List of most massive stars

Short description: None

This is a list of the most massive stars that have been discovered, in solar mass units (M☉).

## Contents

* 1 Uncertainties and caveats
* 1.1 Complications with distance and obscuring clouds
* 1.2 Rare reliable estimates
* 1.3 Relevance of stellar evolution
* 1.4 Mass limits
* 1.4.1 Accretion limits
* 1.4.2 Eddington mass limit
* 2 List of the most massive known stars
* 3 Black holes
* 4 See also
* 5 Footnotes
* 6 References
* 7 External links

## Uncertainties and caveats

Most of the masses listed below are contested and, being the subject of current research, remain under review and subject to constant revision of their masses and other characteristics. Indeed, many of the masses listed in the table below are inferred from theory, using difficult measurements of the stars' temperatures, composition, and absolute brightnesses. All the masses listed below are uncertain: Both the theory and the measurements are pushing the limits of current knowledge and technology. Both theories and measurements could be incorrect.

Artist's impression of disc of obscuring material around a massive star.

### Complications with distance and obscuring clouds

Since massive stars are rare, astronomers must look very far from Earth to find them. All the listed stars are many thousands of light years away making their light especially faint, which makes measurements difficult. In addition to being far away, many stars of such extreme mass are surrounded by clouds of outflowing gas created by extremely powerful stellar winds. This outflow obscures the stars, making it difficult to determine the physical properties of the star needed to calculate its mass: The surrounding gas interferes with the already difficult-to-obtain measurements of stellar temperatures and brightnesses, which greatly complicates the issue of estimating internal chemical compositions and structures.[lower-alpha 1]

Eta Carinae is the bright spot hidden in the double-lobed dust cloud. It is the most massive star that has a Bayer designation. It was only discovered to be (at least) two stars in the past few decades.

Both the obscuring clouds and the great distances also make it difficult to judge whether the star is just a single supermassive object or, instead, a multiple star system. A number of the "stars" listed below may actually be two or more companions orbiting too closely for our telescopes to distinguish, each star possibly being massive in itself but not necessarily "supermassive" to either be on this list, or near the top of it. And certainly other combinations are possible – for example a supermassive star with one or more smaller companions or more than one giant star – but without being able to clearly see inside the surrounding cloud, it is difficult to know what kind of object is actually generating the bright point of light seen from the Earth.

More globally, statistics on stellar populations seem to indicate that the upper mass limit is in the 120-solar-mass range,[1] so any mass estimate above this range is suspect.

### Rare reliable estimates

Eclipsing binary stars are the only stars whose masses are estimated with some confidence. However, note that almost all of the masses listed in the table below were inferred by indirect methods; only a few of the masses in the table were determined using eclipsing systems.

Amongst the most reliable listed masses are those for the eclipsing binaries NGC 3603-A1, WR 21a, and WR 20a. Masses for all three were obtained from orbital measurements.[lower-alpha 2] This involves measuring their radial velocities and also their light curves. The radial velocities only yield minimum values for the masses, depending on inclination, but light curves of eclipsing binaries provide the missing information: inclination of the orbit to our line of sight.

### Relevance of stellar evolution

Some stars may once have been more massive than they are today. Many large stars have likely suffered significant mass loss – perhaps as much as several tens of solar masses. The lost mass is expected to have been expelled by superwinds: high velocity winds that are driven by the hot photosphere into interstellar space. The process forms an enlarged extended envelope around the star that interacts with the nearby interstellar medium and infuses the adjacent volume of space with elements heavier than hydrogen or helium.[lower-alpha 3]

There are also – or rather were – stars that might have appeared on the list but no longer exist as stars, or are supernova impostors; today we see only their debris.[lower-alpha 4] The masses of the precursor stars that fueled these destructive events can be estimated from the type of explosion and the energy released, but those masses are not listed here.

This list only concerns "living" stars – those which are still seen by Earth-based observers existing as active stars: Still engaged in interior nuclear fusion that generates heat and light. That is, the light now arriving at the Earth as images of the stars listed still shows them to internally generate new energy as of the time (in the distant past) that light now being received was emitted. The list specifically excludes both white dwarfs – former stars that are now seen to be "dead" but radiating residual heat – and black holes – fragmentary remains of exploded stars which have gravitationally collapsed, even though accretion disks surrounding those black holes might generate heat or light exterior to the star's remains (now inside the black hole), radiated by infalling matter (see § Black holes below).

### Mass limits

There are two related theoretical limits on how massive a star can possibly be: The accretion mass limit and the Eddington mass limit.

* The accretion limit is related to star formation: After about 120 M☉ have accreted in a protostar, the combined mass should have become hot enough for its heat to drive away any further incoming matter. In effect, the protostar reaches a temperature where it evaporates away material already collected as fast as it collects new material.
* The Eddington limit is based on light pressure from the core of an already-formed star: As mass increases past ~150 M☉, the intensity of light radiated from a Population I star's core will become sufficient for the light-pressure pushing outward to exceed the gravitational force pulling inward, and the surface material of the star will be free to float away into space. Since their different compositions make them more transparent, Population II and Population III stars have higher and much higher mass limits, respectively.

#### Accretion limits

Astronomers have long hypothesized that as a protostar grows to a size beyond 120 M☉, something drastic must happen.[2] Although the limit can be stretched for very early Population III stars, and although the exact value is uncertain, if any stars still exist above 150~200 M☉ they would challenge current theories of stellar evolution.

Studying the Arches Cluster, which is currently the densest known cluster of stars in our galaxy, astronomers have confirmed that no stars in that cluster exceed about 150 M☉.

The R136 cluster is an unusually dense collection of young, hot, blue stars.

Rare ultramassive stars that exceed this limit – for example in the R136 star cluster – might be explained by an exceptional event hypothesized to have occurred: some of the pairs of massive stars in close orbit in young, unstable multiple-star systems must, on rare occasions, collide and merge when certain unusual circumstances hold that make a collision possible.[3]

#### Eddington mass limit

Main article: Astronomy:Eddington luminosity

Eddington's limit on stellar mass arises because of light-pressure: For a sufficiently massive star the outward pressure of radiant energy generated by nuclear fusion in the star's core exceeds the inward pull of its own gravity. The lowest mass for which this effect is active is the Eddington limit.

Stars of greater mass have a higher rate of core energy generation, and heavier stars' luminosities increase far out of proportion to the increase in their masses. The Eddington limit is the point beyond which a star ought to push itself apart, or at least shed enough mass to reduce its internal energy generation to a lower, sustainable rate. The actual limit-point mass depends on how opaque the gas in the star is, and metal-rich Population I stars have lower mass limits than metal-poor Population II stars. Before their demise, the hypothetical metal-free Population III stars would have had the highest allowed mass, somewhere around 300 M☉.

In theory, a more massive star could not hold itself together because of the mass loss resulting from the outflow of stellar material. In practice the theoretical Eddington Limit must be modified for high luminosity stars and the empirical Humphreys–Davidson limit is used instead.[4]

## List of the most massive known stars

Legend  Wolf–Rayet star

Luminous blue variable/Slash star
O-type star
B-type star
A-type star

The following two lists show a few of the known stars, including the stars in open clusters, OB associations, and H II regions. Despite their high luminosity, many of them 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 with a sky blue background.

The first list gives stars that are estimated to be 60 M☉ or larger; the majority of which are shown. The second list includes some notable stars which are below 60 M☉ for the purpose of comparison. The method used to determine each star's mass is included to give an idea of the data's uncertainty; note that the mass of binary stars can be determined far more accurately. The masses listed below are the stars' current (evolved) mass, not their initial (formation) mass.

This list is incomplete; you can help by expanding it.

Stars with 60 M☉ or greater Name  | Location  | M (M☉)  | L (L☉)  | Teff (K)  | Spectral type | Dist. (ly)  | mV | Mass estimated by  | Link  | Refs

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R136a1 | R136 | 291±46 | 7,244,000+699,000
−1,078,000 | 46,000+1,250
−2,375 | WN5h | 163,000  | 12.28±0.01 | evolution | SIMBAD | [5][6][7][8]
W49-2 | W49 South | 250±120 | 4,365,000+3,397,000
−1,910,000 | 35,500+1,700
−1,600 | O2–3.5If*  | 36,200  |  | evolution | SIMBAD | [9][10]
BAT99-98 | NGC 2070 | 226 | 5,012,000 | 45,000 | WN6  | 165,000  | 13.5 | mass-luminosity relation | SIMBAD
R136a2 | R136 | 195±35 | 5,129,000+367,000
−342,000 | 47,000+1,000
−625 | WN5h  | 163,000  | 12.80±0.01 | evolution | SIMBAD | [5][6][7][8]
Melnick 42 | R136 | 189 | 3,631,000 | 47,300 | O2If* | 163,000  | 12.86 | mass-luminosity relation | SIMBAD | [11][12]
R136a3 | R136 | 184±40 | 5,012,000+236,000
−226,000 | 50,000+2,500
−8,000 | WN5h  | 163,000  | 12.97±0.01 | evolution | SIMBAD | [5][6][7][8]
W51-57  | G49.5-0.4 | 160 | 1,820,000–4,786,000 | 42,700 | O4V | 20,000  |  | evolution |  | [13]
HD 15558 A  | IC 1805 | ≥152±51 | 661,000 |  | O5.5III(f)  | 24,400  | 7.87
combined  | binary | SIMBAD | [14][15]
W51-3  | G49.5-0.4 | 148+105
−82 | 1,349,000+626,000
−437,000–3,890,000+4,238,000
−2,028,000 | 39,800 | O3V–O8V  | 20,000  |  | evolution | SIMBAD | [13]
Melnick 34 A  | R136 | 147±22 | 2,692,000+544,000
−453,000 | 53,000±1,200 | WN5h  | 163,000  | 13.10
combined  | mass-luminosity relation | SIMBAD | [16][12]
VFTS 1022  | R136 | 142.8+25.6
−25.2 | 3,020,000+782,000
−621,000 | 42,170±1,520 | O3.5If*/WN7 | 164,000  | 13.44 | evolution | SIMBAD | [17]
R136c | R136 | 142.0+32.7
−24.7 | 3,802,000+1,568,000
−1,110,000 | 42,170±1,890 | WN5h  | 163,000  | 12.86 | evolution | SIMBAD | [17][12][lower-alpha 5]
LH 10-3209 A  | NGC 1763 | 140 | 2,312,000 | 50,900 | O3III(f*)  | 160,000  | 12.73 | evolution | SIMBAD | [18][19][20][lower-alpha 5]
VFTS 682 | Runaway from R136 | 137.8+27.5
−15.9 | 3,236,000+838,000
−666,000 | 54,450±1,960 | WN5h  | 164,000  | 16.08 | evolution | SIMBAD | [17]
VFTS 506  | NGC 2070 | 136.8±24.2 | 2,692,000 | 55,000 | ON2V((n))((f*))  | 164,000  | 13.31 | evolution | SIMBAD | [21]
Melnick 34 B  | R136 | 136±20 | 2,344,000+474,000
−394,000 | 53,000±1,200 | WN5h  | 163,000  | 13.10
combined  | mass-luminosity relation | SIMBAD | [16][12]
W51d  | G49.5-0.4 | 135 | 1,288,000–2,884,000 | 42,700 | O3V–O4V  | 20,000  |  | evolution |  | [13]
NGC 3603-B | HD 97950 | 132±13 | 2,884,000+504,000
−429,000 | 42,000±2,000 | WN6h  | 24,800  | 11.33 | evolution | SIMBAD | [22][23]
HD 269810 | NGC 2029 | 130 | 2,188,000 | 52,500 | O2III(f*)  | 163,000  | 12.22 | spectroscopy | SIMBAD
W49-1  | W49 cluster 1 | 130±30 | 1,905,000+786,000
−556,000 | 44,700+2,100
−2,000 | O2–3.5If*  | 36,200  |  | evolution | SIMBAD | [9]
R136a7 | R136 | 127+15
−16 | 2,291,000+280,000
−341,000 | 54,000+2,000
−3,000 | O3III(f*)  | 163,000  | 13.97±0.01 | evolution | SIMBAD | [7][12][8]
WR 42e | Runaway from HD 97950 | 123 | 3,200,000 | 43,700 | O3If*/WN6  | 25,000  | 14.529 | evolution | SIMBAD | [24][25]
Sk -69° 249 A  | NGC 2074 | 119 | 4,130,000 | 38,900 | O7If  | 160,000  | 12.02±0.21 | evolution | SIMBAD | [26][27]
Sk -69° 212  | NGC 2044  | 119 | 2,377,000 | 45,400 | O5III(f)  | 160,000  | 12.416±0.0600 | evolution | SIMBAD
ST5-31  | NGC 2074 | 119 | 2,168,000 | 50,700 | O3If*  | 160,000  | 12.273±0.084 | evolution | SIMBAD | [26][28]
R136a5 | R136 | 116+6
−5 | 2,089,000+149,000
−139,000 | 48,000±750 | O2I(n)f*  | 157,000  | 13.71±0.01 | evolution | SIMBAD | [7][12][8]
MSP 183  | Wd2 | 115 | 724,000 | 49,000±3,000 | O3V((f))  | 20,000  | 13.878±0.017 | spectroscopy | SIMBAD | [29][30]
WR 24 | Collinder 228 | 114 | 2,951,000 | 50,100 | WN6ha-w  | 14,000  | 6.48 | evolution | SIMBAD | [31][32]
NGC 3603-C1  | HD 97950 | 113+11
−8 | 2,239,000+392,000
−333,000 | 44,000±2,000 | WN6h  | 24,800  | 11.89
combined  | evolution | SIMBAD | [22][23][lower-alpha 5]
Arches-F9  |  Arches Cluster | 111.3 | 2,239,000 | 36,800 | WN8-9h  | 25,000  |  | wind | SIMBAD | [33][34][35]
VFTS 545  | R136 | 110.4+18.9
−16.6 | 1,995,000+516,000
−410,000 | 47,320±1,700 | O2If*/WN5  | 164,000  | 13.40 | evolution | SIMBAD | [17][12]
HSH95-36  | R136 | 110±5 | 1,862,000+133,000
−124,000 | 49,500+750
−1,000 | O2If*  | 163,000  | 14.41±0.01 | evolution | SIMBAD | [7][12][8]
Cygnus OB2 #12 A  | Cygnus OB2 | 110 | 1,660,000 | 13,700 | B3–4Ia+ | 5,200  | 11.702
combined  | spectroscopy | SIMBAD | [36][37][lower-alpha 5]
Melnick 39 A  | R136 | 109±7 | 1,585,000+654,000
−463,000 | 44,000±2,500 | O3If*/WN6-A  | 160,000  | 13.0
combined  | binary | SIMBAD | [38]
R136a4 | R136 | 108+6
−7 | 1,905,000+90,000
−207,000 | 50,000+500
−2,000 | O3V((f*))(n)  | 157,000  | 13.96±0.01 | evolution | SIMBAD | [7][12][8]
VFTS 621  | NGC 2070 | 107 | 1,380,000 | 50,100 | O2V((f*))z  | 164,000  | 15.39 | mass-luminosity relation | SIMBAD | [11][12]
W49-3  | W49 CC | 105±20 | 1,514,000+528,000
−392,000 | 40,700+5,000
−4,400 | O3–O7V  | 36,200  |  | evolution | SIMBAD | [9][10]
R99 | LH 49  | 103 | 3,162,000 | 28,000 | Ofpe/WN9  | 164,000  | 11.520±0.049 | mass-luminosity relation | SIMBAD | [39][15]
Arches-F6  | Arches Cluster | 101.0 | 2,089,000+255,000
−227,000 | 33,300±1,300 | WN8-9ha  | 25,000  |  | wind | SIMBAD | [33][40]
Arches-F1  | Arches Cluster | 100.9 | 1,995,000 | 33,700 | WN8-9h  | 25,000  |  | wind | SIMBAD | [33][34][35]
Peony Star | near Galactic Center | 100 | 2,951,000+1,217,000
−862,000 | 25,100 | WN10  | 26,000  |  | evolution | SIMBAD | [41][10]
HD 93129 Aa  | Trumpler 14 | 100+25
−60 | 1,413,000+172,000
−154,000 | 52,000±3,000 | O2If*  | 7,500  | 7.310±0.011
combined  | spectroscopy | SIMBAD | [42][15]
Mc30-1 A  | Mercer 30  | 99 | 3,236,000 | 32,200 | O6–7.5If+  | 40,000  |  | evolution | SIMBAD | [43][lower-alpha 6][lower-alpha 5]
VFTS 1028  | R136 | 99 | 1,230,000 | 47,300 | O3III(f*) or O4–5V  | 164,000  | 13.82 | mass-luminosity relation | SIMBAD | [11]
WR 25 A  | Trumpler 16 | 98 | 2,399,000 | 50,100 | WN6h-w  | 6,500  | 8.80
combined  | evolution | SIMBAD | [31][15][lower-alpha 5]
BI 253 |  Runaway from R136 | 97.6+22.2
−23.1 | 1,175,000+410,000
−304,000 | 54,000±1,500 | O2V-III(n)((f*))  | 164,000  | 13.669±0.062 | evolution | SIMBAD | [17][44]
R136a8 | R136 | 96±6 | 1,479,000+106,000
−99,000 | 49,500±1,250 | O2–3V  | 157,000  | 14.42±0.01 | evolution | SIMBAD
W49-15  | W49 cluster 1 | 96±14 | 1,288,000+334,000
−265,000 | 43,700±1,000 | O2–3.5If*  | 36,200  |  | evolution | SIMBAD | [9]
HM 1-6  | HM 1 | 95 | 1,500,000 | 44,800 | O5If  | 11,000  | 11.64 | evolution | SIMBAD
NGC 3603-42  | HD 97950 | 95 | 946,000 | 46,500 | O3III(f*)  | 25,000  | 12.86 | evolution | SIMBAD | [18][23]
ST2-22  | NGC 2044  | 94 | 1,247,000 | 51,300 | O3V((f))  | 160,000  | 14.3 | evolution | SIMBAD | [26][45]
VFTS 562  | NGC 2070 | 94 | 1,122,000 | 42,200 | O4V  | 164,000  | 13.66 | mass-luminosity relation | SIMBAD | [11][12]
NGC 3603-A1a | HD 97950 | 93.3±11.0 | 1,000,000 | 37,000 | O3If*/WN6  | 24,800  | 11.18
combined  | eclipsing binary | SIMBAD | [46][22][23]
WR 21a A  |  Runaway from Wd2 | 93.2+2.2
−1.9 | 1,514,000+224,000
−195,000 | 42,000 | O2.5If*/WN6ha  | 26,100  | 12.661±0.03 combined  | eclipsing binary | SIMBAD | [47][48]
HD 303308 | Trumpler 16 | 93 | 1,138,000 | 51,300 | O3V  | 9,200  | 8.17 | evolution | SIMBAD | [49][48]
VFTS 512  | NGC 2070 | 93 | 1,096,000 | 47,300 | O2V-III((f*))  | 164,000  | 14.28 | mass-luminosity relation | SIMBAD | [11][12]
R136b | R136 | 92±5 | 2,239,000+160,000
−149,000 | 35,500±750 | O4If  | 163,000  | 13.24±0.01 | evolution | SIMBAD | [7][12][8]
VFTS 16 | Runaway from R136 | 91.6+11.5
−10.5 | 1,318,000+341,000
−271,000 | 50,600+500
−590 | O2III-If*  | 164,000  | 13.546±0.010 | evolution | SIMBAD | [17][12]
NGC 346-W1  | NGC 346 | 91 | 1,500,000 | 43,400 | O5.5If  | 200,000  | 12.57 | evolution | SIMBAD | [26][50]
NGC 3603-A3  | HD 97950 | 91 | 863,000 | 46,400 | O3III(f*)  | 24,800  | 12.95 | evolution | SIMBAD | [18][23]
η Carinae A  | Trumpler 16 | 90 | 4,000,000 | 9,470 (near the top of the wind)  | LBV | 7,500  | 6.48±0.01
combined  | spectroscopy | SIMBAD | [51][52]
R146  | Runaway from R136 | 88.4+16.9
−15.8 | 1,950,000+505,000
−401,000 | 53,090±1,910 | WN5ha  | 164,000  | 13.116±0.0201 | evolution | SIMBAD | [17][12]
WR 89  | HM 1 | 87 | 2,138,000 | 39,800 | WN8h  | 11,000  | 11.02±0.01 | evolution | SIMBAD | [31][48]
Arches-F7  | Arches Cluster | 86.3 | 1,862,000+227,000
−203,000 | 33,900±1,300 | WN8-9ha  | 25,000  |  | wind | SIMBAD | [33][40]
R147  | Runaway from R136 | 85.6+15.2
−16.6 | 2,291,000+593,000
−471,000 | 47,320±1,700 | WN5h  | 164,000  | 12.993±0.042 | evolution | SIMBAD | [17][53]
Sk 80 | NGC 346 | 85 | 1,500,000 | 38,900 | O7If  | 200,000  | 12.31 | evolution | SIMBAD | [26][54]
BAT99-92 B  | Tarantula Nebula | 85 | 1,175,000 | 23,000 | B1Ia | 165,000  | 11.39±0.02 combined  | spectroscopy | SIMBAD | [55]
Sk -70° 91  | BSDL 1830  | 84.09 | 851,000 | 48,849 | ON2III  | 165,000  | 12.78 | evolution | SIMBAD | [56][19][lower-alpha 7]
Sk -66° 172  | LH 95 | 84.09 | 851,000 | 48,849 | O2III(f*)  | 160,000  | 13.1 | evolution | SIMBAD | [56][19]
Sk -68° 137  | Runaway from R136 | 84.09 | 851,000 | 48,849 | O2III(f*)  | 160,000  | 13.346±0.0101 | evolution | SIMBAD | [56][19]
LH 64-16  | NGC 2001 | 84.09 | 851,000 | 48849 | ON2III(f*)  | 160,000  | 13.666±0.010 | evolution | SIMBAD | [56][28]
Melnick 33Na A | R136 | 83±19 | 1,413,000+725,000
−479,000 | 50,000±2,500 | OC2.5If*  | 163,000  | 13.79
combined  | evolution | SIMBAD | [57][58]
Melnick 39 B  | R136 | 83±5 | 1,000,000+413,000
−292,000 | 48,000±2,500 | O3If*/WN6-A  | 160,000  | 13.0
combined  | binary | SIMBAD | [38]
WR 20a A  | Wd2 | 82.2±4.7 | 603,000+139,000
−113,000 | 43,000 | WN6ha  | 20,000  | 13.5
combined  | eclipsing binary | SIMBAD | [59]
Arches-F2 A  | Arches Cluster | 82±12 | 1,862,000+227,000
−203,000 | 34,100+2,000
−1,000 | WN8–9h  | 25,000  |  | eclipsing binary | SIMBAD | [60]
R139 A  | NGC 2070 | 81.6+7.5
−7.2 | 1,585,000+235,000
−205,000 | 34,000±1,100 | O6.5I  | 163,000  | 11.94
combined  | evolution | SIMBAD | [61]
WR 20a B  | Wd2 | 81.4±4.7 | 537,000+124,000
−101,000 | 41,840±250 | WN6ha  | 20,000  | 13.5
combined  | eclipsing binary | SIMBAD | [59]
Tr27-27  | Trumpler 27 | 81 | 1,247,000 | 37,200 | O8III((f))  | 3,900  | 13.31 | evolution | SIMBAD | [49][48]
HSH95-46  | R136 | 80+5
−6 | 1,259,000+59,000
−162,000 | 47,500+500
−2,500 | O2-3III(f*)  | 163,000  | 14.56±0.01 | evolution | SIMBAD | [7][12]
Arches-F15  | Arches Cluster | 79.7 | 794,000+118,000
−102,000 | 32,000±1,500 | O6–7Ia+  | 25,000  |  | wind | SIMBAD | [33][40]
BI 237  | BSDL 2527  | 79.66 | 661,000 | 51,269 | O2V((f*))  | 165,000  | 13.830±0.0431 | spectroscopy | SIMBAD | [56][19][lower-alpha 8]
VFTS 1017  | R136 | 79.0+17.8
−15.9 | 1,622,000+420,000
−334,000 | 50,120±1,800 | O2If*/WN5  | 164,000  | 14.50 | evolution | SIMBAD | [17][12]
VFTS 151  | TLD1  | 79 | 1,072,000 | 42,200 | O6.5II(f)p  | 164,000  |  | mass-luminosity relation | SIMBAD | [11][12]
VFTS 94  | NGC 2060 | 79 | 955,000 | 42,200 | O3.5Inf*p  | 164,000  | 14.161±0.0271 | mass-luminosity relation | SIMBAD | [11][19]
VFTS 1018  | R136 | 79 | 832,000 | 42,200 | O3III(f*)  | 163,000  | 14.34 | mass-luminosity relation | SIMBAD | [11]
LH 41-32  | NGC 1910 | 78 | 946,000 | 48,200 | O4III  | 160,000  | 13.086±0.0101 | evolution | SIMBAD | [26][19]
Pismis 24-17  | Pismis 24 | 78 | 851,000 |  | O3.5III  | 5,900  | 11.84 | spectroscopy | SIMBAD | [62][63]
LSS 4067 | HM 1 | 77 | 794,000+118,000
−102,000 | 40,000±2,000 | O4If  | 11,000  | 11.26±0.07 | evolution | SIMBAD | [64][65][66]
W51-2  | G49.2-0.3 | 77+26
−22 | 724000+167000
−136000–1288000+617000
−417000 | 42,700+2,000
−1,900 | O3V–O5V  | 20,000  |  | evolution | SIMBAD | [13]
R139 B  | NGC 2070 | 76.4+7.1
−6.7 | 1,445,000+214,000
−187,000 | 34,700±1,100 | O7I  | 163,000  | 11.94
combined  | evolution | SIMBAD | [61]
NGC 346-W3  | NGC 346 | 76 | 813,000+99,000
−88,000 | 51,300 | O2III(f*)  | 200,000  | 12.80±0.04 | evolution | SIMBAD | [26][50][67]
BAT99-68  | NGC 2044  | 76 | 1,000,000 | 45,000 | O3If*/WN7  | 165,000  | 14.13 | mass-luminosity relation | SIMBAD | [39][19]
HD 93632 | Collinder 228 | 76 | 946,000 | 45,400 | O5III(f)  | 10,000  | 9.10 | evolution | SIMBAD | [49][15]
AB1  | DEM S10  | 75 | 1,175,000 | 79,000 | WN3ha  | 197,000  | 15.24±0.02 | spectroscopy | SIMBAD | [68][50][lower-alpha 9]
VFTS 457  | NGC 2070 | 74.6+20.1
−9.2 | 1,585,000+410,000
−326,000 | 39,810±1,430 | O3.5If*/WN7  | 164,000  | 13.74 | evolution | SIMBAD | [17][12]
HD 38282 A  | Runaway from R136 | 74±4 | 2,754,000+336,000
−300,000 | 50,000±2,000 | WN5/6h  | 163,000  | 11.11±0.03
combined  | binary | SIMBAD | [69][48]
BAT99-6 A  | NGC 1747  | 74 | 794,000 | 45,000 | O3If*/WN7  | 165,000  | 11.95 combined  | spectroscopy | SIMBAD | [55]
VFTS 608  | NGC 2070 | 74 | 724,000 | 42,200 | O4III(f)  | 164,000  | 14.22 | mass-luminosity relation | SIMBAD | [11][12]
HSH95-31  | R136 | 73±3 | 955,000+68,000
−64,000 | 47,500+1,000
−750 | O2V((f*))  | 163,000  | 14.35 | evolution | SIMBAD | [7][12]
Mc30-11  | Mercer 30  | 73 | 741,000 | 36,800 | O5.5-6I-II  | 40,000  |  | spectroscopy | SIMBAD | [43][lower-alpha 6]
Mc30-3  | Mercer 30  | 73 | 676,000 | 39,300 | O6If  | 40,000  |  | spectroscopy | SIMBAD | [43][lower-alpha 6]
VFTS 599  | NGC 2070 | 72.0+9.2
−7.4 | 1,023,000+265,000
−210,000 | 47,300+820
−500 | O3III(f*)  | 164,000  | 13.80 | evolution | SIMBAD | [17][12]
NGC 2044-W35  | NGC 2044  | 72 | 863,000 | 48,200 | O4III  | 160,000  | 14.10 | evolution | SIMBAD | [26][19]
VFTS 542  | R136 | 71.4+16.3
−11.3 | 1,445,000+374,000
−297,000 | 44,670±2,010 | O2If*/WN5  | 164,000  | 13.47 | evolution | SIMBAD | [17][12]
VFTS 1021  | R136 | 71.4+12.7
−9.2 | 1,259,000+326,000
−259,000 | 35,500±1,500 | O4If+  | 164,000  | 13.31 | evolution | SIMBAD | [17]
ST2-1  | NGC 2044  | 71 | 946,000 | 44,100 | O5.5III  | 160,000  | 14.3 | evolution | SIMBAD | [26][45]
NGC 3603-A1b | HD 97950 | 70.4±9.3 | 1,000,000 | 42,000 | O3If*/WN5  | 24,800  | 11.18
combined  | eclipsing binary | SIMBAD | [46][22][23]
Arches-F12  | Arches Cluster | 70.0 | 1,585,000 | 37,300 | WN7–8h  | 25,000  |  | wind | SIMBAD | [33][34][35]
HD 37974 | NGC 2050  | 70 | 1,400,000 | 22,500 | B0.5Ia+  | 163,000  | 10.99±0.03 | spectroscopy | SIMBAD | [70][48]
M33 X-7 B  | Triangulum Galaxy | 70.0±6.9 | 525,000+92,000
−78,000 | 34,000–36,000 | O7III–O8III  | 2,700,000  | 18.70 | binary | SIMBAD | [71][72]
QZ Carinae Aa1  | Collinder 228 | 69.8±5 | 398,000 | 29,564±1,000 | O9.7I  | 9,200  | 6.24 combined  | quaternary | SIMBAD | [73][74]
VFTS 125  | NGC 2060 | 69.6+22.3
−17.2 | 794,000+496,000
−281,000 | 55,150±5,520 | Ope  | 164,000  | 16.6 | evolution | SIMBAD | [17][45]
HD 38282 B  | Runaway from R136 | 69±4 | 2,455,000+300,000
−267,000 | 45,000±2,000 | WN6/7h  | 163,000  | 11.11±0.03
combined  | binary | SIMBAD | [69][48]
HD 229059 | Berkeley 87 | 69 | 1,038,000 | 26,300 | B1Ia  | 3,000  | 8.70 | evolution | SIMBAD | [49][15]
ST2-32  | NGC 2044  | 69 | 863,000 | 45,400 | O5III  | 160,000  | 13.903±0.0921 | evolution | SIMBAD | [26][19]
ST2-3  | NGC 2044  | 69 | 863,000 | 44,100 | O5.5V  | 160,000  | 14.264±0.1241 | evolution | SIMBAD | [26][19]
W28-23  | NGC 2033  | 69 | 655,000 | 51,300 | O3V  | 160,000  | 13.702±0.050 | evolution | SIMBAD | [26][28]
HD 46150  | NGC 2244 | 69 | 447,000+129,000
−100,000 | 42,500+2,100
−2,000 | O5V((f))z  | 5,200  | 6.73 | evolution | SIMBAD | [18][75][76]
HD 93403 A  | Carina OB1 | 68.5+12.3
−14.6 | 1,047,000+49,000
−47,000 | 39,300±1,100 | O5.5I  | 10,400  | 8.27±0.74
combined  | evolution | SIMBAD | [77][48]
HSH95-47  | R136 | 68±4 | 955,000+117,000
−64,000 | 43,500+1,750
−1,000 | O2V((f*))  | 163,000  | 14.72±0.01 | evolution | SIMBAD | [7][12][8]
HSH95-48  | R136 | 68±4 | 912,000+65,000
−80,000 | 46,500+1,000
−1,500 | O2–3III(f*)  | 163,000  | 14.75±0.01 | evolution | SIMBAD | [7][8]
HD 93130 | Collinder 228 | 68 | 863,000 | 39,900 | O7II(f)  | 10,000  | 8.04 | evolution | SIMBAD | [49][15]
W51-61  | G49.5-0.4 | 68 | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O7.5V  | 20,000  |  | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [13][10]
Sk -69° 200  | NGC 2033 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | B1I  | 160,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [26][19]
Arches-F18  | Arches Cluster Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O4–5Ia+  | 25,000  |  | windLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [33][34][35]
Arches-F4  | Arches Cluster Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | WN7–8h  | 25,000  |  | windLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [33][34][35]
Z15  | Messier 81Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | B0.5  | 11,986,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [78]
HD 5980 B  | NGC 346 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | WN6−7  | 200,000  | Lua error: Internal error: The interpreter has terminated with signal "24".
combined Lua error: Internal error: The interpreter has terminated with signal "24". | binaryLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [79][80]
Sk -67° 108  | LMC Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O5III(f)  | 164,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [81]
HD 190429 A  | near Barnard 146 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O4If  | 7,800  | Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [82][15]
LH 31-1003  | NGC 1858 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O6Ib(f)  | 160,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [26][19]
VFTS 169  | NGC 2060 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O2.5V(n)((f*))  | 164,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [17][19]
Pismis 24-1SW  | Pismis 24 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". |  | O4III  | 6,500  |  | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [62][83]
HSH95-89  | R136 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O4V  | 163,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [8]
HSH95-40  | R136 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O3V  | 163,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [7][12]
HSH95-58  | R136 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O2–3V  | 163,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [7][12][8]
VFTS 145  | TLD1 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O8fp  | 164,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | mass-luminosity relationLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [11][12]
VFTS 518  | NGC 2070 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O3.5III(f*)  | 164,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | mass-luminosity relationLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [11][12]
W49-8  | W49 CCLua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O3–O7V  | 36,200  |  | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [9][10]
BD+43° 3654 | Runaway from Cygnus OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O6If+  | 5,400  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [84][85]
Sk -70° 115  | NGC 2122 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O6.5Ifc  | 164,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [81]
Sk -69° 25  | NGC 1748 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O6V((f))  | 160,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [26][19]
HSH95-50  | R136 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O3–4V((f*))  | 163,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [7][12][8]
W49-5  | W49 cluster 1Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O3–O5V  | 36,200  |  | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [9][10]
ST5-71  | NGC 2074 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O5III  | 160,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [26][19]
VFTS 259  | Tarantula Nebula Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O6Iaf  | 164,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [17][12]
Mc30-6a A  | Mercer 30 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Ofpe/WN9  | 40,000  |  | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [43][lower-alpha 6][lower-alpha 5]
AB9  | DEM S80 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | WN3ha  | 197,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [68][50][lower-alpha 10]
LH 41-1017  | NGC 1910 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | B1  | 160,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [26][19]
Brey 32 B  | NGC 1966 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O6.5V  | 165,000  | Lua error: Internal error: The interpreter has terminated with signal "24".
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [26][48]
HD 93160 | Trumpler 14 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O6III  | 8,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [49][15]
HSH95-35  | R136 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O3V  | 163,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [7][12][8]
HD 229196 | Cygnus OB9 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". |  | Lua error: Internal error: The interpreter has terminated with signal "24". | O5  | 5,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [84][63]
HD 5980 A  | NGC 346 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | WN6h  | 200,000  | Lua error: Internal error: The interpreter has terminated with signal "24".
combined Lua error: Internal error: The interpreter has terminated with signal "24". | binaryLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [79][80]
WR 102hb | Quintuplet cluster Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | WN9h  | 26,000  |  | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [86][87]
VFTS 267  | Tarantula Nebula Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O3.5III(f*)  | 164,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [81]
LH 41-18  | NGC 1910 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O8.5V((f))  | 160,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [26][19]
AB8 B  | NGC 602c Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O4V  | 197,000  | Lua error: Internal error: The interpreter has terminated with signal "24".
combined Lua error: Internal error: The interpreter has terminated with signal "24". | binaryLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [79][88]
Mc30-9 A  | Mercer 30 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O6-7I-III  | 40,000  |  | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [43][lower-alpha 6][lower-alpha 5]
ST5-25  | NGC 2074 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O4V  | 160,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [26][28]
VFTS 422  | NGC 2070 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O4III(f)  | 164,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | mass-luminosity relationLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [11][12]
Sk -67° 166  | NGC 2014 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O4If+  | 160,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [56][19]
Sk -65° 47  | NGC 1923 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O4If  | 160,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [56][19]
Mc30-7 A  | Mercer 30 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | WN6  | 40,000  |  | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [43][lower-alpha 6][lower-alpha 5]
BAT99-96  | NGC 2070 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | WN8(h)  | 164,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [17]
Arches-F2 B  | Arches Cluster Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O5–6Ia+  | 25,000  |  | eclipsing binaryLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [60]
HSH95-55  | R136 Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | O2V((f*))z  | 163,000  | Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [7][12][8]

A few notable large stars with masses less than 60 M☉ are shown in the table below for the purpose of comparison, ending with the Sun, which is very close, but would otherwise be too small to be included in the list. At present, all the listed stars are naked-eye visible and relatively nearby.

Star name  | Location  | Mass
(M☉, Sun = 1)Lua error: Internal error: The interpreter has terminated with signal "24". | Eff. temp.
(K)Lua error: Internal error: The interpreter has terminated with signal "24". | Approx. dist.
(ly)Lua error: Internal error: The interpreter has terminated with signal "24". | Appt. vis. mag.Lua error: Internal error: The interpreter has terminated with signal "24". | Mass est.Lua error: Internal error: The interpreter has terminated with signal "24". method  | Link  | Ref.

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|
|
|
|

λ Cephei | Runaway star from Cepheus OB3 Lua error: Internal error: The interpreter has terminated with signal "24". | 51.4  | 36,000  | 3,100  | 5.05 | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [82][15]
τ Canis Majoris Aa  | NGC 2362 Lua error: Internal error: The interpreter has terminated with signal "24". | 50  | 32,000  | 5,120  | 4.89 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [89][15]
θ Muscae Ab  | Centaurus OB1 Lua error: Internal error: The interpreter has terminated with signal "24". | 44  | 33,000  | 7,400  | 5.53
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [90][15]
θ2 Orionis A  | Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 39  | 34,900  | 1,500  | 5.02 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [91][92]
α Camelopardalis | Runaway star from NGC 1502 Lua error: Internal error: The interpreter has terminated with signal "24". | 37.6  | 29,000  | 6,000  | 4.29 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [93][15]
P Cygni | IC 4996 of Cygnus OB1 Lua error: Internal error: The interpreter has terminated with signal "24". | 37  | 18,700  | 5,100  | 4.82 | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [94][15][lower-alpha 11]
ζ1 Scorpii | NGC 6231 of Scorpius OB1 Lua error: Internal error: The interpreter has terminated with signal "24". | 36 - 53  | 17,200  | 8,210  | 4.705 | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [95][96]
ζ Orionis Aa  | Alnitak in Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 33  | 29,500  | 1,260  | 2.08 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [97]
θ1 Orionis C1  | Trapezium Cluster of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 33  | 39,000  | 1,340  | 5.13
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [98][15]
κ Cassiopeiae  | Cassiopeia OB14 Lua error: Internal error: The interpreter has terminated with signal "24". | 33  | 23,500  | 4,000  | 4.16 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [99][15]
μ Normae | NGC 6169 Lua error: Internal error: The interpreter has terminated with signal "24". | 33  | 28,000  | 3,260  | 4.91 | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [100][15]
η Carinae B  | Trumpler 16 of Carina Nebula Lua error: Internal error: The interpreter has terminated with signal "24". | 30  | 37,200  | 7,500  | 4.3
combined Lua error: Internal error: The interpreter has terminated with signal "24". | binaryLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [101][102]
γ2 Velorum B  | Vela OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 28.5  | 35,000  | 1,230  | 1.83
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [103][15]
Alnilam | ε Orionis in Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | 25,000  | 1,250  | 1.69 | spectroscopy + interferometryLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [104][15]
Meissa A  | In Collinder 69 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 27.9  | 37,700  | 1,300  | 3.54 | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [100][105]
ξ Persei | Menkib in California Nebula of Perseus OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 26.1  | 35,000  | 1,200  | 4.04 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [93][15]
ζ Puppis |  Naos in Vela R2 of Vela Molecular Ridge Lua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24". | 40,000  | 1,080  | 2.25 | empiricalLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [106][15][lower-alpha 12]
WR 79a  | NGC 6231 of Scorpius OB1 Lua error: Internal error: The interpreter has terminated with signal "24". | 24.4  | 35,000  | 5,600  | 5.77 | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [100][15]
Mintaka Aa1  | In Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 24  | 29,500  | 1,200  | 2.5
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [107][108]
ι Orionis Aa1  |  Hatysa in NGC 1980 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 23.1  | 32,500  | 1,340  | 2.77
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD
κ Crucis | Jewel Box Cluster of Centaurus OB1 Lua error: Internal error: The interpreter has terminated with signal "24". | 23  | 16,300  | 7,500  | 5.98 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [109][80]
WR 78  | NGC 6231 of Scorpius OB1 Lua error: Internal error: The interpreter has terminated with signal "24". | 22  | 50,100  | 4,100  | 6.48 | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [31][32]
ο2 Canis Majoris | Field star Lua error: Internal error: The interpreter has terminated with signal "24". | 21.4  | 15,500  | 2,800  | 3.043 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [100][15]
Rigel A  | In Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 21  | 12,100  | 860  | 0.13 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [110][15]
ζ Ophiuchi  | Upper Scorpius subgroup of Scorpius OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 20.2  | 34,000  | 370  | 2.569 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [93][15]
υ Orionis  | Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 20  | 33,400  | 2,900  | 4.618 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [111][112]
σ Orionis Aa  | Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 18  | 35,000  | 1,260  | 4.07
combined Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [113][114]
μ Columbae | Runaway star from Trapezium Cluster Lua error: Internal error: The interpreter has terminated with signal "24". | 16  | 33,000  | 1,300  | 5.18 | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [115][15]
Saiph | In Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 15.5  | 26,500  | 650  | 2.09 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [116][15]
σ Cygni | Cygnus OB4 Lua error: Internal error: The interpreter has terminated with signal "24". | 15  | 10,800  | 3,260  | 4.233 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [117][118]
θ Carinae A  | IC 2602 of Scorpius OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 14.9  | 31,000  | 460  | 2.76
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [100][119]
θ2 Orionis B  | Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 14.8  | 29,300  | 1,500  | 6.38 | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [120]
ζ Persei | Perseus OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 14.5  | 20,800  | 750  | 2.86 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [116][15]
σ Orionis B  | Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 14  | 31,000  | 1,260  | 4.07
combined Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [113][114]
β Canis Majoris  | Mirzam in Local Bubble of Scorpius OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 13.5  | 23,200  | 490  | 1.985 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [121][122]
ε Persei A  | α Persei Cluster Lua error: Internal error: The interpreter has terminated with signal "24". | 13.5  | 26,500  | 640  | 2.88
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD
ι Orionis Aa2  | NGC 1980 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 13.1  | 27,000  | 1,340  | 2.77
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [123][124]
δ Scorpii A  |  Dschubba in Upper Scorpius subgroup of Scorpius OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 13  | 27,400  | 440  | 2.307
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [125][126]
σ Orionis Ab  | Orion OB1 of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 13  | 29,000  | 1,260  | 4.07
combined Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [113][114]
θ Muscae Aa  |  WR 48 in Centaurus OB1 Lua error: Internal error: The interpreter has terminated with signal "24". | 11.5  | 83,000  | 7,400  | 5.53
combined Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [127][15]
γ2 Velorum A  | WR 11 in Vela OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 9  | 57,000  | 1,230  | 1.83
combined Lua error: Internal error: The interpreter has terminated with signal "24". | spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [103][15]
ρ Ophiuchi A  | ρ Ophiuchi cloud complex of Scorpius OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 8.7  | 22,000  | 360  | 4.63
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [100][15]
Bellatrix | In Bellatrix Cluster of Orion complex Lua error: Internal error: The interpreter has terminated with signal "24". | 7.7  | 21,800  | 250  | 1.64 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [128][15]
Antares B  | Loop I Bubble of Scorpius OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 7.2  | 18,500  | 550  | 5.5 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [129][105]
λ Tauri A  | Pisces-Eridanus stellar stream Lua error: Internal error: The interpreter has terminated with signal "24". | 7.18  | 18,700  | 480  | 3.47
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [130][131]
δ Persei | α Persei Cluster Lua error: Internal error: The interpreter has terminated with signal "24". | 7  | 14,900  | 520  | 3.01 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [100][119]
ψ Persei | α Persei Cluster Lua error: Internal error: The interpreter has terminated with signal "24". | 6.2  | 16,000  | 580  | 4.31 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [100][15]
α Pavonis Aa  |  Peacock in Tucana-Horologium association Lua error: Internal error: The interpreter has terminated with signal "24". | 5.91  | 17,700  | 180  | 1.94 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [132][124]
Alcyone | In Pleiades Lua error: Internal error: The interpreter has terminated with signal "24". | 5.9  | 12,300  | 440  | 2.87
combined Lua error: Internal error: The interpreter has terminated with signal "24". | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [133][15]
γ Canis Majoris | Muliphein in Collinder 121 Lua error: Internal error: The interpreter has terminated with signal "24". | 5.6  | 13,600  | 440  | 4.1 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [100][134]
η Canis Majoris  | Aludra in Collinder 121 Lua error: Internal error: The interpreter has terminated with signal "24". | 5.5 or 9.5  | 15,000  | 2,000  | 2.45 | SED modelling / spectroscopyLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [135][15]
ο Velorum  | IC 2391 of Scorpius OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 5.5  | 16,200  | 490  | 3.6 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [136][119]
ο Aquarii  | Pisces-Eridanus stellar stream Lua error: Internal error: The interpreter has terminated with signal "24". | 4.2  | 13,500  | 440  | 4.71 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [137][138]
ν Fornacis | Pisces-Eridanus stellar stream Lua error: Internal error: The interpreter has terminated with signal "24". | 3.65  | 13,400  | 370  | 4.69 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [139][15]
φ Eridani | Tucana-Horologium association Lua error: Internal error: The interpreter has terminated with signal "24". | 3.55  | 13,700  | 150  | 3.55 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [132][140]
η Chamaeleontis  | η Chamaeleontis moving group of Scorpius OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 3.2  | 12,500  | 310  | 5.453 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [141][80]
ε Chamaeleontis  | ε Chamaeleontis moving group of Scorpius OB2 Lua error: Internal error: The interpreter has terminated with signal "24". | 2.87  | 10,900  | 360  | 4.91 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [142][119]
τ1 Aquarii | Pisces-Eridanus stellar stream Lua error: Internal error: The interpreter has terminated with signal "24". | 2.68  | 10,600  | 320  | 5.66 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [143][144]
ε Hydri | Tucana-Horologium association Lua error: Internal error: The interpreter has terminated with signal "24". | 2.64  | 11,000  | 150  | 4.12 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [143][145]
β1 Tucanae | Tucana-Horologium association Lua error: Internal error: The interpreter has terminated with signal "24". | 2.5  | 10,600  | 140  | 4.37 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [100][105]
Sirius A |  ~11 th nearest star Lua error: Internal error: The interpreter has terminated with signal "24". | 2.06  | 9,850  | 8.6  | −1.46 | evolutionLua error: Internal error: The interpreter has terminated with signal "24". | SIMBAD | [146][147]
Sun | Solar System Lua error: Internal error: The interpreter has terminated with signal "24". | 1  | 5,772  | 0.0000158  | −26.744 | standardLua error: Internal error: The interpreter has terminated with signal "24". | Lua error: Internal error: The interpreter has terminated with signal "24".Lua error: Internal error: The interpreter has terminated with signal "24". | [148][149][150]

1. ↑ For methods that involve modelling the a star's internal dynamics, different chemical composition indicates a different estimate for stellar mass for any one measured temperature and / or brightness.
2. ↑ For a binary star, it is possible to measure the individual masses of the two stars by studying their orbital motions, using Kepler's laws of planetary motion.
3. ↑ The superwinds from massive stars are similar to the superwinds generated by asymptotic giant branch (AGB) stars – red giants – that form planetary nebulae. These stars' later remnants become the (technically non-stellar) white dwarf cores of planetary nebulae.
4. ↑ For examples of stellar debris see hypernovae and supernova remnant.
5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 5.8 This is a binary system but the secondary is much less massive than the primary.
6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Mercer 30 is an open cluster in Dragonfish Nebula.
7. ↑ BSDL 1830 is a star cluster in Large Magellanic Cloud.
8. ↑ BSDL 2527 is a star cluster in Large Magellanic Cloud.
9. ↑ DEM S10 is a H II region in Small Magellanic Cloud.
10. ↑ DEM S80 is a H II region in Small Magellanic Cloud.
11. ↑ IC 4996 is an open cluster in Cygnus OB1.
12. ↑ Vela R2 is a OB association in Vela Molecular Ridge.

Lua error: Internal error: The interpreter has terminated with signal "24".

## Black holes

Lua error: Internal error: The interpreter has terminated with signal "24".

Black holes are the end point of the evolution of massive stars.[upper-alpha 1] Technically they are not stars, as they no longer generate heat and light via nuclear fusion in their cores. Some black holes may have cosmological origins, and would then never have been stars. This is thought to be especially likely in the cases of the most massive black holes.

* Stellar black holes are objects with approximately 4–15 M☉ .
* Intermediate-mass black holes range from 100 to Lua error: Internal error: The interpreter has terminated with signal "24". M☉ .
* Supermassive black holes are in the range of millions or billions M☉.

## See also

* Hypergiant
* List of brightest stars
* List of brown dwarfs
* List of galaxies
* List of hottest stars
* List of largest cosmic structures
* List of largest nebulae
* List of largest stars
* List of most luminous stars
* List of most massive black holes
* List of most massive neutron stars
* List of most massive star clusters
* Lists of stars
* Luminous blue variable
* Supergiant
* Supernova impostor
* Wolf–Rayet star

Lua error: Internal error: The interpreter has terminated with signal "24".Lua error: Internal error: The interpreter has terminated with signal "24".

## Footnotes

Lua error: Internal error: The interpreter has terminated with signal "24".

1. ↑ A very few low / no metallicity stars (populations II and III) between 140–250 M☉ end their lives by a type II-P supernova explosion, which is powerful enough to blow (almost) all matter away from the vicinity of the star, so that not enough material remains to create either a black hole, or a neutron star, or a white dwarf: There is no central remnant; all that remains is an expanding shell of shocked gas from the SN explosion colliding with previously quiescent material ejected before the core collapse explosion.

Lua error: Internal error: The interpreter has terminated with signal "24".

## References

1. ↑ van Marle, A.J.; Owocki, S.P.; Shaviv, N.J. (March 2008). "Continuum-driven winds from super-Eddington stars: A tale of two limits". First Stars III. 990. Santa Fe, NM. pp. 250–253. doi:10.1063/1.2905555. Bibcode: 2008AIPC..990..250V.
2. ↑ Maeder, A.; Georgy, C.; Meynet, G.; Ekström, S. (March 2012). "On the Eddington limit and Wolf-Rayet stars". Astronomy & Astrophysics 539: A110. doi:10.1051/0004-6361/201118328. ISSN 0004-6361. Bibcode: 2012A&A...539A.110M.
3. ↑ Banerjee, Sambaran; Kroupa, Pavel; Oh, Seungkyung (21 October 2012). "The emergence of super-canonical stars in R136-type starburst clusters: Super-canonical stars in R136" (in en). Monthly Notices of the Royal Astronomical Society 426 (2): 1416–1426. doi:10.1111/j.1365-2966.2012.21672.x. ISSN 0035-8711. Bibcode: 2012MNRAS.426.1416B.
4. ↑ Ulmer, Andrew; Fitzpatrick, Edward L. (September 1998). "Revisiting the modified Eddington limit for massive stars" (in en). The Astrophysical Journal 504 (1): 200–206. doi:10.1086/306048. ISSN 0004-637X. Bibcode: 1998ApJ...504..200U.
5. ↑ 5.0 5.1 5.2 Keszthelyi, Z.; Brands, S. A.; de Koter, A.; Langer, N.; Puls, J. (2025-06-18). "Evolutionary models for the Very Massive Stars in the R136 cluster of 30 Doradus in the Large Magellanic Cloud". Astronomy and Astrophysics 700: A186. doi:10.1051/0004-6361/202554758. Bibcode: 2025A&A...700A.186K.
6. ↑ 6.0 6.1 6.2 Bestenlehner, Joachim M.; Crowther, Paul A.; Caballero-Nieves, Saida M.; Schneider, Fabian R.N.; Simón-Díaz, Sergio; Brands, Sarah A.; de Koter, Alex; Gräfener, Götz et al. (2020-12-01). "The R136 star cluster dissected with Hubble Space Telescope / STIS - II. Physical properties of the most massive stars in R136". Monthly Notices of the Royal Astronomical Society 499 (2): 1918–1936. doi:10.1093/mnras/staa2801. ISSN 0035-8711. Bibcode: 2020MNRAS.499.1918B.
7. ↑ 7.00 7.01 7.02 7.03 7.04 7.05 7.06 7.07 7.08 7.09 7.10 7.11 7.12 7.13 7.14 7.15 7.16 Brands, S.; de Koter, A.; Bestenlehner, J.; Crowther, P.; Sundqvist, J.; Puls, J. et al. (7 April 2022). "The R136 star cluster dissected with Hubble Space Telescope/STIS. III. The most massive stars and their clumped winds". Astronomy & Astrophysics 663: A36. doi:10.1051/0004-6361/202142742. ISSN 0004-6361. Bibcode: 2022A&A...663A..36B.
8. ↑ 8.00 8.01 8.02 8.03 8.04 8.05 8.06 8.07 8.08 8.09 8.10 8.11 8.12 8.13 8.14 Cite error: Invalid `<ref>` tag; no text was provided for refs named `crowther2016`
9. ↑ 9.0 9.1 9.2 9.3 9.4 9.5 Wu, Shi-Wei; Bik, Arjan; Bestenlehner, Joachim M.; Henning, Thomas; Pasquali, Anna; Brandner, Wolfgang; Stolte, Andrea (May 2016). "The massive stellar population of W49: A spectroscopic survey". Astronomy & Astrophysics 589: A16. doi:10.1051/0004-6361/201527823. ISSN 0004-6361. Bibcode: 2016A&A...589A..16W.
10. ↑ 10.0 10.1 10.2 10.3 10.4 10.5 Cutri, Roc M.; Skrutskie, Michael F.; van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas et al. (2003). ﻿VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)﻿ (Report). Collection of Electronic Catalogues. 2246. CDS/ADC. p. II/246. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246.
11. ↑ 11.00 11.01 11.02 11.03 11.04 11.05 11.06 11.07 11.08 11.09 11.10 11.11 Bestenlehner, J.M.; Gräfener, G.; Vink, J.S.; Najarro, F.; de Koter, A.; Sana, H. et al. (October 2014). "The VLT-FLAMES Tarantula Survey: XVII. Physical and wind properties of massive stars at the top of the main sequence". Astronomy & Astrophysics 570: A38. doi:10.1051/0004-6361/201423643. ISSN 0004-6361. Bibcode: 2014A&A...570A..38B.
12. ↑ 12.00 12.01 12.02 12.03 12.04 12.05 12.06 12.07 12.08 12.09 12.10 12.11 12.12 12.13 12.14 12.15 12.16 12.17 12.18 12.19 12.20 12.21 12.22 12.23 12.24 12.25 12.26 12.27 12.28 12.29 12.30 12.31 12.32 Cite error: Invalid `<ref>` tag; no text was provided for refs named `Doran2013`
13. ↑ 13.0 13.1 13.2 13.3 13.4 Bik, A.; Henning, Th.; Wu, S.-W.; Zhang, M.; Brandner, W.; Pasquali, A.; Stolte, A. (April 2019). "Near-infrared spectroscopy of the massive stellar population of W51: evidence for multi-seeded star formation". Astronomy & Astrophysics 624: A63. doi:10.1051/0004-6361/201935061. ISSN 0004-6361. Bibcode: 2019A&A...624A..63B.
14. ↑ De Becker, M.; Rauw, G.; Manfroid, J.; Eenens, P. (September 2006). "Early-type stars in the young open cluster IC 1805: II. The probably single stars HD 15570 and HD 15629, and the massive binary/triple system HD 15558". Astronomy & Astrophysics 456 (3): 1121–1130. doi:10.1051/0004-6361:20065300. ISSN 0004-6361. Bibcode: 2006A&A...456.1121D.
15. ↑ 15.00 15.01 15.02 15.03 15.04 15.05 15.06 15.07 15.08 15.09 15.10 15.11 15.12 15.13 15.14 15.15 15.16 15.17 15.18 15.19 15.20 15.21 15.22 15.23 15.24 15.25 15.26 15.27 15.28 15.29 15.30 15.31 15.32 15.33 15.34 15.35 Ducati, J.R. (2002). ﻿VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system﻿ (Report). Collection of Electronic Catalogues. 2237. CDS/ADC.
16. ↑ 16.0 16.1 Tehrani, Katie A.; Crowther, Paul A.; Bestenlehner, Joachim M.; Littlefair, Stuart P.; Pollock, A.M.T.; Parker, Richard J.; Schnurr, Olivier (1 April 2019). "Weighing Melnick 34: the most massive binary system known" (in en). Monthly Notices of the Royal Astronomical Society 484 (2): 2692–2710. doi:10.1093/mnras/stz147. ISSN 0035-8711. Bibcode: 2019MNRAS.484.2692T.
17. ↑ 17.00 17.01 17.02 17.03 17.04 17.05 17.06 17.07 17.08 17.09 17.10 17.11 17.12 17.13 17.14 17.15 17.16 Schneider, F.R.N.; Sana, H.; Evans, C.J.; Bestenlehner, J.M.; Castro, N.; Fossati, L. et al. (5 January 2018). "An excess of massive stars in the local 30 Doradus starburst" (in en). Science 359 (6371): 69–71. doi:10.1126/science.aan0106. ISSN 0036-8075. PMID 29302009. Bibcode: 2018Sci...359...69S.
18. ↑ 18.0 18.1 18.2 18.3 Walborn, Nolan R.; Howarth, Ian D.; Lennon, Daniel J.; Massey, Philip; Oey, M. S.; Moffat, Anthony F. J. et al. (May 2002). "A New Spectral Classification System for the Earliest O Stars: Definition of Type O2". The Astronomical Journal 123 (5): 2754–2771. doi:10.1086/339831. ISSN 0004-6256. Bibcode: 2002AJ....123.2754W.
19. ↑ 19.00 19.01 19.02 19.03 19.04 19.05 19.06 19.07 19.08 19.09 19.10 19.11 19.12 19.13 19.14 19.15 19.16 19.17 19.18 19.19 Bonanos, A.Z.; Massa, D.L.; Sewilo, M.; Lennon, D.J.; Panagia, N.; Smith, L.J. et al. (1 October 2009). "Spitzer SAGE Infrared Photometry of Massive Stars in the Large Magellanic Cloud". The Astronomical Journal 138 (4): 1003–1021. doi:10.1088/0004-6256/138/4/1003. ISSN 0004-6256. Bibcode: 2009AJ....138.1003B.
20. ↑ Walborn, Nolan R.; Drissen, Laurent; Parker, Joel Wm.; Saha, Abhijit; MacKenty, John W.; White, Richard L. (October 1999). "[ITAL]HST[/ITAL]/FOS Spatially Resolved Spectral Classification of Compact OB Groups in the Large Magellanic Cloud". The Astronomical Journal 118 (4): 1684–1699. doi:10.1086/301038.
21. ↑ Sabín-Sanjulián, C.; Simón-Díaz, S.; Herrero, A.; Puls, J.; Schneider, F. R. N.; Evans, C. J.; Garcia, M.; Najarro, F. et al. (May 2017). "The VLT-FLAMES Tarantula Survey: XXVI. Properties of the O-dwarf population in 30 Doradus". Astronomy & Astrophysics 601: A79. doi:10.1051/0004-6361/201629210.
22. ↑ 22.0 22.1 22.2 22.3 Crowther, Paul A.; Schnurr, Olivier; Hirschi, Raphael; Yusof, Norhasliza; Parker, Richard J.; Goodwin, Simon P.; Kassim, Hasan Abu (21 October 2010). "The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M⊙ stellar mass limit" (in en). Monthly Notices of the Royal Astronomical Society 408 (2): 731–751. doi:10.1111/j.1365-2966.2010.17167.x. ISSN 0035-8711. Bibcode: 2010MNRAS.408..731C.
23. ↑ 23.0 23.1 23.2 23.3 23.4 23.5 Melena, Nicholas W.; Massey, Philip; Morrell, Nidia I.; Zangari, Amanda M. (1 March 2008). "The massive star content of NGC 3603". The Astronomical Journal 135 (3): 878–891. doi:10.1088/0004-6256/135/3/878. ISSN 0004-6256. Bibcode: 2008AJ....135..878M.
24. ↑ Roman-Lopes, A.; Franco, G.A.P.; Sanmartim, D. (26 May 2016). "SOAR Optical and Near-infrared Spectroscopic Survey of Newly Discovered Massive Stars in the Periphery of Galactic Massive Star Clusters I-NGC 3603". The Astrophysical Journal 823 (2): 96. doi:10.3847/0004-637X/823/2/96. ISSN 1538-4357. Bibcode: 2016ApJ...823...96R.
25. ↑ Roman-Lopes, A. (1 November 2012). "A Galactic O2 If*/WN6 star possibly ejected from its birthplace in NGC 3603". Monthly Notices of the Royal Astronomical Society: Letters 427 (1): L65–L69. doi:10.1111/j.1745-3933.2012.01346.x. Bibcode: 2012MNRAS.427L..65R.
26. ↑ 26.00 26.01 26.02 26.03 26.04 26.05 26.06 26.07 26.08 26.09 26.10 26.11 26.12 26.13 26.14 26.15 26.16 26.17 26.18 26.19 Cite error: Invalid `<ref>` tag; no text was provided for refs named `Massey2000`
27. ↑ Fabricius, C.; Høg, E.; Makarov, V.V.; Mason, B.D.; Wycoff, G.L.; Urban, S.E. (March 2002). "The Tycho double star catalogue". Astronomy & Astrophysics 384 (1): 180–189. doi:10.1051/0004-6361:20011822. ISSN 0004-6361. Bibcode: 2002A&A...384..180F.
28. ↑ 28.0 28.1 28.2 28.3 Zaritsky, Dennis; Harris, Jason; Thompson, Ian B.; Grebel, Eva K. (October 2004). "The Magellanic Clouds Photometric Survey: The Large Magellanic Cloud Stellar Catalog and Extinction Map" (in en). The Astronomical Journal 128 (4): 1606–1614. doi:10.1086/423910. ISSN 0004-6256. Bibcode: 2004AJ....128.1606Z.
29. ↑ Drew, J.E.; Herrero, A.; Mohr-Smith, M.; Monguió, M.; Wright, N.J.; Kupfer, T.; Napiwotzki, R. (21 October 2018). "Massive stars in the hinterland of the young cluster, Westerlund 2" (in en). Monthly Notices of the Royal Astronomical Society 480 (2): 2109–2124. doi:10.1093/mnras/sty1905. ISSN 0035-8711. Bibcode: 2018MNRAS.480.2109D.
30. ↑ Vargas Álvarez, Carlos A.; Kobulnicky, Henry A.; Bradley, David R.; Kannappan, Sheila J.; Norris, Mark A.; Cool, Richard J.; Miller, Brendan P. (25 March 2013). "The distance to the massive galactic cluster Westerlund 2 from a spectroscopic and HST photometric study". The Astronomical Journal 145 (5): 125. doi:10.1088/0004-6256/145/5/125. ISSN 0004-6256. Bibcode: 2013AJ....145..125V.
31. ↑ 31.0 31.1 31.2 31.3 Hamann, W.-R.; Gräfener, G.; Liermann, A.; Hainich, R.; Sander, A.a.C.; Shenar, T. et al. (1 May 2019). "The galactic WN stars revisited - impact of Gaia distances on fundamental stellar parameters" (in en). Astronomy & Astrophysics 625: A57. doi:10.1051/0004-6361/201834850. ISSN 0004-6361. Bibcode: 2019A&A...625A..57H.
32. ↑ 32.0 32.1 Samus, N.N.; Kazarovets, E.V.; Durlevich, O.V.; Kireeva, N.N.; Pastukhova, E.N. (January 2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2017ARep...61...80S; 2017AZh....94...87S 1. Bibcode: 2009yCat....102025S.
33. ↑ 33.0 33.1 33.2 33.3 33.4 33.5 33.6 33.7 Gräfener, G.; Vink, J.S.; de Koter, A.; Langer, N. (November 2011). "The Eddington factor as the key to understand the winds of the most massive stars: Evidence for a Γ-dependence of Wolf-Rayet type mass loss". Astronomy & Astrophysics 535: A56. doi:10.1051/0004-6361/201116701. ISSN 0004-6361. Bibcode: 2011A&A...535A..56G.
34. ↑ 34.0 34.1 34.2 34.3 34.4 Figer, Donald F.; Najarro, Francisco; Gilmore, Diane; Morris, Mark; Kim, Sungsoo S.; Serabyn, Eugene et al. (10 December 2002). "Massive Stars in the Arches Cluster" (in en). The Astrophysical Journal 581 (1): 258–275. doi:10.1086/344154. ISSN 0004-637X. Bibcode: 2002ApJ...581..258F.
35. ↑ 35.0 35.1 35.2 35.3 35.4 Clark, J. S.; Lohr, M. E.; Najarro, F.; Dong, H.; Martins, F. (September 2018). "The Arches cluster revisited: I. Data presentation and stellar census". Astronomy & Astrophysics 617: A65. doi:10.1051/0004-6361/201832826. Bibcode: 2018A&A...617A..65C.
36. ↑ Oskinova, L. M.; Huenemoerder, D. P.; Hamann, W. -R.; Shenar, T.; Sander, A. A. C.; Ignace, R.; Todt, H.; Hainich, R. (2017). "On the Binary Nature of Massive Blue Hypergiants: High-resolution X-Ray Spectroscopy Suggests That Cyg OB2 12 is a Colliding Wind Binary". The Astrophysical Journal 845 (1): 39. doi:10.3847/1538-4357/aa7e79. Bibcode: 2017ApJ...845...39O.
37. ↑ Laur, Jaan; Kolka, Indrek; Eenmäe, Tõnis; Tuvikene, Taavi; Leedjärv, Laurits (February 2017). "Variability survey of brightest stars in selected OB associations". Astronomy & Astrophysics 598: A108. doi:10.1051/0004-6361/201629395. ISSN 0004-6361. Bibcode: 2017A&A...598A.108L.
38. ↑ 38.0 38.1 Pollock, A. M. T.; Crowther, P. A.; Bestenlehner, J. M.; Broos, Patrick S.; Townsley, Leisa K. (2025-03-21). "Melnick 39 is a very massive intermediate-period colliding-wind binary". Monthly Notices of the Royal Astronomical Society 539 (2): 1291. doi:10.1093/mnras/staf501. Bibcode: 2025MNRAS.539.1291P.
39. ↑ 39.0 39.1 Cite error: Invalid `<ref>` tag; no text was provided for refs named `hainich`
40. ↑ 40.0 40.1 40.2 Clark, J S; Lohr, M E; Najarro, F; Patrick, L R; Ritchie, B W (23 March 2023). "The Arches cluster revisited – IV. Observational constraints on the binary properties of very massive stars". Monthly Notices of the Royal Astronomical Society 521 (3): 4473–4489. doi:10.1093/mnras/stad449.
41. ↑ Oskinova, L. M.; Steinke, M.; Hamann, W.-R.; Sander, A.; Todt, H.; Liermann, A. (21 December 2013). "One of the most massive stars in the Galaxy may have formed in isolation" (in en). Monthly Notices of the Royal Astronomical Society 436 (4): 3357–3365. doi:10.1093/mnras/stt1817. ISSN 0035-8711. Bibcode: 2013MNRAS.436.3357O.
42. ↑ Gruner, D.; Hainich, R.; Sander, A. A. C.; Shenar, T.; Todt, H.; Oskinova, L. M.; Ramachandran, V.; Ayres, T. et al. (January 2019). "The extreme O-type spectroscopic binary HD 93129A: A quantitative, multiwavelength analysis". Astronomy & Astrophysics 621: A63. doi:10.1051/0004-6361/201833178. Bibcode: 2019A&A...621A..63G.
43. ↑ 43.0 43.1 43.2 43.3 43.4 43.5 de la Fuente, D.; Najarro, F.; Borissova, J.; Ramírez Alegría, S.; Hanson, M.M.; Trombley, C. et al. (May 2016). "Probing the Dragonfish star-forming complex: The ionizing population of the young massive cluster Mercer 30". Astronomy & Astrophysics 589: A69. doi:10.1051/0004-6361/201528004. ISSN 0004-6361. Bibcode: 2016A&A...589A..69D.
44. ↑ Rivero González, J.G.; Puls, J.; Najarro, F.; Brott, I. (January 2012). "Nitrogen line spectroscopy of O-stars: II. Surface nitrogen abundances for O-stars in the Large Magellanic Cloud". Astronomy & Astrophysics 537: A79. doi:10.1051/0004-6361/201117790. ISSN 0004-6361. Bibcode: 2012A&A...537A..79R.
45. ↑ 45.0 45.1 45.2 Schild, H.; Testor, G. (March 1992). "Spectral types and UBV magnitudes of stars in the 30 Doradus complex". Astronomy and Astrophysics Supplement Series 92: 729–748. ISSN 0365-0138. Bibcode: 1992A&AS...92..729S.
46. ↑ 46.0 46.1 Massey, Philip; Bodansky, Sarah; Penny, Laura R.; Neugent, Kathryn F. (2025). "A New Determination of the Mass of NGC 3603-A1: The Most Massive Binary Known?". The Astrophysical Journal 990 (1): 52. doi:10.3847/1538-4357/ade799. Bibcode: 2025ApJ...990...52M.
47. ↑ Barbá, Rodolfo H.; Gamen, Roberto C.; Martín-Ravelo, Pablo; Arias, Julia I.; Morrell, Nidia I. (2022). "The winking eye of a very massive star: WR 21a revealed as an eclipsing binary by TESS". Monthly Notices of the Royal Astronomical Society 516 (1): 1149. doi:10.1093/mnras/stac2173. Bibcode: 2022MNRAS.516.1149B.
48. ↑ 48.0 48.1 48.2 48.3 48.4 48.5 48.6 48.7 48.8 Cite error: Invalid `<ref>` tag; no text was provided for refs named `zacharias`
49. ↑ 49.0 49.1 49.2 49.3 49.4 49.5 Cite error: Invalid `<ref>` tag; no text was provided for refs named `Massey2001`
50. ↑ 50.0 50.1 50.2 50.3 Bonanos, A.Z.; Lennon, D.J.; Köhlinger, F.; van Loon, J.Th.; Massa, D. L.; Sewilo, M. et al. (1 August 2010). "Spitzer SAGE-SMC infrared photometry of massive stars in the Small Magellanic Cloud". The Astronomical Journal 140 (2): 416–429. doi:10.1088/0004-6256/140/2/416. ISSN 0004-6256. Bibcode: 2010AJ....140..416B.
51. ↑ Clementel, N.; Madura, T.I.; Kruip, C.J.H.; Paardekooper, J.-P.; Gull, T.R. (1 March 2015). "3D radiative transfer simulations of Eta Carinae's inner colliding winds - I. Ionization structure of helium at apastron" (in en). Monthly Notices of the Royal Astronomical Society 447 (3): 2445–2458. doi:10.1093/mnras/stu2614. ISSN 0035-8711. Bibcode: 2015MNRAS.447.2445C.
52. ↑ Gull, Theodore R.; Hillier, D. John; Hartman, Henrik; Corcoran, Michael F.; Damineli, Augusto; Espinoza-Galeas, David et al. (2022-07-01). "Eta Carinae: An evolving view of the central binary, its interacting winds and its foreground ejecta". The Astrophysical Journal 933 (2): 175. doi:10.3847/1538-4357/ac74c2. ISSN 0004-637X. Bibcode: 2022ApJ...933..175G.
53. ↑ Ulaczyk, K.; Szymański, M.K.; Udalski, A.; Kubiak, M.; Pietrzyński, G.; Soszyński, I. et al. (1 June 2013). "Variable Stars from the OGLE-III Shallow Survey in the Large Magellanic Cloud". Acta Astronomica 63 (2): 159–179. doi:10.1086/338286. ISSN 0001-5237. Bibcode: 2013AcA....63..159U.
54. ↑ Evans, C.J.; Lennon, D.J.; Smartt, S. J.; Trundle, C. (September 2006). "The VLT-FLAMES survey of massive stars: observations centered on the Magellanic Cloud clusters NGC 330, NGC 346, NGC 2004, and the N11 region". Astronomy & Astrophysics 456 (2): 623–638. doi:10.1051/0004-6361:20064988. ISSN 0004-6361. Bibcode: 2006A&A...456..623E.
55. ↑ 55.0 55.1 Shenar, T.; Sablowski, D. P.; Hainich, R.; Todt, H.; Moffat, A. F. J.; Oskinova, L. M.; Ramachandran, V.; Sana, H. et al. (July 2019). "The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud: Spectroscopy, orbital analysis, formation, and evolution". Astronomy & Astrophysics 627: A151. doi:10.1051/0004-6361/201935684. Bibcode: 2019A&A...627A.151S.
56. ↑ 56.0 56.1 56.2 56.3 56.4 56.5 56.6 Massa, D.; Fullerton, A. W.; Prinja, R. K. (September 2017). "Mass-loss rates from mid-infrared excesses in LMC and SMC O stars" (in en). Monthly Notices of the Royal Astronomical Society 470 (3): 3765–3774. doi:10.1093/mnras/stx1443. ISSN 0035-8711. Bibcode: 2017MNRAS.470.3765M.
57. ↑ Bestenlehner, Joachim M.; Crowther, Paul A.; Broos, Patrick S.; Pollock, Andrew M.T.; Townsley, Leisa K. (2022). "Melnick 33Na: A very massive colliding-wind binary system in 30 Doradus". Monthly Notices of the Royal Astronomical Society 510 (4): 6133–6149. doi:10.1093/mnras/stab3521. Bibcode: 2022MNRAS.510.6133B.
58. ↑ Castro, N.; Crowther, P.A.; Evans, C.J.; Mackey, J.; Castro-Rodriguez, N.; Vink, J.S. et al. (2018). "Mapping the core of the Tarantula Nebula with VLT-MUSE. I. Spectral and nebular content around R136". Astronomy & Astrophysics 614: 12. doi:10.1051/0004-6361/201732084. A147. Bibcode: 2018A&A...614A.147C.
59. ↑ 59.0 59.1 Lua error: Internal error: The interpreter has terminated with signal "24".
60. ↑ 60.0 60.1 Lohr, M. E.; Clark, J. S.; Najarro, F.; Patrick, L. R.; Crowther, P. A.; Evans, C. J. (September 2018). "The Arches cluster revisited: II. A massive eclipsing spectroscopic binary in the Arches cluster". Astronomy & Astrophysics 617: A66. doi:10.1051/0004-6361/201832670. Bibcode: 2018A&A...617A..66L.
61. ↑ 61.0 61.1 Mahy, L.; Sana, H.; Abdul-Masih, M.; Almeida, L. A.; Langer, N.; Shenar, T.; de Koter, A.; de Mink, S. E. et al. (February 2020). "The Tarantula Massive Binary Monitoring: III. Atmosphere analysis of double-lined spectroscopic systems". Astronomy & Astrophysics 634: A118. doi:10.1051/0004-6361/201936151. Bibcode: 2020A&A...634A.118M.
62. ↑ 62.0 62.1 Fang, M.; van Boekel, R.; King, R. R.; Henning, Th.; Bouwman, J.; Doi, Y. et al. (March 2012). "Star formation and disk properties in Pismis 24". Astronomy & Astrophysics 539: A119. doi:10.1051/0004-6361/201015914. ISSN 0004-6361. Bibcode: 2012A&A...539A.119F.
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64. ↑ Crowther, P. A.; Hadfield, L. J.; Clark, J. S.; Negueruela, I.; Vacca, W. D. (1 November 2006). "A census of the Wolf-Rayet content in Westerlund 1 from near-infrared imaging and spectroscopy". Monthly Notices of the Royal Astronomical Society 372 (3): 1407–1424. doi:10.1111/j.1365-2966.2006.10952.x. Bibcode: 2006MNRAS.372.1407C.
65. ↑ Vázquez, R.A.; Baume, G. (June 2001). "The open cluster Havlen-Moffat no. 1 revisited". Astronomy & Astrophysics 371 (3): 908–920. doi:10.1051/0004-6361:20010410. ISSN 0004-6361. Bibcode: 2001A&A...371..908V.
66. ↑ Nebot Gómez-Morán, A.; Oskinova, L. M. (2018). "The X-ray catalog of spectroscopically identified Galactic O stars. Investigating the dependence of X-ray luminosity on stellar and wind parameters". Astronomy and Astrophysics 620: A89. doi:10.1051/0004-6361/201833453. Bibcode: 2018A&A...620A..89N.
67. ↑ Mang Román, Armin; Zeidler, Peter; Hamann, Wolf-Rainer; Oskinova, Lidia M.; Rickard, M. J.; Reyero Serantes, S.; Todt, H.; Gallagher, J. S. et al. (10 May 2025). "First JWST/NIRSpec Spectroscopy of O Stars in the Small Magellanic Cloud". The Astrophysical Journal Letters 984 (2): L49. doi:10.3847/2041-8213/adcc22. Bibcode: 2025ApJ...984L..49M.
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69. ↑ 69.0 69.1 Shenar, T.; Sana, H.; Marchant, P.; Pablo, B.; Richardson, N.; Moffat, A. F. J.; Van Reeth, T.; Barbá, R. H. et al. (June 2021). "The Tarantula Massive Binary Monitoring: V. R 144: a wind-eclipsing binary with a total mass ≳140 M ⊙". Astronomy & Astrophysics 650: A147. doi:10.1051/0004-6361/202140693.
70. ↑ Kastner, Joel H.; Buchanan, Catherine L.; Sargent, B.; Forrest, W. J. (10 February 2006). "Spitzer Spectroscopy of Dusty Disks around B[e] Hypergiants in the Large Magellanic Cloud" (in en). The Astrophysical Journal 638 (1): L29–L32. doi:10.1086/500804. ISSN 0004-637X. Bibcode: 2006ApJ...638L..29K.
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72. ↑ Grimm, H.-J.; McDowell, J.; Zezas, A.; Kim, D.-W.; Fabbiano, G. (December 2005). "The X-Ray Binary Population in M33. I. Source List and Luminosity Function" (in en). The Astrophysical Journal Supplement Series 161 (2): 271–303. doi:10.1086/468185. ISSN 0067-0049. Bibcode: 2005ApJS..161..271G.
73. ↑ Brož, M.; Harmanec, P.; Zasche, P.; Catalan-Hurtado, R.; Barlow, B. N.; Frondorf, W.; Wolf, M.; Drechsel, H. et al. (2022). "Towards a consistent model of the hot quadruple system HD 93206 = QZ Carinæ. II. N-body model". Astronomy & Astrophysics 666: A24. doi:10.1051/0004-6361/202243596. Bibcode: 2022A&A...666A..24B.
74. ↑ Rainot, A.; Reggiani, M.; Sana, H.; Bodensteiner, J.; Gomez-Gonzalez, C. A.; Absil, O.; Christiaens, V.; Delorme, P. et al. (2020). "Carina High-contrast Imaging Project for massive Stars (CHIPS). I. Methodology and proof of concept on QZ Car (≡ HD 93206)". Astronomy and Astrophysics 640: A15. doi:10.1051/0004-6361/201936448. Bibcode: 2020A&A...640A..15R.
75. ↑ Holgado, G.; Simón-Díaz, S.; Herrero, A.; Barbá, R. H. (September 2022). "The IACOB project: VII. The rotational properties of Galactic massive O-type stars revisited". Astronomy & Astrophysics 665: A150. doi:10.1051/0004-6361/202243851. Bibcode: 2022A&A...665A.150H.
76. ↑ Blomme, R.; Mahy, L.; Catala, C.; Cuypers, J.; Gosset, E.; Godart, M.; Montalban, J.; Ventura, P. et al. (September 2011). "Variability in the CoRoT photometry of three hot O-type stars: HD 46223, HD 46150, and HD 46966". Astronomy & Astrophysics 533: A4. doi:10.1051/0004-6361/201116949.
77. ↑ Rauw, G.; Sana, H.; Gosset, E.; Vreux, J.-M.; Jehin, E.; Parmentier, G. (August 2000). "A new orbital solution for the massive binary system HD 93403". Astronomy & Astrophysics 360: 1003–1010. ISSN 0004-6361. Bibcode: 2000A&A...360.1003R.
78. ↑ Urbaneja, Miguel (2011). "Quantitative Spectroscopy of Blue Supergiant Stars in the Disk of M81: Metallicity, Metallicity Gradient, and Distance". The Astrophysical Journal 747 (1): 15. doi:10.1088/0004-637X/747/1/15. Bibcode: 2012ApJ...747...15K.
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82. ↑ 82.0 82.1 Bouret, J.-C.; Hillier, D.J.; Lanz, T.; Fullerton, A.W. (2012). "Properties of galactic early-type O-supergiants: A combined FUV-UV and optical analysis". Astronomy & Astrophysics 544: A67. doi:10.1051/0004-6361/201118594. Bibcode: 2012A&A...544A..67B.
83. ↑ Skiff, B. A. (October 2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009- )". VizieR On-line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014) 1. Bibcode: 2014yCat....1.2023S.
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85. ↑ Patten, Nikhil; Kobulnicky, Henry A.; Povich, Matthew S.; Whisnant, Angelica S.; Andrews, Sydney; Boone, Alexandra; Dandu, Srujan; Jones, Naomi et al. (1 August 2025). "Fundamental Parameters for Central Stars of 103 Infrared Bow Shock Nebulae". The Astrophysical Journal 988 (2): 183. doi:10.3847/1538-4357/ade22f. Bibcode: 2025ApJ...988..183P.
86. ↑ Liermann, Adriane; Hamann, Wolf-Rainer; Oskinova, Lidia M.; Todt, Helge (January 2011). "High-mass stars in the Galactic center Quintuplet cluster". Société Royale des Sciences de Liège, Bulletin 80: 160–164. ISSN 0037-9565. Bibcode: 2011BSRSL..80..160L.
87. ↑ Liermann, A.; Hamann, W.-R.; Oskinova, L. M.; Todt, H.; Butler, K. (December 2010). "The Quintuplet cluster: II. Analysis of the WN stars". Astronomy & Astrophysics 524: A82. doi:10.1051/0004-6361/200912612. Bibcode: 2010A&A...524A..82L.
88. ↑ Massey, Philip (July 2002). "A UBVR CCD Survey of the Magellanic Clouds" (in en). The Astrophysical Journal Supplement Series 141 (1): 81–122. doi:10.1086/338286. ISSN 0067-0049. Bibcode: 2002ApJS..141...81M.
89. ↑ de Vries, N.; Portegies Zwart, S.; Figueira, J. (2014). "The evolution of triples with a Roche lobe filling outer star". Monthly Notices of the Royal Astronomical Society 438 (3): 1909. doi:10.1093/mnras/stt1688. Bibcode: 2014MNRAS.438.1909D.
90. ↑ Hill, G. M.; Moffat, A. F. J.; St-Louis, N. (1 October 2002). "Modelling the colliding-winds spectra of the 19-d WR + OB binary in the massive triple system θ Muscae" (in en). Monthly Notices of the Royal Astronomical Society 335 (4): 1069–1078. doi:10.1046/j.1365-8711.2002.05694.x. ISSN 0035-8711. Bibcode: 2002MNRAS.335.1069H.
91. ↑ Mitschang, Arik W.; Schulz, Norbert S.; Huenemoerder, David P.; Nichols, Joy S.; Testa, Paola (2011). "Detailed X-ray line properties of θ2 Ori A in quiescence". The Astrophysical Journal 734 (1): 14. doi:10.1088/0004-637X/734/1/14. Bibcode: 2011ApJ...734...14M.θ2+Ori+A+in+quiescence&rft.jtitle=The+Astrophysical+Journal&rft.aulast=Mitschang&rft.aufirst=Arik+W.&rft.au=Mitschang, Arik+W.&rft.au=Schulz, Norbert+S.&rft.au=Huenemoerder, David+P.&rft.au=Nichols, Joy+S.&rft.au=Testa, Paola&rft.date=2011&rft.volume=734&rft.issue=1&rft.pages=14&rft_id=info:doi/10.1088/0004-637X/734/1/14&rft_id=info:bibcode/2011ApJ...734...14M&rfr_id=info:sid/en.wikibooks.org:Astronomy:List_of_most_massive_stars">
92. ↑ Aldoretta, E.J.; Caballero-Nieves, S.M.; Gies, D.R.; Nelan, E.P.; Wallace, D.J.; Hartkopf, W.I. et al. (2015). "The multiplicity of massive stars: A high angular-resolution survey with the guidance sensor". The Astronomical Journal 149 (1): 26. doi:10.1088/0004-6256/149/1/26. Bibcode: 2015AJ....149...26A.
93. ↑ 93.0 93.1 93.2 Repolust, T.; Puls, J.; Herrero, A. (February 2004). "Stellar and wind parameters of Galactic O-stars: The influence of line-blocking/blanketing". Astronomy & Astrophysics 415 (1): 349–376. doi:10.1051/0004-6361:20034594. ISSN 0004-6361. Bibcode: 2004A&A...415..349R.
94. ↑ Rivet, J-P; Siciak, A.; de Almeida, E.S.G.; Vakili, F.; Domiciano de Souza, A.; Fouché, M. et al. (2020). "Intensity interferometry of P Cygni in the H α emission line: Towards distance calibration of LBV supergiant stars". Monthly Notices of the Royal Astronomical Society 494 (1): 218–227. doi:10.1093/mnras/staa588. Bibcode: 2020MNRAS.494..218R.
95. ↑ Clark, J. S.; Najarro, F.; Negueruela, I.; Ritchie, B. W.; Urbaneja, M. A.; Howarth, I. D. (May 2012). "On the nature of the galactic early-B hypergiants". Astronomy & Astrophysics 541: A145. doi:10.1051/0004-6361/201117472. ISSN 0004-6361. Bibcode: 2012A&A...541A.145C.
96. ↑ Kozok, J. R. (September 1985). "Photometric observations of emission B-stars in the southern Milky Way". Astronomy and Astrophysics Supplement Series 61: 387–405. Bibcode: 1985A&AS...61..387K.
97. ↑ Hummel, C. A.; Rivinius, Th.; Nieva, M.-F.; Stahl, O.; van Belle, G.; Zavala, R. T. (2013). "Dynamical mass of the O-type supergiant in ζ Orionis A". Astronomy & Astrophysics 554: A52. doi:10.1051/0004-6361/201321434. ISSN 0004-6361. Bibcode: 2013A&A...554A..52H.
98. ↑ Balega, Yu. Yu.; Chentsov, E.L.; Leushin, V.V.; Rzaev, A.Kh.; Weigelt, G. (2014). "Young massive binary θ1 Ori C: Radial velocities of components". Astrophysical Bulletin 69 (1): 46–57. doi:10.1134/S1990341314010052. ISSN 1990-3413. Bibcode: 2014AstBu..69...46B.
99. ↑ Searle, S. C.; Prinja, R. K.; Massa, D.; Ryans, R. (2008). "Quantitative studies of the optical and UV spectra of Galactic early B supergiants. I. Fundamental parameters". Astronomy and Astrophysics 481 (3): 777–797. doi:10.1051/0004-6361:20077125. Bibcode: 2008A&A...481..777S.
100. ↑ 100.00 100.01 100.02 100.03 100.04 100.05 100.06 100.07 100.08 100.09 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society 410 (1): 190–200. doi:10.1111/j.1365-2966.2010.17434.x. Bibcode: 2011MNRAS.410..190T.
101. ↑ Kashi, Amit; Soker, Noam (1 November 2010). "Periastron Passage Triggering of the 19th Century Eruptions of Eta Carinae". The Astrophysical Journal 723 (1): 602–611. doi:10.1088/0004-637X/723/1/602. ISSN 0004-637X. Bibcode: 2010ApJ...723..602K.
102. ↑ Hamaguchi, Kenji; Corcoran, Michael F.; Pittard, Julian M.; Sharma, Neetika; Takahashi, Hiromitsu; Russell, Christopher M.P. et al. (September 2018). "Non-thermal X-rays from colliding wind shock acceleration in the massive binary Eta Carinae" (in en). Nature Astronomy 2 (9): 731–736. doi:10.1038/s41550-018-0505-1. ISSN 2397-3366. Bibcode: 2018NatAs...2..731H.
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104. ↑ Oplištilová, Alžběta; Brož, Miroslav; Hummel, Christian A.; Harmanec, Petr; Barlow, Brad (2025-07-03). "Star formation and disk properties in Pismis 24". Astronomy & Astrophysics 539: A119. doi:10.1051/0004-6361/201015914. Bibcode: 2012A&A...539A.119F.
105. ↑ 105.0 105.1 105.2 Hoffleit, Dorrit; Jaschek, Carlos (1991). The Bright star catalogue (5th Revised ed.). New Haven, Conn.: Yale University Observatory. Bibcode: 1991bsc..book.....H.
106. ↑ Howarth, Ian D; van Leeuwen, Floor (2019-01-31). "The distance, rotation, and physical parameters of ζ Pup" (in en). Monthly Notices of the Royal Astronomical Society 484 (4): 5350. doi:10.1093/mnras/stz291. ISSN 0035-8711. Bibcode: 2019MNRAS.484.5350H.
107. ↑ Shenar, T.; Oskinova, L.; Hamann, W.-R.; Corcoran, M.F.; Moffat, A.F.J.; Pablo, H. et al. (2015). "A Coordinated X-Ray and Optical Campaign of the Nearest Massive Eclipsing Binary, δ Orionis Aa. IV. A Multiwavelength, Non-LTE Spectroscopic Analysis". Astrophysical Journal 809 (2): 135. doi:10.1088/0004-637X/809/2/135. Bibcode: 2015ApJ...809..135S.
108. ↑ Tokovinin, A A. (1997). "MSC - a catalogue of physical multiple stars". Astronomy and Astrophysics Supplement Series 124: 75–84. doi:10.1051/aas:1997181. Bibcode: 1997A&AS..124...75T.
109. ↑ Dufton, P.L.; Smartt, S.J.; Lee, J.K.; Ryans, R.S.I.; Hunter, I.; Evans, C.J. et al. (2006). "The VLT-FLAMES survey of massive stars: stellar parameters and rotational velocities in NGC 3293, NGC 4755 and NGC 6611". Astronomy & Astrophysics 457 (1): 265–280. doi:10.1051/0004-6361:20065392. ISSN 0004-6361. Bibcode: 2006A&A...457..265D.
110. ↑ Shultz, M.; Wade, G.A.; Petit, V.; Grunhut, J.; Neiner, C.; Hanes, D. (2014). "An observational evaluation of magnetic confinement in the winds of BA supergiants". Monthly Notices of the Royal Astronomical Society 438 (2): 1114. doi:10.1093/mnras/stt2260. Bibcode: 2014MNRAS.438.1114S.
111. ↑ Smith, M.A. (August 1981). "Nonradial pulsations in the zero-age main-sequence star upsilon Orionis (O9.5V)" (in en). The Astrophysical Journal 248: 214–221. doi:10.1086/159145. ISSN 0004-637X. Bibcode: 1981ApJ...248..214S.
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115. ↑ Martins, F.; Schaerer, D.; Hillier, D. J.; Meynadier, F.; Heydari-Malayeri, M.; Walborn, N. R. (2005). "O stars with weak winds: the Galactic case". Astronomy & Astrophysics 441 (2): 735–762. doi:10.1051/0004-6361:20052927. ISSN 0004-6361. Bibcode: 2005A&A...441..735M.
116. ↑ 116.0 116.1 Hohle, M.M.; Neuhäuser, R.; Schutz, B.F. (April 2010). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten 331 (4): 349. doi:10.1002/asna.200911355. Bibcode: 2010AN....331..349H.
117. ↑ Przybilla, N.; Firnstein, M.; Nieva, M.F.; Meynet, G.; Maeder, A. (2010). "Mixing of CNO-cycled matter in massive stars". Astronomy and Astrophysics 517: A38. doi:10.1051/0004-6361/201014164. Bibcode: 2010A&A...517A..38P.
118. ↑ Firnstein, M.; Przybilla, N. (2012). "Quantitative spectroscopy of Galactic BA-type supergiants. I. Atmospheric parameters". Astronomy & Astrophysics 543: A80. doi:10.1051/0004-6361/201219034. Bibcode: 2012A&A...543A..80F.
119. ↑ 119.0 119.1 119.2 119.3 Johnson, H.L.; Iriarte, B.; Mitchell, R.I.; Wisniewskj, W.Z. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99): 99. Bibcode: 1966CoLPL...4...99J.
120. ↑ Nieva, María-Fernanda; Przybilla, Norbert (2014). "Fundamental properties of nearby single early B-type stars". Astronomy & Astrophysics 566: A7. doi:10.1051/0004-6361/201423373. Bibcode: 2014A&A...566A...7N.
121. ↑ Mazumdar, A.; Briquet, M.; Desmet, M.; Aerts, C. (November 2006). "An asteroseismic study of the β Cephei star β Canis Majoris". Astronomy and Astrophysics 459 (2): 589–596. doi:10.1051/0004-6361:20064980. Bibcode: 2006A&A...459..589M.
122. ↑ Cousins, A.W.J. (1972). "UBV Photometry of Some Very Bright Stars". Monthly Notes of the Astronomical Society of Southern Africa 31: 69. Bibcode: 1972MNSSA..31...69C.
123. ↑ Cite error: Invalid `<ref>` tag; no text was provided for refs named `marchenko`
124. ↑ 124.0 124.1 Nicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Astronomy and Astrophysics Supplement Series 34: 1–49. Bibcode: 1978A&AS...34....1N.
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126. ↑ Gutierrez-Moreno, Adelina; Moreno, Hugo (1968-06-01). "A Photometric Investigation of the SCORPlO-CENTAURUS Association". The Astrophysical Journal Supplement Series 15: 459. doi:10.1086/190168. ISSN 0067-0049. Bibcode: 1968ApJS...15..459G.
127. ↑ Nugis, T.; Lamers, H.J.G.L.M. (2000). "Mass-loss rates of Wolf-Rayet stars as a function of stellar parameters". Astronomy and Astrophysics 360: 227. Bibcode: 2000A&A...360..227N.
128. ↑ Challouf, M.; Nardetto, N.; Mourard, D.; Graczyk, D.; Aroui, H.; Chesneau, O. et al. (2014). "Improving the surface brightness-color relation for early-type stars using optical interferometry". Astronomy & Astrophysics 570: A104. doi:10.1051/0004-6361/201423772. Bibcode: 2014A&A...570A.104C.
129. ↑ Kudritzki, R.P.; Reimers, D. (1978). "On the absolute scale of mass-loss in red giants. II. Circumstellar absorption lines in the spectrum of α Sco B and mass-loss of α Sco A". Astronomy and Astrophysics 70: 227. Bibcode: 1978A&A....70..227K.α+Sco+B+and+mass-loss+of+α+Sco+A&rft.jtitle=Astronomy+and+Astrophysics&rft.aulast=Kudritzki&rft.aufirst=R.P.&rft.au=Kudritzki, R.P.&rft.au=Reimers, D.&rft.date=1978&rft.volume=70&rft.pages=227&rft_id=info:bibcode/1978A&A....70..227K;&rfr_id=info:sid/en.wikibooks.org:Astronomy:List_of_most_massive_stars">
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132. ↑ 132.0 132.1 David, Trevor J.; Hillenbrand, Lynne A. (2015). "The ages of early-type stars: Strömgren photometric methods calibrated, validated, tested, and applied to hosts and prospective hosts of directly imaged exoplanets". The Astrophysical Journal 804 (2): 146. doi:10.1088/0004-637X/804/2/146. Bibcode: 2015ApJ...804..146D.
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135. ↑ Sánchez Arias, Julieta Paz; Németh, Péter; De Almeida, Elisson Saldanha da Gama; Ruiz Diaz, Matias Agustin; Kraus, Michaela; Haucke, Maximiliano (2023). "Unveiling the Evolutionary State of Three B Supergiant Stars: PU Gem, ϵ CMa, and η CMa". Galaxies 11 (5): 93. doi:10.3390/galaxies11050093. Bibcode: 2023Galax..11...93S.
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149. ↑ Bessell, M.S.; Castelli, F.; Plez, B. (May 1998). "Model atmospheres broad-band colors, bolometric corrections and temperature calibrations for O–M stars". Astronomy & Astrophysics 333: 231–250. ISSN 0004-6361. Bibcode: 1998A&A...333..231B.
150. ↑ Lua error: Internal error: The interpreter has terminated with signal "24".

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## External links

* "Statistics in Arches cluster". May 2005. http://hubblesite.org/newscenter/archive/releases/2005/05/.
* "Most Massive Star Discovered". 7 June 2007. http://www.space.com/scienceastronomy/070607_massive_star.html.
* "Arches cluster". March 2005. https://www.sciencedaily.com/releases/2005/03/050309142833.htm.
* "How heavy can a star get?". http://www.3towers.com/sGrasslands/Essays/HeavyStar/HeavyStar01.asp.
* "Hubble Unveils Monster Stars". March 2016. https://www.nasa.gov/feature/goddard/2016/hubble-unveils-monster-stars.

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