 27000
RW Cephei 295000 -9.11 11500 6.52 3750
VY Canis Majoris 270000 -9.4 3900 6.5 to 9.6 90
Plaskett's star A 224000 -8.6 6600 6.06 (A + B) 2000
θ1 Orionis C 204000 -8.6 1500 5.13 1000
VV Cephei A 200000 -9 4900 4.91 3826
Deneb 196000 -8.38 2600 1.25 75
μ Cephei (the Garnet Star) 135000 -8.09 2090 4.04 3551
Betelgeuse 126000 -8 643 0.58 3590
Rigel 120000 -7.84 860 0.12 150
Antares 97000 -7.2 600 0.92 3570
Canopus 15100 -5.53 310 -0.74 6998
Bellatrix 9211 -2.78 250 1.64 22000
Polaris Aa 1260 -3.6 433 1.97 6015
Aldebaran 518 -0.63 65 0.85 3910
Arcturus 170 -0.31 37 -0.04 30
Capella Aa 78.7 0.4 42 0.08 50
Vega 40.12 0.58 25 0 180
Sirius A 25.4 1.4 8.6 -1.46 9940
α Centauri A 1.519 4.38 4.4 -0.01 5790
Sun (Sol) 1.00 4.74 0.0000158 -26.74 5772
  1. M33-013406.63, also called LGGS J013406.63+304147.8, was thought of as a star with over 8 million luminosity in the past, but a new reference indicated that M33-013406.63 maybe a binary, the primary will be reduced to about 4 million luminosity.
  2. Identified as a binary system, or possibly three stars. The secondary is also luminous at around 1,000,000 times the Sun, but almost completely swamped by the primary.
  3. The paper mistakenly lists the bolometric magnitude as −10.5 instead of −11.5.
  4. This is a binary system but the secondary is much less luminous than the primary.
  5. Variable, luminosity was five times higher at outburst in 1994.
  6. Luminous blue variable, peak luminosity shown.

Note that even the most luminous stars are much less luminous than the more luminous persistent extragalactic objects, such as quasars. For example, 3C 273 has an average apparent magnitude of 12.8 (when observing with a telescope), but an absolute magnitude of −26.7. If this object were 10 parsecs away from Earth it would appear nearly as bright in the sky as the Sun (apparent magnitude −26.74). This quasar's luminosity is, therefore, about 2 trillion (1012) times that of the Sun, or about 100 times that of the total light of average large galaxies like our Milky Way. (Note that quasars often vary somewhat in luminosity.)

In terms of gamma rays, a magnetar (type of neutron star) called SGR 1806−20, had an extreme burst reach Earth on 27 December 2004. It was the brightest event known to have impacted this planet from an origin outside the Solar System; if these gamma rays were visible, with an absolute magnitude of approximately −29, it would have been brighter than the Sun (as measured by the Swift spacecraft).

The gamma-ray burst GRB 971214 measured in 1998 was at the time thought to be the most energetic event in the observable universe, with the equivalent energy of several hundred supernovae. Later studies pointed out that the energy was probably the energy of one supernova which had been "beamed" towards Earth by the geometry of a relativistic jet.

See also

References
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  4. Kourniotis, M; Kraus, M; Arias, M L; Cidale, L; Torres, A F (2018-11-01). "On the evolutionary state of massive stars in transition phases in M33". Monthly Notices of the Royal Astronomical Society. 480 (3): 3706–3717. arXiv:1808.00008. doi:10.1093/mnras/sty2087. ISSN 0035-8711.
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