List of largest stars

Below are lists of the largest stars currently known, ordered by radius and separated into categories by galaxy. The unit of measurement used is the radius of the Sun (approximately 695,700 km; 432,300 mi).^[1]

Overview

Although red supergiants are often considered the largest stars, some other star types have been found to temporarily increase significantly in radius, such as during LBV eruptions or luminous red novae. Luminous red novae appear to expand extremely rapidly, reaching thousands to tens of thousands of solar radii within only a few months, significantly larger than the largest red supergiants.^[2]

Some studies use models that predict high-accreting Population III or Population I supermassive stars (SMSs) in the very early universe could have evolved "red supergiant protostars". These protostars are thought to have accretion rates larger than the rate of contraction, resulting in lower temperatures but with radii reaching up to many tens of thousands of R_☉, comparable to some of the largest known black holes.^[3]^[4]^[5]

Angular diameters

The angular diameters of stars can be measured directly using stellar interferometry. Other methods can use lunar occultations or from eclipsing binaries, which can be used to test indirect methods of finding stellar radii. Only a few supergiants can be occulted by the Moon, including Antares and 119 Tauri. Examples of eclipsing binaries are Epsilon Aurigae (Almaaz), VV Cephei, and V766 Centauri (HR 5171). Angular diameter measurements can be inconsistent because the boundary of the very tenuous atmosphere (opacity) differs depending on the wavelength of light in which the star is observed.^{[citation needed]}

Uncertainties remain with the membership and order of the lists, especially when deriving various parameters used in calculations, such as stellar luminosity and effective temperature. Often stellar radii can only be expressed as an average or be within a large range of values. Values for stellar radii vary significantly in different sources and for different observation methods.^{[citation needed]}

All the sizes stated in these lists have inaccuracies and may be disputed. The lists are still a work in progress and parameters are prone to change.

Caveats

Various issues exist in determining accurate radii of the largest stars, which in many cases do display significant errors. The following lists are generally based on various considerations or assumptions; these include:

Stellar radii or diameters are usually derived only approximately using the Stefan–Boltzmann law for the deduced stellar luminosity and effective surface temperature.
Stellar distances, and their errors, for most stars, remain uncertain or poorly determined.
Many extended supergiant atmospheres also significantly change in size over time, regularly or irregularly pulsating over several months or years as variable stars. This makes adopted luminosities poorly known and may significantly change the quoted radii.
Other direct methods for determining stellar radii rely on lunar occultations or from eclipses in binary systems. This is only possible for a very small number of stars.
Many distance estimates for red supergiants come from stellar cluster or association membership, because it is difficult to calculate accurate distances for red supergiants that are not part of any cluster or association.
In these lists are some examples of extremely distant extragalactic stars, which may have slightly different properties and natures than the currently largest known stars in the Milky Way. For example, some red supergiants in the Magellanic Clouds are suspected to have slightly different limiting temperatures and luminosities. Such stars may exceed accepted limits by undergoing large eruptions or changing their spectral types over just a few months (or potentially years).^[6]^[7]

Lists

The following lists show the largest known stars based on the host galaxy.

Milky Way

List of the largest known stars in the Milky Way
Star name	Solar radius (`R`_☉)	Method^[a]	Notes
Orbit of Saturn	2,047–2,049.9^[8]^[b]		Reported for reference
WOH G64 (For comparison)	1,540^[c] ± 77^[9]	L/T_eff	Located in the Large Magellanic Cloud. The largest known star with a well-defined radius.^[9]^[10]^[14]^[11]
Theoretical limit of star size (Milky Way)	~1,500^[15]–1,800^[16]		Lower value comes from the rough average radii of the three largest stars studied in the paper. It is consistent with the largest possible stellar radii predicted from the current evolutionary theory, and it is believed that stars above this radius would be too unstable and usually do not form.^[15] Higher value is derived from evolutionary modelling of red supergiants with low metallicites and an initial mass of 50 `M`_☉. Reported for reference
RSGC1-F01	1,530 ± 365^[17]	L/T_eff
VY Canis Majoris	1,420±120^[18]^[19]^[20]	AD	An extreme oxygen-rich red hypergiant that has experienced two dimming periods in the 20th century where the star became dimmer by up to 2.5 magnitudes.^[21] Potentially the largest known star in the Milky Way.^[19] There is a possilbility that this size might be a bit overestimated (on the order of 1 sigma). Hence, the quoted radius might be just an upper limit.^[18]
AH Scorpii	1,411±124^[22]^[23]	AD
RSGC1-F06	1,382 ± 331^[17]	L/T_eff
S Persei	1,364±6^[24]	AD
VX Sagittarii	1,356^[25] – 1,480+180 −160^[23]	AD	The most luminous known asymptotic giant branch star.^[25] Widely recognised as being among the largest known stars.^[26]
NML Cygni	<1,350+195 −229^[d]	AD	Surrounding dusty region is very complex making the radius hard to determine.^[27]
Stephenson 2 DFK 2	1,301 ± 285^[17]	L/T_eff	Another red supergiant, Stephenson 2 DFK 1 has an estimated radius of 2,150 `R`_☉. However, it is potentially not a member of the Stephenson 2 cluster and also has a distance with an uncertainty of ≳50% due to it only being measured with radial velocities.^[17]^[29]
Stephenson 2 DFK 49	1,300 ± 283^[17]	L/T_eff	A K-type star similar to the yellow hypergiant IRC +10420 that has left its red supergiant stage.^[17]
HD 143183 (V558 Normae)	1,261^[30]	L/T_eff
PZ Cassiopeiae	1,259 – 1,336,^[31] 1,585+160 −120^[32]	L/T_eff & AD
RSGC1-F10	1,246 ± 292^[17]	L/T_eff
V354 Cephei	1,245^[30]	L/T_eff
Westerlund 1 W237 (Westerlund 1 BKS B)	1,241±70^[33]	L/T_eff
ST Cephei	1,218^[30]	L/T_eff
IRC -10414	~1,200^[34]	L/T_eff
V517 Monocerotis	1,196+80 −159^[35]	L/T_eff
RSGC1-F05	1,185 ± 312^[17]	L/T_eff
GCIRS 7	1,170±60,^[36] 1,359,^[37] 1,368^[38]	AD & L/T_eff
Westerlund 1 W26 (Westerlund 1 BKS AS)	1,165±58–1,221±120^[33]	L/T_eff
EV Carinae	1,165^[39]	L/T_eff
[A72c] 16	1,157^[30]	L/T_eff
WY Velorum A	1,157^[30]	L/T_eff	A symbiotic binary.^[40]
RSGC1-F08	1,150 ± 259^[17]	L/T_eff
RSGC1-F02	1,128 ± 262^[17]	L/T_eff
Orbit of Jupiter	1,114.5–1,115.8^[8]^[b]		Reported for reference
V582 Cassiopeiae	1,111^[30]	L/T_eff
RW Cygni	1,103+251 −177^[41]	AD
RW Cephei	1,100±40^[42]	AD	A K-type hypergiant star that experienced a "great dimming" event in 2022, similar to Betelgeuse.
RT Carinae	1,090^[15]	L/T_eff
RSGC1-F04	1,082,^[43] 1,100,^[44] 1,422+305 −390^[17]	L/T_eff
UU Persei	1,079+9 −8^[35]	L/T_eff
LL Pegasi	1,074^[45]	L/T_eff
HD 126577	1,066+9 −32^[35]	L/T_eff
V766 Centauri Aa	1,060–1,160^[46]	?	V766 Centauri Aa is a rare variable yellow hypergiant.
HaroChavira 1	1,058^[47]	L/T_eff
CM Velorum	1,048^[30] – 1,416.24+0.40 −0.96^[35]	L/T_eff
AG Camelopardalis	1,048^[30]	L/T_eff
SU Persei [pt]	1,044+31 −21 – 1,139+34 −23,^[24]	AD
SW Cephei	1,035+75 −120^[32]	AD
KY Cygni	1,032^[47]	L/T_eff
RSGC1-F11	1,032 ± 232^[17]	L/T_eff
BC Cygni	1,031^[47]–1,187+34 −37^[35]	L/T_eff	A more detailed but older study gives values of 1,081 `R`_☉ (856–1,375) for the year 2000, and 1,303 `R`_☉ (1,021–1,553) for the year 1900.^[48]
MY Cephei	1,028 ± 169 – 1,138 ± 387^[49]^[e]	L/T_eff
V346 Puppis	1,025^[50]	L/T_eff
V530 Cassiopeiae	1,017^[30]	L/T_eff
RSGC1-F13	1,017 ± 246^[17]	L/T_eff
V602 Carinae	1,015^[51]	AD
VV Cephei A	1,015^[52]	AD	A red supergiant star orbited by a smaller B-type main-sequence star with a radius estimated between 13^[53] and 25 `R`_☉.^[54] Widely recognised as being among the largest known stars.^[26] Another estimate give a radius of 660 `R`_☉^[30] based on the Gaia DR3 distance of 1 kpc.^[35]
U Lacertae A	1,013^[30]	L/T_eff
KW Sagittarii	1,009±142^[22]^[23]	AD
Ve 4-64	1,007^[30]	L/T_eff
RSGC1-F07	1,006 ± 238^[17]	L/T_eff
V349 Carinae	1,002+12 −74^[35]	L/T_eff
V674 Cephei	999^[30]	L/T_eff
RSGC1-F09	996 ± 498^[17]	L/T_eff
IRAS 18111-2257	~990 – 1,200^[55]	L/T_eff	Estimated based on the bolometric luminosity (14,000–20,000 `L`_☉) and assumed effective temperature of 2,000 K. Another period-luminosity-derived luminosity for this star results in a radius of 1,730 `R`_☉.^[55]
CZ Hydrae	986^[56]	L/T_eff
CIT 11	982^[30]	L/T_eff
V381 Cephei Aa	977^[30]	L/T_eff
MSX6C G086.5890–00.7718	(975+175 −183–1,035+186 −158)^[57]–1,196.91+6.31 −6.35^[35]	L/T_eff	Lower values based on the Gaia DR3 effective temperature and the luminosity of Levesque et al. (2005) and that of Messineo & Brown (2019). Higher value based on the GSP Phot-Aeneas library using BR/RP spectra in Gaia DR3.
μ Cephei (Herschel's Garnet Star)	972±228,^[58] 1,259,^[59] 1,420,^[15] 1,426 ⁺²⁸² ₋₁₁₉^[f]	L/T_eff & AD	Widely recognised as being among the largest known stars.^[26] Might be the largest star visible to the naked eye.^[60]
V3953 Sagittarii (IRC −30398)	970^[61]	L/T_eff
V396 Centauri	965^[30]	L/T_eff
UW Aquilae	964^[30]	L/T_eff
RSGC1-F12	955 ± 226^[17]	L/T_eff
RSGC1-F03	942 ± 196^[17]	L/T_eff
V398 Cassiopeiae (HD 240275)	941^[30]	L/T_eff
IRC +60342	940^[30]	L/T_eff
ψ¹ Aurigae	934^[30]	L/T_eff
GX Monocerotis	931^[61]	L/T_eff
V645 Cephei	920^[30]	L/T_eff
S Cassiopeiae	920^[61]	L/T_eff	One of the coolest known stars, at an effective temperature of 1800 K (1500 °C).
NV Aurigae (IRC +50137)	918^[61]	L/T_eff
Stephenson 2 DFK 5	911 ± 182^[17]	L/T_eff
UY Scuti	909^[30]	L/T_eff	Initially reported 1,708 `R`_☉, making it the largest star, a 2023 measurement put the radius at a smaller value of 909 `R`_☉ based on the multimessenger monitoring of supernovae.^[30]
NR Vulpeculae	908^[30] – 923+62 −50^[32]	L/T_eff
KU Andromedae (IRC +40004)	900^[62] – 1,044 ^[61]	L/T_eff
V774 Sagittarii	889^[30]	L/T_eff
V923 Centauri	881^[30]	L/T_eff
IRAS 20341+4047	880^[30]	L/T_eff
V540 Sagittarii	880^[30]	L/T_eff
V386 Cephei	879^[30]	L/T_eff
Trumpler 27-1 (CD-33 12241)	876+5 −12^[35]	?
T Lyrae	876^[61]	L/T_eff
TYC 3996-552-2	870^[30]	L/T_eff
V1300 Aquilae (IRC −10529)	858^[62]–1,059 ^[61]	L/T_eff
V1417 Aquilae	866^[63]	L/T_eff
Westerlund 1 W20 (Westerlund 1 BKS D)	858±48^[33]	L/T_eff
FX Serpentis	857^[50]	L/T_eff
AZ Cygni	856+20 −14 – 927+21 −15^[24]	AD	Estimated based on data from the CHARA array. Another radii of 890+21 −15 `R`_☉ (2014), 895+21 −15 `R`_☉ (2015) and 890+21 −15 `R`_☉ (2016) are calculated based on the same data.^[24]
V348 Velorum	855^[30]	L/T_eff
Stephenson 2 DFK 3	965 ± 208^[17]	L/T_eff
BI Cygni	852+12 −9 – 908+12 −10^[24]	AD
TW Carinae	835^[30]	L/T_eff
V358 Cassiopeiae	835^[30]	L/T_eff
VLH96 A	833^[64]	L/T_eff
DO 26226	826^[30]	L/T_eff
HD 155737	823^[30]	L/T_eff
6 Geminorum	821^[24]	L/T_eff
RW Leonis Minoris	820^[65] – 1,028^[61]	L/T_eff
HaroChavira 2	813^[47]	L/T_eff
HD 300933 A	806^[30]	L/T_eff
[W61c] R 53	801^[30]	L/T_eff
U Arietis	801±205^[66]	AD
RT Ophiuchi	801±217^[66]	AD
HD 95687	797^[30]	L/T_eff
BO Carinae	790±158^[15]	L/T_eff
HD 62745	790^[30]	L/T_eff
WX Piscium	790^[67] – 1,044^[61]	L/T_eff
VR5–7	775 ± 65^[68]	L/T_eff
T Cancri	770^[50]	L/T_eff
V Cygni	770^[63]	L/T_eff
CL Carinae	770^[30]	L/T_eff
RS Persei	770±30,^[69] 775+110 −85^[32]	AD
V355 Cephei	770±154^[15] – 790^[30]	L/T_eff
BD+63 3	770^[30]	L/T_eff
BD+63 270	769^[30]	L/T_eff
V644 Cephei	765^[30]	L/T_eff
BM VIII 11	754^[30]	L/T_eff
[SLN74] 2130	752^[30]	L/T_eff
IRAS 10176-5802	751.2+0.4 −0.6^[35]–(793+281 −152–849+172 −133)^[57]	L/T_eff	Lower value based on the GSP Phot-Aeneas library using BR/RP spectra in Gaia DR3. Higher values based on the Gaia DR3 effective temperature and the luminosity of Levesque et al. (2005) and that of Messineo & Brown (2019).
HD 303250	750±150^[15]	L/T_eff
R Leporis (Hind's Crimson Star)	750^[70]	AD	Size range from 645 to 860 `R`_☉.
V384 Persei	750^[62] – 937^[61]	L/T_eff
V466 Persei	750^[65]	L/T_eff
V Coronae Borealis	749^[62]	L/T_eff
GY Aquilae	748^[23] – 920^[71]	AD
TT Centauri	744^[61]	L/T_eff
UU Pegasi	742±193^[66]	AD
IM Cassiopeiae	740^[30]	L/T_eff
GY Camelopardalis	736^[62]	L/T_eff
RSGC3-S3	735 ± 151^[17]	L/T_eff
R Andromedae	733^[62]	L/T_eff
Stephenson 2 DFK 10	730^[17]	L/T_eff
V1259 Orionis	729^[56]	L/T_eff
RSGC3-S15	728 ± 138^[17]	L/T_eff
HD 105563 A	723^[30]	L/T_eff
Westerlund 1 W75 (Westerlund 1 BKS E)	722±36^[33]	L/T_eff
V1111 Ophiuchi (IRC +10365)	721^[62] – 902^[61]	L/T_eff
XX Persei	718+80 −56^[32]	AD	Another study from the same author estimates 681+12 −9 R_☉.^[24]
AI Volantis	717^[62]	L/T_eff
RX Telescopii	716^[30]	L/T_eff
V Camelopardalis	716±185^[66]	AD
CD-61 3575	716^[30]	L/T_eff
S Cephei	715^[50]	L/T_eff
AS Cephei	713^[30]	L/T_eff
V770 Cassiopeiae (BD+60 299)	713^[30]	L/T_eff
AZ Cephei	712^[30]	L/T_eff
MZ Puppis	708^[30]	L/T_eff
GP Cassiopeiae	707^[30] – 771.74+0.23 −0.86^[35]	L/T_eff
GCIRS 12N	703 ± 107^[68]	L/T_eff
V528 Carinae	700±140^[15]	L/T_eff
The following well-known stars are listed for the purpose of comparison.
Antares (α Scorpii A)	680^[72]	AD	Fourteenth brightest star in the night sky.^[73] Widely recognised as being among the largest known stars.^[26]
Betelgeuse (α Orionis)	640,^[74] 764+116 −62,^[75] 782 ± 55^[76]	AD & SEIS	Tenth brightest star in the night sky.^[73] Widely recognised as being among the largest known stars,^[26] radius decreased to ~500 `R`_☉ during the 2020 great dimming event.^[77]
R Horologii	635^[62]	L/T_eff	A red giant star with one of the largest ranges in brightness known of stars in the night sky visible to the unaided eye. Despite its large radius, it is less massive than the Sun.
119 Tauri (CE Tauri, Ruby Star)	587 – 593^[78]	AD
ρ Cassiopeiae	564±67 – 700±112^[79]	AD	A yellow hypergiant star, similar to V382 Carinae, that is also visble to the naked eye.
CW Leonis	560^[80]	L/T_eff	The nearest carbon star.
V509 Cassiopeiae	511±112^[42]	AD	A variable yellow hypergiant whose size varied from around 680 `R`_☉ in 1950–1970 to 910 `R`_☉ in 1977, and later decreased to 390 `R`_☉ in the 1990s.^[81]
V382 Carinae (x Carinae)	485 ± 56^[82]	L/T_eff	A yellow hypergiant, one of the rarest types of stars.
V838 Monocerotis	464^[83]	L/T_eff	During the 2002 Red Nova, the star's radius may have increased up to 3,190 `R`_☉.^[84]
Pistol Star (V4647 Sagittarii)	420^[85]	L/T_eff	One of the most luminous stars known.
La Superba (Y Canum Venaticorum)	344^[86]	L/T_eff
Mira (ο Ceti A)	332–402^[87]	AD	Prototype of the Mira variables.
Orbit of Mars	322–323.1^[8]^[b]		Reported for reference
R Doradus	298±21^[88]	AD	The extrasolar star with the largest apparent size.
Rasalgethi (α Herculis A)	284±60 (264–303)^[89]	L/T_eff
Cygnus OB2#12	246^[90]	?	One of the most massive and luminous stars known.
Orbit of Earth (~1 AU)	214^[8]^[b]		Reported for reference
Suhail (λ Velorum)	211±6^[91]	AD
Wezen (δ Canis Majoris)	188^[92]	L/T_eff	Thirty-sixth brightest star in the night sky.^[73]
Enif (ε Pegasi)	178^[92]	L/T_eff
Orbit of Venus	158.6^[8]^[b]		Reported for reference
η Carinae A	128 – 742^[93]	OD	During the 1843 Great Eruption, the star's radius may have increased up to 4,319–6,032 `R`_☉.^[94]
Deneb (α Cygni)	107^[95]^[g] – 203±17^[96]	AD & ?	Eighteenth brightest star in the night sky.^[73]
Orbit of Mercury	82.9–84.6^[8]^[b]		Reported for reference
Rigel (β Orionis A)	74.1+6.1 −7.3^[97]	AD	Seventh brightest star in the night sky.
Canopus (α Carinae)	73.3^[98]	AD	Second brightest star in the night sky.
Gacrux (γ Crucis)	73^[99]	L/T_eff	Twenty-sixth brightest star in the night sky.
Polaris (α Ursae Minoris)	46.27±0.42^[100]	AD	The current star in the North Pole. It is a Classical Cepheid variable, and the brightest example of its class.
Aldebaran (α Tauri)	45.1±0.1^[101]	AD	Fourteenth brightest star in the night sky.
Arcturus (α Boötis)	25.4 ± 0.2^[102]	AD	This is the nearest red giant to the Earth, and the fourth brightest star in the night sky.
Pollux (β Geminorum)	9.06 ± 0.03^[97]	AD	The nearest giant star to the Earth.
Spica (α Virginis A)	7.47±0.54^[103]		One of the nearest supernova candidates and the sixteenth-brightest star in the night sky.
Regulus (α Leonis A)	4.16 × 3.14^[104]		The nearest B-type star to the Earth.
Vega (α Lyrae)	2.726±0.006 × 2.418±0.012^[105]	AD	Fifth brightest star in the night sky.^[73]
Altair (α Aquilae)	2.01 × 1.57^[106]		Twelfth brightest star in the night sky.
Sirius (α Canis Majoris A)	1.713^[107]	AD	The brightest star in the night sky.
Rigil Kentaurus (α Centauri A)	1.2175^[108]	AD	Third brightest star in the night sky.
Sun	1		The largest object in the Solar System.

Magellanic Clouds

List of the largest known stars in the Magellanic Clouds
Star name	Solar radii (Sun = 1)	Galaxy	Method^[a]	Notes
WOH G64	1,540^[9]^[10]^[11]^[12]^[13] ± 77^[9]	Large Magellanic Cloud	L/T_eff	Surrounded by a large torus-shaped dust envelope.^[109]^[110] The largest known star with a well-defined radius.^[9]^[10]^[14]^[11]
HV 888	1,477^[111]–1,584^[12]	Large Magellanic Cloud	L/T_eff
HD 269551 A	1,439^[112]	Large Magellanic Cloud	L/T_eff
HV 12463	1,420^[112]	Large Magellanic Cloud	L/T_eff
IRAS 05280–6910	1,367^[113]	Large Magellanic Cloud	L/T_eff	The most reddened object in the Large Magellanic Cloud.^[12]
MSX LMC 597	1,278^[114]–1,444^[12]	Large Magellanic Cloud	L/T_eff
OGLE BRIGHT-LMC-LPV-52	1,275^[112]–1,384^[114]	Large Magellanic Cloud
HV 2834	1,253^[114]	Large Magellanic Cloud	L/T_eff
LMC 145013	1,243^[112]	Large Magellanic Cloud	L/T_eff
IRAS 05346-6949	1,211^[115]	Large Magellanic Cloud	L/T_eff	It has an estimated mass-loss rate of 0.0017 `M`_☉ (566 Earths) per year, the highest for any star.^[115]
HV 5618	1,163^[112]	Large Magellanic Cloud	L/T_eff
HV 2242	1,160^[116] – 1,180^[112]	Large Magellanic Cloud	L/T_eff
LMC 25320	1,156^[112]	Large Magellanic Cloud	L/T_eff
SMC 18592	1,129^[112]	Small Magellanic Cloud	L/T_eff
MSX SMC 018	1,119^[115]	Small Magellanic Cloud	L/T_eff
LMC252	1,117^[112]–1,164^[114]	Large Magellanic Cloud
LMC045	1,112^[112]	Large Magellanic Cloud	L/T_eff
SP77 21-12	1,103^[112]	Large Magellanic Cloud	L/T_eff
MSX LMC 810	1,104^[114]	Large Magellanic Cloud	L/T_eff
WOH S338	1,100^[116]	Large Magellanic Cloud	L/T_eff
LMC 136042	1,092^[112]	Large Magellanic Cloud	L/T_eff
LMC 175188	1,090^[112]–1,317^[114]	Large Magellanic Cloud
IRAS 04516-6902	1,085^[113]	Large Magellanic Cloud	L/T_eff
WOH S274	1,071^[112]	Large Magellanic Cloud	L/T_eff
[W60] D44	1,063^[112]	Large Magellanic Cloud	L/T_eff
HV 12233	1,057^[112]	Large Magellanic Cloud	L/T_eff
MSX LMC 589	1,051^[114]	Large Magellanic Cloud	L/T_eff
MSX LMC 947	1,050^[114]	Large Magellanic Cloud	L/T_eff
LMC 144217	1,039^[112]	Large Magellanic Cloud
SP77 31-18	1,038^[112]	Large Magellanic Cloud	L/T_eff
IRAS 05402-6956	1,032^[113]	Large Magellanic Cloud	L/T_eff
IRAS 04509-6922	1,027^[113]–1,187^[114]	Large Magellanic Cloud	L/T_eff
HV 2255	1,027^[112]–1,236^[114]	Large Magellanic Cloud
TRM 36	1,019^[112]	Large Magellanic Cloud	L/T_eff
LMC 175549	1,005^[112]	Large Magellanic Cloud	L/T_eff
TRM 89	1,004^[112]–1,526^[114]	Large Magellanic Cloud
B90 (WOH S264)	1000+70 −80 – 1,210^[117]	Large Magellanic Cloud	L/T_eff	Has an unusually high metallicity and velocity.^[117] Often referred to as its SIMBAD designation [W60] B90. Discrepancy in radius is caused by a potential underestimation of the effective temperature measured from the Titanium(II) oxide bands.
HV 2450	1,000+2 −1^[118]–1,071^[118]	Large Magellanic Cloud	L/T_eff	A yellow hypergiant.
LMC 149767	994^[112]	Large Magellanic Cloud	L/T_eff
UCAC2 2674864 (HV 2834)	990+115 −100^[10]	Large Magellanic Cloud	L/T_eff
HV 996	988^[112]–1,176^[114]	Large Magellanic Cloud
W61 8–88	986^[112]	Large Magellanic Cloud	L/T_eff
HV 2362	982^[112] – 1,030^[116]	Large Magellanic Cloud	L/T_eff
MG73 59	979^[119]	Large Magellanic Cloud	L/T_eff	A yellow supergiant.
HD 268757	979^[119]	Large Magellanic Cloud	L/T_eff	A G8 yellow hypergiant.
SMC 56389	976^[112]	Small Magellanic Cloud	L/T_eff
LMC 136404	974^[112]	Large Magellanic Cloud	L/T_eff
SP77 46-32	973^[112]–1,133^[114]	Large Magellanic Cloud
HV 2084	967^[112]–1,083^[114]	Small Magellanic Cloud
WOH S74	965^[112]–1,014^[114]	Large Magellanic Cloud	L/T_eff
SMC 10889	963^[112]	Small Magellanic Cloud	L/T_eff
TRM 67	951^[112]	Large Magellanic Cloud	L/T_eff
LHA 120-S 26	951^[112]	Large Magellanic Cloud	L/T_eff
LMC 139413	951^[112]	Large Magellanic Cloud	L/T_eff
TRM 87	947^[112]	Large Magellanic Cloud	L/T_eff
LMC 148035	947^[112]	Large Magellanic Cloud	L/T_eff
HV 12802	946^[112]–1,377^[114]	Large Magellanic Cloud
SMC 018136	945^[112]	Small Magellanic Cloud	L/T_eff
LMC 142202	943^[112]	Large Magellanic Cloud	L/T_eff
LMC 147199	939^[112] – 990^[116]	Large Magellanic Cloud	L/T_eff
SP77 37-24	936^[112]	Large Magellanic Cloud	L/T_eff
LMC 148381	932^[112]	Large Magellanic Cloud	L/T_eff
LMC 23095	926^[114] – 1,280^[112]	Large Magellanic Cloud	L/T_eff
SP77 31-16	923±28^[118]	Large Magellanic Cloud	L/T_eff	A yellow hypergiant.
LMC 170452	920^[112]	Large Magellanic Cloud	L/T_eff
SP77 44-5	918^[112]	Large Magellanic Cloud	L/T_eff
LMC 66778	915^[112] – 990^[116]	Large Magellanic Cloud	L/T_eff
NGC371 R20	913^[120]	Small Magellanic Cloud	L/T_eff
LMC 150040	911^[112]	Large Magellanic Cloud	L/T_eff
HV 2236	911^[112]–971^[114]	Large Magellanic Cloud	L/T_eff
TRM 108	906^[112]	Large Magellanic Cloud	L/T_eff
LMC 169142	902^[112]	Large Magellanic Cloud	L/T_eff
WOH S457	902±45^[121]	Large Magellanic Cloud	L/T_eff
IRAS 04498-6842 (LI-LMC 60)	898^[113] – 1,137^[114] – 1,765,^[12] 1,224^[112]	Large Magellanic Cloud	L/T_eff	Lower value derived from fitting models that assume the star's effective temperature to be 3,400 K. Higher value based on the measured effective temperature from van Loon et al. (2005). A newer paper estimates parameters that would result in a radius of 1,765 `R`_☉.^[12]
LMC 135720	898^[112]	Large Magellanic Cloud	L/T_eff
SMC 81961	892^[112]	Small Magellanic Cloud	L/T_eff
SP77 44-19	891^[112]–1,297^[114]	Large Magellanic Cloud	L/T_eff
SP77 45–49	890^[112]	Large Magellanic Cloud	L/T_eff
LMC 175464	892^[114]–982^[112]	Large Magellanic Cloud
SMC 49478	888^[112]	Small Magellanic Cloud	L/T_eff
HV 12185	890+55 −65^[10]	Large Magellanic Cloud	L/T_eff
SP77 45–53	885^[114]–981^[112]	Large Magellanic Cloud
LMC 170079	882^[112]	Large Magellanic Cloud	L/T_eff
SMC 5092	880^[112]	Small Magellanic Cloud	L/T_eff
HV 12793	880+45 −65^[10]	Large Magellanic Cloud	L/T_eff
W61 21–22	877^[112]	Large Magellanic Cloud	L/T_eff
SP77 35-1	877^[112]	Large Magellanic Cloud	L/T_eff
UCAC3 43-23216	873^[112]	Large Magellanic Cloud	L/T_eff
HV 11423	872^[112]	Small Magellanic Cloud	L/T_eff
WOH S57	875+70 −60^[10]	Large Magellanic Cloud	L/T_eff
SP77 53-3	870^[112]	Large Magellanic Cloud	L/T_eff
SP77 36-14	870^[112]	Large Magellanic Cloud	L/T_eff
SP77 31-19	870^[112]	Large Magellanic Cloud	L/T_eff
LMC 158646	865^[112]	Large Magellanic Cloud	L/T_eff
SP77 31-20	864^[112]	Large Magellanic Cloud	L/T_eff
LMC 113364	864^[112]	Large Magellanic Cloud	L/T_eff
SMC 83202	864^[112]	Small Magellanic Cloud	L/T_eff
LMC 175746	863^[112]	Large Magellanic Cloud	L/T_eff
LMC207	863^[112]	Large Magellanic Cloud	L/T_eff
SP77 29-8	858^[112]	Large Magellanic Cloud	L/T_eff
SP77 54-38	859^[114]–911^[112]	Large Magellanic Cloud
LMC 174714	855^[112]–965^[114]	Large Magellanic Cloud
LMC 176135	854^[112]	Large Magellanic Cloud	L/T_eff
LMC178	845^[112]	Large Magellanic Cloud	L/T_eff
SP77 31-26	845^[112]	Large Magellanic Cloud	L/T_eff
LMC 106201	844^[112]	Large Magellanic Cloud	L/T_eff
SP77 48-13	838^[112]	Large Magellanic Cloud	L/T_eff
MSX LMC 1318	837^[112]	Large Magellanic Cloud	L/T_eff
SP77 28-13	835^[112]	Large Magellanic Cloud	L/T_eff
LMC 143898	833^[112]	Large Magellanic Cloud	L/T_eff
TYC 9161-866-1	833^[112]	Large Magellanic Cloud	L/T_eff
SMC 59803	829^[112]	Small Magellanic Cloud	L/T_eff
LMC 157401	828^[112]	Large Magellanic Cloud	L/T_eff
SP77 39-22	828^[112]	Large Magellanic Cloud	L/T_eff
WOH S52	828^[112]	Large Magellanic Cloud	L/T_eff
SP77 30-22	826^[112]	Large Magellanic Cloud	L/T_eff
LMC 145728	826^[112]	Large Magellanic Cloud	L/T_eff
LMC 169049	825^[112]	Large Magellanic Cloud	L/T_eff
SP77 46-34	825^[112]	Large Magellanic Cloud	L/T_eff
LMC 177997	825^[114]–867^[112]	Large Magellanic Cloud
SP77 28-2	825±60^[10]	Large Magellanic Cloud	L/T_eff
SP77 22-9	823^[112] – 850^[116]	Large Magellanic Cloud	L/T_eff
Z Doradus	824±108^[121]–956^[114]	Large Magellanic Cloud	L/T_eff
WOH S421	822^[112]–840^[114]	Large Magellanic Cloud
LMC 72727	822^[112]	Large Magellanic Cloud	L/T_eff
SP77 37-28	821^[112]	Large Magellanic Cloud	L/T_eff
MSX LMC 575	816^[112]–933^[114]	Large Magellanic Cloud
LMC 143035	815^[112]	Large Magellanic Cloud	L/T_eff
WOH S49	815^[112]	Large Magellanic Cloud	L/T_eff
SP77 52-28	812^[112]	Large Magellanic Cloud	L/T_eff
SHV 0520422-693821	808^[112]	Large Magellanic Cloud	L/T_eff
HD 268850	808^[114]–898^[112]	Large Magellanic Cloud
SMC 20133	809^[114]–835^[112]	Small Magellanic Cloud
SMC 25888	804^[112]	Small Magellanic Cloud	L/T_eff
SP77 55-20	803^[112]	Large Magellanic Cloud	L/T_eff
PGMW 1058	800^[112]	Large Magellanic Cloud	L/T_eff
LMC 145112	798^[112]	Large Magellanic Cloud	L/T_eff
SMC 47757	795^[112]	Small Magellanic Cloud	L/T_eff
LMC 175709	794^[112]	Large Magellanic Cloud	L/T_eff
SMC 46497	794^[112]	Small Magellanic Cloud	L/T_eff
WOH S60	789^[112]	Large Magellanic Cloud	L/T_eff
WOH S102	789^[112]	Large Magellanic Cloud	L/T_eff
LMC 164709	787^[112]	Large Magellanic Cloud	L/T_eff
SP77 31-28	787^[112]	Large Magellanic Cloud	L/T_eff
TRM 73	787^[114]–816^[112]	Large Magellanic Cloud
SP77 31-21	784^[112]	Large Magellanic Cloud	L/T_eff
SMC 8930	784^[112]	Small Magellanic Cloud	L/T_eff
PMMR 62	784^[112]	Small Magellanic Cloud	L/T_eff
SP77 46-31	782^[112]	Large Magellanic Cloud	L/T_eff
LMC211	780^[112]	Large Magellanic Cloud	L/T_eff
LMC 140403	778^[112]	Large Magellanic Cloud	L/T_eff
LMC 134383	778^[112]–803^[114]	Large Magellanic Cloud	L/T_eff
SP77 47-11	778^[112]	Large Magellanic Cloud	L/T_eff
SP77 40-7	778^[112] – 810^[116]	Large Magellanic Cloud	L/T_eff
W61 19–24	780+50 −70^[10]	Large Magellanic Cloud	L/T_eff
WOH S28	780^[116]	Large Magellanic Cloud	L/T_eff
LMC 141568	776^[112]	Large Magellanic Cloud	L/T_eff
SP77 51-2	776^[112]	Large Magellanic Cloud	L/T_eff
SP77 31–43	773^[112]	Large Magellanic Cloud	L/T_eff
MSX LMC 833	773^[112]–849^[114]	Large Magellanic Cloud
SP77 52-32	772^[112]	Large Magellanic Cloud	L/T_eff
SP77 22-10	767^[112]	Large Magellanic Cloud	L/T_eff
SP77 48-6	768^[122]	Large Magellanic Cloud	L/T_eff
SMC 12322	765^[112]	Small Magellanic Cloud	L/T_eff
WOH S517	764^[112]	Large Magellanic Cloud	L/T_eff
WOH S183	763^[112]	Large Magellanic Cloud	L/T_eff
LMC256	762^[112]	Large Magellanic Cloud	L/T_eff
LMC 154311	762^[112]	Large Magellanic Cloud	L/T_eff
LMC 119219	762^[112]	Large Magellanic Cloud	L/T_eff
WOH S452	762±275^[121]	Large Magellanic Cloud	L/T_eff
MSX SMC 024	761^[114]	Large Magellanic Cloud	L/T_eff
WOH S282	758^[112]	Large Magellanic Cloud	L/T_eff
LMC 64048	758^[112]	Large Magellanic Cloud	L/T_eff
PGMW 3160	758^[112]	Large Magellanic Cloud	L/T_eff
WOH S438	757±211^[121]	Large Magellanic Cloud	L/T_eff
LMC 61753	755^[112]	Large Magellanic Cloud	L/T_eff
LMC 140296	754^[112]	Large Magellanic Cloud	L/T_eff
WOH S478	753^[112]	Large Magellanic Cloud	L/T_eff
LMC 139027	751^[112] – 790^[116]	Large Magellanic Cloud	L/T_eff
SP77 45-16	749^[112] – 800^[116]	Large Magellanic Cloud	L/T_eff
SP77 37-20	749^[112]	Large Magellanic Cloud	L/T_eff
SP77 54-27	750^[116] – 758^[112] – 800^[116]	Large Magellanic Cloud	L/T_eff
LMC 155529	747^[112]	Large Magellanic Cloud	L/T_eff
LMC 143877	746^[112]	Large Magellanic Cloud	L/T_eff
SMC 64663	745^[112]	Small Magellanic Cloud	L/T_eff
WOH G302	745^[112]	Large Magellanic Cloud	L/T_eff
TRM 65	743^[112]	Large Magellanic Cloud	L/T_eff
HV 12149	741^[112]–767^[114]	Small Magellanic Cloud
SMC 50840	740^[112]	Small Magellanic Cloud	L/T_eff
SMC 46662	740^[112]–874^[114]	Small Magellanic Cloud
SP77 29-11	738^[112]	Large Magellanic Cloud	L/T_eff
SMC 30616	737^[112]	Small Magellanic Cloud	L/T_eff
LMC 162635	736^[112]	Large Magellanic Cloud	L/T_eff
SP77 39-17	736^[112] – 760^[116]	Large Magellanic Cloud	L/T_eff
LMC 163466	734^[112]	Large Magellanic Cloud	L/T_eff
HV 2310	734^[114]	Large Magellanic Cloud	L/T_eff
HD 269723	734±17,^[118] 814^[119]–829^[122]	Large Magellanic Cloud	L/T_eff	A yellow hypergiant.
SP77 44-17	732^[112]	Large Magellanic Cloud	L/T_eff
SP77 38-5a	732^[112]	Large Magellanic Cloud	L/T_eff
LMC 67982	730^[112]	Large Magellanic Cloud	L/T_eff
LHA 120-S 129	730^[112]	Large Magellanic Cloud	L/T_eff
PMMR 64	730+75 −65^[10]	Small Magellanic Cloud	L/T_eff
SP77 51-15	727^[112]	Large Magellanic Cloud	L/T_eff
LMC 168757	725^[112]	Large Magellanic Cloud	L/T_eff
LMC 163007	725^[112]	Large Magellanic Cloud	L/T_eff
W61 8–14	724^[112]	Large Magellanic Cloud	L/T_eff
IRAS 05425-6914	724^[112]	Large Magellanic Cloud	L/T_eff
SMC 55188	724^[112]	Small Magellanic Cloud	L/T_eff
SP77 44-13	721^[112]	Large Magellanic Cloud	L/T_eff
MSX LMC 905	719^[112]	Large Magellanic Cloud	L/T_eff
LMC 147928	719^[112]	Large Magellanic Cloud	L/T_eff
LH 43-15	719^[112] – 740^[116]	Large Magellanic Cloud	L/T_eff
PMMR 116	717^[122]	Small Magellanic Cloud	L/T_eff
LMC 123778	715^[112]	Large Magellanic Cloud	L/T_eff
WOH S314	714^[112]	Large Magellanic Cloud	L/T_eff
SP77 61-23	713^[112]	Large Magellanic Cloud	L/T_eff
WOH S230	713^[112]	Large Magellanic Cloud	L/T_eff
LMC 150396	710^[112]	Large Magellanic Cloud	L/T_eff
SP77 48-17	709^[112]	Large Magellanic Cloud	L/T_eff
LMC 165242	707^[112]	Large Magellanic Cloud	L/T_eff
SP77 51-19	707^[112]	Large Magellanic Cloud	L/T_eff
LMC 170539	707^[112]	Large Magellanic Cloud	L/T_eff
LMC 154729	705^[112]	Large Magellanic Cloud	L/T_eff
OGLE BRIGHT-LMC-LPV-101	703^[112]	Large Magellanic Cloud	L/T_eff
MSX SMC 055	702^[120]–1,557+215 −130^[114]	Small Magellanic Cloud	L/T_eff	A super-AGB candidate.
LMC 168290	702^[112]	Large Magellanic Cloud	L/T_eff
LMC180	702^[112]	Large Magellanic Cloud	L/T_eff
SP77 45-2	702^[112]	Large Magellanic Cloud	L/T_eff
SP77 48-6	700+29 −28^[118]	Large Magellanic Cloud	L/T_eff	A yellow hypergiant.
The following well-known stars are listed for the purpose of comparison.
HV 2112	675 – 1,193^[123]	Small Magellanic Cloud	L/T_eff	It has been previously considered to be a possible Thorne–Żytkow object.^[123]
HV 11417	673^[114]–798^[112]	Small Magellanic Cloud	L/T_eff	Candidate Thorne-Zytkow object.^[123]
HD 269953	647^[119]–720^[122]	Large Magellanic Cloud	L/T_eff	A yellow hypergiant.
HD 33579	471^[122]	Large Magellanic Cloud	L/T_eff	The brightest star in the Large Magellanic Cloud.
S Doradus	100^[124]	Large Magellanic Cloud	L/T_eff	A luminous blue variable in the S Doradus instability strip.
HD 37974	99^[125]	Large Magellanic Cloud	L/T_eff	An unusual blue hypergiant with a large dusty disk.^[125]
R136a1	42.7+1.6 −0.9^[126]	Large Magellanic Cloud	L/T_eff	One of the most luminous and most massive stars.
BAT 99-98	37.5^[127]	Large Magellanic Cloud	L/T_eff	One of the most luminous and most massive stars.
HD 5980 A	24^[128]	Small Magellanic Cloud	L/T_eff	A luminous blue variable and one of the most luminous stars.

Andromeda (M31) and Triangulum (M33) galaxies

List of the largest known stars in Andromeda and Triangulum galaxies
Star name	Solar radii (Sun = 1)	Galaxy	Method^[a]	Notes
LGGS J013339.28+303118.8	1,566^[129]	Triangulum Galaxy	L/T_eff
WOH G64 (For comparison)	1,540^[9]^[10]^[11]^[12]^[13] ± 77^[9]	Large Magellanic Cloud	L/T_eff	Located in the Large Magellanic Cloud. The largest known star with a well-defined radius.^[9]^[10]^[14]^[11]
LGGS J004428.48+415130.9	1,410^[130]	Andromeda Galaxy	L/T_eff
LGGS J013418.56+303808.6	1,363^[129]	Triangulum Galaxy	L/T_eff
LGGS J013414.27+303417.7	1,342^[129]–1,479^[112]	Triangulum Galaxy	L/T_eff
LGGS J004514.91+413735.0	1,324^[112]	Andromeda Galaxy	L/T_eff
LGGS J004125.23+411208.9	1,302^[112]	Andromeda Galaxy	L/T_eff
LGGS J013350.62+303230.3	1,283^[112]	Triangulum Galaxy	L/T_eff
LGGS J004312.43+413747.1	1,279^[112]	Andromeda Galaxy	L/T_eff
LGGS J003951.33+405303.7	1,272^[112]	Andromeda Galaxy	L/T_eff
LGGS J013416.52+305155.4	1,227^[112]	Triangulum Galaxy	L/T_eff
LGGS J004416.83+411933.2	1,209^[112]	Andromeda Galaxy	L/T_eff
LGGS J004531.13+414825.7	1,201^[112]	Andromeda Galaxy	L/T_eff
2MASS J01343365+3046547	1,196^[112]	Triangulum Galaxy	L/T_eff
LGGS J013409.63+303907.6	1,182^[112]	Triangulum Galaxy	L/T_eff
LGGS J004133.18+411217.2	1,180^[112]	Andromeda Galaxy	L/T_eff
LGGS J004455.90+413035.2	1,172^[112]	Andromeda Galaxy	L/T_eff
LGGS J013352.96+303816.0	1,163^[112]	Andromeda Galaxy	L/T_eff
LGGS J004047.22+404445.5	1,162^[112]	Andromeda Galaxy	L/T_eff
LGGS J004254.18+414033.6	1,154^[112]	Andromeda Galaxy	L/T_eff
LGGS J004428.48+415130.9	1,130^[112]	Andromeda Galaxy	L/T_eff
LGGS J013414.27+303417.7	1,129^[129]	Triangulum Galaxy	L/T_eff
LGGS J004035.08+404522.3	1,122^[112]	Andromeda Galaxy	L/T_eff
LGGS J013341.98+302102.0	1,119^[112]	Triangulum Galaxy	L/T_eff
LGGS J013307.37+304543.2	1,119^[112]	Triangulum Galaxy	L/T_eff
LGGS J004218.33+412633.9	1,111^[112]	Andromeda Galaxy	L/T_eff
LGGS J004102.54+403426.5	1,108^[112]	Andromeda Galaxy	L/T_eff
LGGS J013335.90+303344.5	1,104^[112]	Triangulum Galaxy	L/T_eff
LGGS J013358.54+303419.9	1,103^[112]	Triangulum Galaxy	L/T_eff
LGGS J013414.49+303511.6	1,102^[112]	Triangulum Galaxy	L/T_eff
LGGS J013336.64+303532.3	1,102^[112]–1,408^[129]	Triangulum Galaxy	L/T_eff
LGGS J004259.34+413726.0	1,094^[112]	Andromeda Galaxy	L/T_eff
LGGS J004509.98+414627.5	1,089^[112]	Andromeda Galaxy	L/T_eff
LGGS J013241.94+302047.5	1,083^[112]	Triangulum Galaxy	L/T_eff
LGGS J004034.74+404459.6	1,078^[112]	Andromeda Galaxy	L/T_eff
LGGS J004059.50+404542.6	1,071^[112]	Andromeda Galaxy	L/T_eff
LGGS J013430.75+303218.8	1,067^[112]	Triangulum Galaxy	L/T_eff
LGGS J013412.27+305314.1	1,063^[112]–1,066^[129]	Triangulum Galaxy	L/T_eff
LGGS J013328.17+304741.5	1,063^[112]	Triangulum Galaxy	L/T_eff
LGGS J004524.97+420727.2	1,059^[112]	Andromeda Galaxy	L/T_eff
LGGS J013233.77+302718.8	1,058^[112]–1,129^[129]	Triangulum Galaxy	L/T_eff
LGGS J004125.72+411212.7	1,058^[112]	Andromeda Galaxy	L/T_eff
LGGS J004114.18+403759.8	1,058^[112]	Andromeda Galaxy	L/T_eff
LGGS J013307.60+304259.0	1,051^[112]	Triangulum Galaxy	L/T_eff
LGGS J004103.67+410211.8	1,047^[112]	Andromeda Galaxy	L/T_eff
LGGS J013305.48+303138.5	1,046^[112]	Triangulum Galaxy	L/T_eff
LGGS J004442.41+412649.5	1,040^[112]	Andromeda Galaxy	L/T_eff
LGGS J013403.87+303753.2	1,040^[112]	Triangulum Galaxy	L/T_eff
LGGS J013351.47+303640.3	1,034^[112]	Triangulum Galaxy	L/T_eff
LGGS J004306.62+413806.2	1,028^[112]	Andromeda Galaxy	L/T_eff
LGGS J013303.54+303201.2	1,027^[112]–1,131^[129]	Triangulum Galaxy	L/T_eff
LGGS J004234.41+405855.9	1,023^[112]	Andromeda Galaxy	L/T_eff
LGGS J004051.31+404421.7	1,022^[112]	Andromeda Galaxy	L/T_eff
LGGS J004031.00+404311.1	1,011^[112]	Andromeda Galaxy	L/T_eff
LGGS J013406.20+303913.6	1,009^[112]	Triangulum Galaxy	L/T_eff
LGGS J013344.10+304425.1	1,007^[112]	Triangulum Galaxy	L/T_eff
LGGS J004307.36+405852.2	1,007^[112]	Andromeda Galaxy	L/T_eff
LGGS J013407.13+303929.5	994^[112]	Triangulum Galaxy	L/T_eff
LGGS J013312.35+303033.9	993^[112]	Triangulum Galaxy	L/T_eff
LGGS J013330.05+303145.9	988^[112]	Triangulum Galaxy	L/T_eff
LGGS J013350.84+304403.1	984^[112]	Triangulum Galaxy	L/T_eff
LGGS J013329.47+301848.3	981^[112]	Triangulum Galaxy	L/T_eff
LGGS J004148.74+410843.0	981^[112]	Andromeda Galaxy	L/T_eff
LGGS J004415.76+411750.7	977^[112]	Andromeda Galaxy	L/T_eff
LGGS J004127.44+411240.7	977^[112]	Andromeda Galaxy	L/T_eff
LGGS J013312.75+303946.1	975^[112]	Triangulum Galaxy	L/T_eff
LGGS J004027.36+410444.9	973^[112]	Andromeda Galaxy	L/T_eff
LGGS J013434.35+302627.3	973^[112]	Triangulum Galaxy	L/T_eff
LGGS J013423.29+305655.0	993^[112]–972^[129]	Triangulum Galaxy	L/T_eff
LGGS J013319.13+303642.5	970^[112]	Triangulum Galaxy	L/T_eff
LGGS J004305.77+410742.5	969^[112]	Andromeda Galaxy	L/T_eff
LGGS J013403.73+304202.4	965^[112]–1,032^[129]	Triangulum Galaxy	L/T_eff
LGGS J004346.10+411138.8	962^[112]	Andromeda Galaxy	L/T_eff
LGGS J004419.20+412343.7	959^[112]	Andromeda Galaxy	L/T_eff
LGGS J013353.91+302641.8	959^[112]–1,008^[129]	Triangulum Galaxy	L/T_eff
LGGS J013315.23+305329.0	958^[112]	Triangulum Galaxy	L/T_eff
LGGS J013315.23+305329.0	956^[129]	Triangulum Galaxy	L/T_eff
LGGS J004138.35+412320.7	954^[112]	Andromeda Galaxy	L/T_eff
LGGS J004419.45+411749.5	950^[112]	Andromeda Galaxy	L/T_eff
LGGS J013413.95+303339.6	948^[112]	Triangulum Galaxy	L/T_eff
LGGS J013336.42+303530.9	947^[112]	Triangulum Galaxy	L/T_eff
LGGS J004047.82+410936.4	943^[112]	Andromeda Galaxy	L/T_eff
LGGS J013258.18+303606.3	943^[112]	Triangulum Galaxy	L/T_eff
LGGS J004447.74+413050.0	938^[112]	Andromeda Galaxy	L/T_eff
2MASS J01343131+3046088	938^[112]	Triangulum Galaxy	L/T_eff
LGGS J004346.18+411515.0	936^[112]	Andromeda Galaxy	L/T_eff
LGGS J004304.62+410348.4	936^[112]	Andromeda Galaxy	L/T_eff
LGGS J004458.28+413154.3	933^[112]	Andromeda Galaxy	L/T_eff
LGGS J004102.82+410422.3	933^[112]	Andromeda Galaxy	L/T_eff
LGGS J013344.33+303636.0	932^[112]	Triangulum Galaxy	L/T_eff
LGGS J004631.49+421133.1	932^[112]	Andromeda Galaxy	L/T_eff
LGGS J013321.44+304045.4	932^[112]–1,015^[129]	Triangulum Galaxy	L/T_eff
LGGS J013358.04+304900.1	931^[112]	Triangulum Galaxy	L/T_eff
LGGS J013314.31+302952.9	1,067^[112]–930^[129]	Triangulum Galaxy	L/T_eff
LGGS J013315.97+303153.7	929^[112]	Triangulum Galaxy	L/T_eff
LGGS J004126.14+403346.5	927^[112]	Andromeda Galaxy	L/T_eff
LGGS J004347.31+411203.6	925^[112]	Andromeda Galaxy	L/T_eff
LGGS J004252.78+405627.5	923^[112]	Andromeda Galaxy	L/T_eff
LGGS J013411.54+303312.6	918^[112]	Triangulum Galaxy	L/T_eff
LGGS J013357.08+303817.8	918^[112]	Triangulum Galaxy	L/T_eff
LGGS J003943.89+402104.6	917^[112]	Andromeda Galaxy	L/T_eff
LGGS J004503.35+413026.3	916^[112]	Andromeda Galaxy	L/T_eff
LGGS J013338.97+303828.9	915^[112]	Triangulum Galaxy	L/T_eff
LGGS J013330.27+303510.6	915^[112]	Triangulum Galaxy	L/T_eff
LGGS J004033.06+404303.1	912^[112]	Andromeda Galaxy	L/T_eff
LGGS J004357.15+411136.6	911^[112]	Andromeda Galaxy	L/T_eff
LGGS J004406.60+411536.6	911^[112]	Andromeda Galaxy	L/T_eff
LGGS J013312.38+302453.2	911^[112]–952^[129]	Triangulum Galaxy	L/T_eff
LGGS J004451.76+420006.0	911^[112]	Andromeda Galaxy	L/T_eff
LGGS J013322.82+301910.9	934^[112]–911^[129]	Triangulum Galaxy	L/T_eff
LGGS J013355.56+304120.9	908^[112]	Triangulum Galaxy	L/T_eff
LGGS J004034.40+403627.4	907^[112]	Andromeda Galaxy	L/T_eff
LGGS J003910.56+402545.6	906^[112]	Andromeda Galaxy	L/T_eff
LGGS J004142.43+411814.1	906^[112]	Andromeda Galaxy	L/T_eff
LGGS J013316.57+303051.9	902^[112]	Triangulum Galaxy	L/T_eff
LGGS J013245.59+303518.7	900^[112]	Triangulum Galaxy	L/T_eff
LGGS J004034.67+404322.5	898^[112]	Andromeda Galaxy	L/T_eff
LGGS J004027.65+405126.7	898^[112]	Andromeda Galaxy	L/T_eff
LGGS J004322.75+411101.8	895^[112]	Andromeda Galaxy	L/T_eff
LGGS J004116.47+410813.7	895^[112]	Andromeda Galaxy	L/T_eff
LGGS J013306.33+303208.2	894^[112]	Triangulum Galaxy	L/T_eff
LGGS J004039.12+404252.3	894^[112]	Andromeda Galaxy	L/T_eff
LGGS J004433.96+415414.8	893^[112]	Andromeda Galaxy	L/T_eff
LGGS J013454.31+304109.8	891^[129]	Triangulum Galaxy	L/T_eff
LGGS J004030.64+404246.2	890^[112]	Andromeda Galaxy	L/T_eff
LGGS J004252.67+413615.2	889^[112]	Andromeda Galaxy	L/T_eff
LGGS J013349.94+302928.8	888^[112]	Triangulum Galaxy	L/T_eff
2MASS J01335010+3039106	886^[112]	Triangulum Galaxy	L/T_eff
LGGS J013357.37+304558.7	886^[112]	Triangulum Galaxy	L/T_eff
LGGS J013338.77+303532.9	885^[112]	Triangulum Galaxy	L/T_eff
LGGS J013359.20+303212.1	884^[112]	Triangulum Galaxy	L/T_eff
LGGS J013340.42+303131.3	880^[112]	Triangulum Galaxy	L/T_eff
LGGS J004511.40+413717.8	880^[112]	Andromeda Galaxy	L/T_eff
LGGS J013352.16+303902.2	880^[112]	Triangulum Galaxy	L/T_eff
LGGS J004219.25+405116.4	880^[112]	Andromeda Galaxy	L/T_eff
LGGS J004331.90+411145.0	880^[112]	Andromeda Galaxy	L/T_eff
2MASS J01333718+3038206	879^[112]	Triangulum Galaxy	L/T_eff
LGGS J013415.42+302816.4	876^[112]	Triangulum Galaxy	L/T_eff
LGGS J013345.01+302105.1	876^[112]	Triangulum Galaxy	L/T_eff
LGGS J004107.23+411636.8	870^[112]	Andromeda Galaxy	L/T_eff
LGGS J013417.83+303356.0	867^[112]	Triangulum Galaxy	L/T_eff
LGGS J004120.25+403838.1	867^[112]	Andromeda Galaxy	L/T_eff
LGGS J004402.38+412114.9	866^[112]	Andromeda Galaxy	L/T_eff
2MASS J01334194+3038565	866^[112]	Triangulum Galaxy	L/T_eff
LGGS J013309.10+303017.8	865^[112]–933^[129]	Triangulum Galaxy	L/T_eff
LGGS J004429.36+412307.8	862^[112]	Andromeda Galaxy	L/T_eff
LGGS J013310.20+303314.4	861^[112]	Triangulum Galaxy	L/T_eff
LGGS J004404.60+412729.8	860^[112]	Andromeda Galaxy	L/T_eff
LGGS J003907.69+402859.5	860^[112]	Andromeda Galaxy	L/T_eff
LGGS J004219.64+412736.1	859^[112]	Andromeda Galaxy	L/T_eff
LGGS J003949.31+402049.1	859^[112]	Andromeda Galaxy	L/T_eff
LGGS J013310.16+302726.3	855^[112]	Triangulum Galaxy	L/T_eff
LGGS J004036.97+403412.4	855^[112]	Andromeda Galaxy	L/T_eff
LGGS J013343.68+304450.7	855^[112]	Triangulum Galaxy	L/T_eff
LGGS J013409.10+303351.8	854^[112]	Triangulum Galaxy	L/T_eff
LGGS J013407.11+303918.7	854^[112]	Triangulum Galaxy	L/T_eff
LGGS J004107.11+411635.6	854^[112]	Andromeda Galaxy	L/T_eff
LGGS J013400.01+304622.2	852^[112]	Triangulum Galaxy	L/T_eff
LGGS J013327.14+303917.4	851^[112]	Andromeda Galaxy	L/T_eff
LGGS J013339.79+304032.2	850^[112]	Triangulum Galaxy	L/T_eff
LGGS J004501.30+413922.5	850^[112]	Andromeda Galaxy	L/T_eff
LGGS J004450.87+412924.3	850^[112]	Andromeda Galaxy	L/T_eff
LGGS J004040.69+405908.1	850^[112]	Andromeda Galaxy	L/T_eff
LGGS J003942.92+402051.1	850^[112]	Andromeda Galaxy	L/T_eff
2MASS J01335092+3040481	850^[112]	Triangulum Galaxy	L/T_eff
LGGS J013315.19+305319.8	847^[112]	Triangulum Galaxy	L/T_eff
LGGS J013416.89+305158.3	845^[112]–920^[129]	Triangulum Galaxy	L/T_eff
LGGS J004415.17+415640.6	845^[112]	Andromeda Galaxy	L/T_eff
LGGS J004424.94+412322.3	844^[112]	Andromeda Galaxy	L/T_eff
LGGS J013331.93+301952.9	838^[112]	Triangulum Galaxy	L/T_eff
LGGS J004406.16+414846.4	836^[112]	Andromeda Galaxy	L/T_eff
LGGS J013445.65+303235.4	835^[112]	Triangulum Galaxy	L/T_eff
LGGS J004109.39+404901.9	834^[112]	Andromeda Galaxy	L/T_eff
LGGS J004423.83+414928.6	833^[112]	Andromeda Galaxy	L/T_eff
LGGS J013242.31+302113.9	833^[129]	Triangulum Galaxy	L/T_eff
LGGS J004030.48+404051.1	833^[112]	Andromeda Galaxy	L/T_eff
LGGS J004118.29+404940.3	832^[112]	Andromeda Galaxy	L/T_eff
LGGS J013414.17+304701.9	831^[112]	Triangulum Galaxy	L/T_eff
LGGS J013328.89+303058.0	831^[112]	Triangulum Galaxy	L/T_eff
LGGS J004107.70+403702.3	831^[112]	Andromeda Galaxy	L/T_eff
LGGS J003925.67+404111.8	831^[112]	Andromeda Galaxy	L/T_eff
LGGS J004306.95+410038.2	826^[112]	Andromeda Galaxy	L/T_eff
LGGS J013408.81+304637.8	826^[112]	Triangulum Galaxy	L/T_eff
LGGS J013345.22+303138.2	826^[112]	Triangulum Galaxy	L/T_eff
LGGS J003950.65+402531.8	825^[112]	Andromeda Galaxy	L/T_eff
LGGS J013427.65+305642.4	825^[129]	Triangulum Galaxy	L/T_eff
LGGS J013500.04+303703.8	823^[112]	Triangulum Galaxy	L/T_eff
LGGS J004108.42+410655.3	822^[112]	Andromeda Galaxy	L/T_eff
LGGS J013340.77+302108.7	821^[112]–820^[129]	Triangulum Galaxy	L/T_eff
LGGS J004458.57+412925.1	821^[112]	Andromeda Galaxy	L/T_eff
LGGS J013309.97+302727.5	973^[112]	Triangulum Galaxy	L/T_eff
LGGS J004124.81+411206.1	819^[112]	Andromeda Galaxy	L/T_eff
LGGS J013401.65+303128.7	819^[112]	Triangulum Galaxy	L/T_eff
LGGS J013455.65+304349.0	816^[112]	Triangulum Galaxy	L/T_eff
LGGS J013310.60+302301.8	816^[112]	Triangulum Galaxy	L/T_eff
LGGS J004544.71+414331.9	815^[112]	Andromeda Galaxy	L/T_eff
LGGS J004119.35+410836.4	813^[112]	Andromeda Galaxy	L/T_eff
LGGS J013436.65+304517.1	814^[112]–812^[129]	Triangulum Galaxy	L/T_eff
LGGS J013301.79+303954.3	812^[112]	Triangulum Galaxy	L/T_eff
LGGS J013328.85+310041.7	810^[112]–909^[129]	Triangulum Galaxy	L/T_eff
LGGS J013401.08+303432.2	809^[112]	Triangulum Galaxy	L/T_eff
LGGS J004036.45+403613.1	808^[112]	Andromeda Galaxy	L/T_eff
LGGS J004521.53+413758.6	807^[112]	Andromeda Galaxy	L/T_eff
LGGS J004432.38+415149.9	807^[112]	Andromeda Galaxy	L/T_eff
LGGS J013306.95+303506.1	807^[129]	Triangulum Galaxy	L/T_eff	Contradictory classification in literature, it has been considered a candidate LBV, a RSG or a BSG.
LGGS J013242.26+302114.1	807^[112]	Triangulum Galaxy	L/T_eff
LGGS J013321.94+304112.0	806^[112]–829^[129]	Triangulum Galaxy	L/T_eff
LGGS J013304.56+303043.2	804^[112]	Triangulum Galaxy	L/T_eff
LGGS J004331.73+414223.0	803^[112]	Andromeda Galaxy	L/T_eff
LGGS J004044.17+410729.0	803^[112]	Andromeda Galaxy	L/T_eff
LGGS J013352.83+305605.2	803^[112]	Triangulum Galaxy	L/T_eff
LGGS J013343.30+303318.9	873^[112]–803^[129]	Triangulum Galaxy	L/T_eff
LGGS J013342.61+303534.7	800^[112]	Triangulum Galaxy	L/T_eff
LGGS J013326.90+310054.2	800^[112]–909^[129]	Triangulum Galaxy	L/T_eff
LGGS J013300.94+303404.3	798^[112]	Triangulum Galaxy	L/T_eff
LGGS J013416.06+303730.0	798^[112]	Triangulum Galaxy	L/T_eff
LGGS J004503.83+413737.0	797^[112]	Andromeda Galaxy	L/T_eff
LGGS J004503.83+413737.0	797^[112]	Andromeda Galaxy	L/T_eff
LGGS J004438.83+415253.0	794^[112]	Andromeda Galaxy	L/T_eff
LGGS J004235.88+405442.2	794^[112]	Andromeda Galaxy	L/T_eff
LGGS J004335.28+410959.7	794^[112]	Andromeda Galaxy	L/T_eff
LGGS J013402.32+303828.4	793^[112]	Triangulum Galaxy	L/T_eff
LGGS J004125.55+405034.8	792^[112]	Andromeda Galaxy	L/T_eff
LGGS J013507.43+304132.6	791^[112]	Triangulum Galaxy	L/T_eff
LGGS J013353.25+303918.7	791^[112]	Triangulum Galaxy	L/T_eff
LGGS J004308.71+410604.5	790^[112]	Andromeda Galaxy	L/T_eff
LGGS J013417.17+304826.6	789^[112]	Triangulum Galaxy	L/T_eff
LGGS J013310.71+302714.9	789^[112]–884^[129]	Triangulum Galaxy	L/T_eff
LGGS J013432.36+304159.0	788^[112]	Triangulum Galaxy	L/T_eff
LGGS J004356.23+414641.8	788^[112]	Andromeda Galaxy	L/T_eff
LGGS J013340.77+302108.7	788^[112]	Triangulum Galaxy	L/T_eff
LGGS J013346.61+304125.4	786^[112]	Triangulum Galaxy	L/T_eff
LGGS J004447.08+412801.7	785^[112]	Andromeda Galaxy	L/T_eff
LGGS J004255.95+404857.5	785^[131]	Andromeda Galaxy	L/T_eff
LGGS J013231.91+302329.1	783^[112]	Triangulum Galaxy	L/T_eff
LGGS J004110.32+410433.4	782^[112]	Andromeda Galaxy	L/T_eff
LGGS J004159.06+405718.7	780^[112]	Andromeda Galaxy	L/T_eff
LGGS J004241.10+413142.3	775^[112]	Andromeda Galaxy	L/T_eff
LGGS J013401.88+303858.3	776^[129]	Triangulum Galaxy	L/T_eff
LGGS J013445.12+305858.9	773^[112]	Triangulum Galaxy	L/T_eff
LGGS J004030.92+404329.3	773^[112]	Andromeda Galaxy	L/T_eff
LGGS J013359.57+303413.5	771^[112]	Triangulum Galaxy	L/T_eff
LGGS J004353.97+411255.6	771^[112]	Andromeda Galaxy	L/T_eff
LGGS J004029.03+403412.6	770^[112]	Andromeda Galaxy	L/T_eff
LGGS J004526.24+420047.5	767^[112]	Andromeda Galaxy	L/T_eff
LGGS J013348.44+302029.8	767^[112]	Triangulum Galaxy	L/T_eff
LGGS J004552.15+421003.5	767^[112]	Andromeda Galaxy	L/T_eff
LGGS J013320.75+303204.8	764^[112]	Triangulum Galaxy	L/T_eff
LGGS J013416.28+303353.5	763^[112]–801^[129]	Triangulum Galaxy	L/T_eff
LGGS J013357.91+303338.9	763^[112]	Triangulum Galaxy	L/T_eff
LGGS J013253.14+303515.3	762^[112]	Triangulum Galaxy	L/T_eff
LGGS J004051.18+403053.4	762^[112]	Andromeda Galaxy	L/T_eff
LGGS J013402.57+303746.3	762^[112]	Triangulum Galaxy	L/T_eff
LGGS J013352.15+304006.4	762^[112]	Triangulum Galaxy	L/T_eff
LGGS J004427.07+415203.0	762^[112]	Andromeda Galaxy	L/T_eff
LGGS J004233.23+405917.0	762^[112]	Andromeda Galaxy	L/T_eff
LGGS J004156.96+405720.8	761^[112]	Andromeda Galaxy	L/T_eff
LGGS J004117.14+410843.7	761^[112]	Andromeda Galaxy	L/T_eff
LGGS J004124.80+411634.7	760, 1,205, 1,240^[131]	Andromeda Galaxy	L/T_eff
LGGS J004109.61+404920.4	761^[112]	Andromeda Galaxy	L/T_eff
LGGS J003930.09+402313.0	759^[112]	Andromeda Galaxy	L/T_eff
LGGS J013324.71+303423.7	758^[112]	Triangulum Galaxy	L/T_eff
LGGS J013317.40+303210.8	758^[112]	Triangulum Galaxy	L/T_eff
LGGS J013411.83+304631.0	756^[112]	Triangulum Galaxy	L/T_eff
LGGS J004417.75+420039.1	755^[112]	Andromeda Galaxy	L/T_eff
LGGS J004454.50+413007.8	755^[112]	Andromeda Galaxy	L/T_eff
LGGS J013348.77+304526.8	754^[112]	Triangulum Galaxy	L/T_eff
LGGS J004019.69+404912.2	754^[112]	Andromeda Galaxy	L/T_eff
LGGS J004340.32+411157.1	753^[112]	Andromeda Galaxy	L/T_eff
LGGS J013304.02+303215.2	753^[112]	Triangulum Galaxy	L/T_eff
LGGS J013409.16+303846.9	752^[112]	Triangulum Galaxy	L/T_eff
LGGS J013459.81+304156.9	751^[112]–765^[129]	Triangulum Galaxy	L/T_eff
LGGS J013334.82+302029.1	751^[112]–930^[129]	Triangulum Galaxy	L/T_eff
LGGS J013400.71+303422.3	750^[112]	Triangulum Galaxy	L/T_eff
LGGS J004224.65+412623.7	749^[112]	Andromeda Galaxy	L/T_eff
LGGS J013414.88+303401.2	749^[112]	Triangulum Galaxy	L/T_eff
LGGS J004343.33+414529.5	749^[112]	Andromeda Galaxy	L/T_eff
LGGS J004034.76+403648.9	749^[112]	Andromeda Galaxy	L/T_eff
LGGS J013353.53+303418.7	749^[112]	Triangulum Galaxy	L/T_eff
LGGS J004501.84+420259.2	747^[112]	Andromeda Galaxy	L/T_eff
LGGS J013409.70+303916.2	744^[112]	Triangulum Galaxy	L/T_eff
LGGS J013345.71+303609.8	744^[112]	Triangulum Galaxy	L/T_eff
LGGS J004342.75+411442.8	743^[112]	Andromeda Galaxy	L/T_eff
LGGS J013333.32+303147.2	741^[112]	Triangulum Galaxy	L/T_eff
LGGS J013338.97+303506.1	741^[112]	Triangulum Galaxy	L/T_eff
LGGS J013303.61+302841.5	741^[112]	Triangulum Galaxy	L/T_eff
LGGS J004201.12+412516.0	737^[112]	Andromeda Galaxy	L/T_eff
LGGS J004341.35+411213.8	734^[112]	Andromeda Galaxy	L/T_eff
LGGS J013438.76+304608.1	734^[112]	Triangulum Galaxy	L/T_eff
LGGS J013402.33+301749.2	734^[112]–786^[129]	Triangulum Galaxy	L/T_eff
2MASS J01334180+3040207	732^[112]	Triangulum Galaxy	L/T_eff
LGGS J013354.32+301724.6	732^[112]–854^[129]	Triangulum Galaxy	L/T_eff
LGGS J013334.23+303400.3	732^[112]	Triangulum Galaxy	L/T_eff
LGGS J013357.60+304113.3	730^[112]	Triangulum Galaxy	L/T_eff
LGGS J004614.57+421117.4	730^[112]	Andromeda Galaxy	L/T_eff
LGGS J004120.96+404125.3	730^[112]	Andromeda Galaxy	L/T_eff
LGGS J004228.46+405519.0	728^[112]	Andromeda Galaxy	L/T_eff
LGGS J004024.52+404444.8	728^[112]	Andromeda Galaxy	L/T_eff
LGGS J013349.75+304459.8	727^[112]	Triangulum Galaxy	L/T_eff
LGGS J013306.88+303004.6	727^[112]	Triangulum Galaxy	L/T_eff
LGGS J004358.00+412114.1	727^[112]	Andromeda Galaxy	L/T_eff
LGGS J004147.27+411537.8	727^[112]	Andromeda Galaxy	L/T_eff
LGGS J013407.23+304158.8	725^[112]–833^[129]	Triangulum Galaxy	L/T_eff
LGGS J004519.82+415531.9	725^[112]	Andromeda Galaxy	L/T_eff
LGGS J004410.84+411538.8	725^[112]	Andromeda Galaxy	L/T_eff
LGGS J013407.38+305935.0	724^[112]	Triangulum Galaxy	L/T_eff
LGGS J004438.75+415553.6	724^[112]	Andromeda Galaxy	L/T_eff
LGGS J004324.16+411228.3	723^[112]	Andromeda Galaxy	L/T_eff
LGGS J004059.58+403815.6	723^[112]	Andromeda Galaxy	L/T_eff
LGGS J013327.40+304126.4	721^[112]	Triangulum Galaxy	L/T_eff
LGGS J013243.72+301912.5	721^[112]–783^[129]	Triangulum Galaxy	L/T_eff
Gaia DR3 303379932695513216	720^[112]	Triangulum Galaxy	L/T_eff
LGGS J004558.92+414642.1	720^[112]	Andromeda Galaxy	L/T_eff
LGGS J004103.46+403633.2	717^[112]	Andromeda Galaxy	L/T_eff
LGGS J013324.89+301754.3	717^[112]	Triangulum Galaxy	L/T_eff
LGGS J004015.18+405947.7	716^[112]	Andromeda Galaxy	L/T_eff
LGGS J013414.53+303557.7	715^[112]	Triangulum Galaxy	L/T_eff
LGGS J013351.89+303853.5	715^[112]	Triangulum Galaxy	L/T_eff
LGGS J004458.82+413050.4	715^[112]	Andromeda Galaxy	L/T_eff
LGGS J013352.51+303942.2	715^[112]	Triangulum Galaxy	L/T_eff
LGGS J004124.91+411133.1	715^[112]	Andromeda Galaxy	L/T_eff
LGGS J004604.18+415135.4	713^[112]	Andromeda Galaxy	L/T_eff
LGGS J013305.17+303119.8	711^[112]	Triangulum Galaxy	L/T_eff
LGGS J004517.25+413948.2	711^[112]	Andromeda Galaxy	L/T_eff
LGGS J013349.86+303246.1	710^[132]–795^[129]	Triangulum Galaxy	L/T_eff	A yellow supergiant.
2MASS J01335929+3034435	709^[112]	Triangulum Galaxy	L/T_eff
LGGS J004230.32+405624.1	708^[112]	Andromeda Galaxy	L/T_eff
LGGS J004101.02+403506.1	708^[112]	Andromeda Galaxy	L/T_eff
LGGS J004119.21+411237.2	707^[112]	Andromeda Galaxy	L/T_eff
LGGS J004606.25+415018.9	707^[112]	Andromeda Galaxy	L/T_eff
LGGS J013442.05+304540.2	707^[112]–707^[129]	Triangulum Galaxy	L/T_eff
LGGS J013431.84+302721.5	707^[112]–717^[129]	Triangulum Galaxy	L/T_eff
LGGS J013304.68+304456.0	707^[112]–739^[129]	Triangulum Galaxy	L/T_eff
LGGS J004432.27+415158.4	705^[112]	Andromeda Galaxy	L/T_eff
2MASS J01335131+3039149	704^[112]	Triangulum Galaxy	L/T_eff
LGGS J013339.46+302113.0	703^[112]–748^[129]	Triangulum Galaxy	L/T_eff
LGGS J003935.36+401946.4	703^[112]	Andromeda Galaxy	L/T_eff
LGGS J013343.03+303433.5	702^[112]	Triangulum Galaxy	L/T_eff
LGGS J004505.87+413452.3	702^[112]	Andromeda Galaxy	L/T_eff
LGGS J013414.18+305248.0	701^[112]–731^[129]	Triangulum Galaxy	L/T_eff
LGGS J013402.53+304107.7	701^[112]–749^[129]	Triangulum Galaxy	L/T_eff
LGGS J013340.80+304248.5	701^[112]–814^[129]	Triangulum Galaxy	L/T_eff
LGGS J013312.59+303252.5	701^[112]	Triangulum Galaxy	L/T_eff
The following well-known stars are listed for the purpose of comparison.
Var 83	150^[133]	Triangulum Galaxy	L/T_eff	A luminous blue variable and one of the most luminous stars in M33.

Other galaxies (within the Local Group)

List of the largest known stars in other galaxies (within the Local Group)
Star name	Solar radii (Sun = 1)	Galaxy	Method^[a]	Notes
WOH G64 (For comparison)	1,540^[9]^[10]^[11]^[12]^[13] ± 77^[9]	Large Magellanic Cloud	L/T_eff	Located in the Large Magellanic Cloud. The largest known star with a well-defined radius.^[9]^[10]^[14]^[11]
Sextans A 10	995±130^[134]	Sextans A	L/T_eff
WLM 02	883+284 −167^[135]	WLM	L/T_eff
Sextans A 5	870±145^[134]	Sextans A	L/T_eff
Leo A 7	785^[136]	Leo A	L/T_eff
Sextans A 7	710±100^[134]	Sextans A	L/T_eff

Outside the Local Group (inside the Virgo supercluster)

List of the largest known stars in galaxies outside the Local Group inside the Virgo supercluster
Star name	Solar radii (Sun = 1)	Galaxy	Group	Method^[a]	Notes
NGC 1313-310	1,668+168 −190^[137]	NGC 1313		L/T_eff	Luminosity has not yet been constrained well enough yet to confirm its extreme properties, and further observations are needed to show that it is a single, uncontaminated star. Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
WOH G64 (For comparison)	1,540^[9]^[10]^[11]^[12]^[13] ± 77^[9]	Large Magellanic Cloud		L/T_eff	Located in the Large Magellanic Cloud. The largest known star with a well-defined radius.^[9]^[10]^[14]^[11]
NGC 300-125	1,504+176 −157^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 247-154	1,503+79 −75^[137]	NGC 247	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 7793-34	1,392+157 −160^[137]	NGC 7793	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-40	1,286 ⁺¹¹⁶ ₋₁₀₆^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 2403 V14	1,260^[138]	NGC 2403	M81 Group	L/T_eff	A F-type luminous blue variable.
NGC 300-154	1,200 ⁺¹²³ ₋₁₁₁^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-114	1,181 ⁺¹²³ ₋₁₁₁^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-199	1,181 ⁺¹²⁰ ₋₁₀₉^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-153	1,173 ⁺¹²⁰ ₋₁₀₉^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-150	1,167 ⁺¹¹⁹ ₋₁₀₇^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 253-2006	1,167 ⁺⁷⁵ ₋₇₀^[137]	Sculptor Galaxy	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
SPIRITS 14atl	1,134–1,477^[139]	Messier 83	Centaurus A/M83 Group	L/T_eff
NGC 300-59	1,133 ⁺¹⁴⁶ ₋₁₂₉^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 7793-86	1,127 ⁺⁹⁴ ₋₁₀₉^[137]	NGC 7793	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-263	1,108 ⁺¹¹³ ₋₁₀₂^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 247-447	1,101 ⁺⁵⁸ ₋₅₆^[137]	NGC 247	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
SPIRITS 15ahp	1,098^[139]	NGC 2403	M81 Group	L/T_eff
NGC 300-240	1,088 ⁺¹¹² ₋₁₀₁^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 7793-86	1,078 ⁺⁶⁹ ₋₆₄^[137]	NGC 7793	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-173	1,063 ⁺⁸⁴ ₋₇₇^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-340	1,036 ⁺¹⁰⁵ ₋₉₅^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-346	1,023 ⁺¹³⁹ ₋₁₂₈^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 247-533	1,004 ⁺⁶⁶ ₋₆₂^[137]	NGC 247	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-351	992 ⁺¹¹⁵ ₋₁₀₂^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-524	987 ⁺⁷⁷ ₋₇₂^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-135	964 ⁺⁹⁹ ₋₈₉^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-93	955 ⁺⁴⁹ ₋₄₇^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 7793-539	948^[137]	NGC 7793	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-87	948 ⁺¹⁰⁹ ₋₉₈^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-146	921 ⁺⁴⁹ ₋₄₆^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-273	921 ⁺⁹⁴ ₋₈₅^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-186	915 ⁺⁷² ₋₆₅^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-200	905 ⁺⁵⁹ ₋₅₅^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-152	895 ⁺⁵⁸ ₋₅₄^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-413	861 ⁺⁶⁶ ₋₆₁^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-174	856 ⁺⁶⁵ ₋₆₁^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
M81 10584-25-2	851^[138]	Messier 81	M81 Group	L/T_eff
M81 10584-13-3	843^[138]	Messier 81	M81 Group	L/T_eff
NGC 55-75	836 ⁺⁸¹ ₋₁₁₁^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-545	824 ⁺¹⁰⁴ ₋₉₃^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 247-2912	821 ⁺⁵⁴ ₋₅₁^[137]	NGC 247	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-216	801 ⁺¹⁰² ₋₈₉^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 247-1471	798 ⁺⁵² ₋₄₈^[137]	NGC 247	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-499	796 ⁺⁸⁹ ₋₁₀₈^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-379	744 ⁺⁵⁶ ₋₅₂^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-838	744 ⁺⁵⁷ ₋₅₃^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-149	738 ⁺⁴⁷ ₋₅₅^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-194	730 ⁺⁴⁶ ₋₄₄^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
[GKE2015] 7	729^[140]	NGC 300	NGC 55 Group	L/T_eff
NGC 55-270	728 ⁺³⁸ ₋₃₆^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-1047	724 ⁺⁶⁵ ₋₅₉^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 247-3231	719 ⁺⁵⁶ ₋₅₁^[137]	NGC 247	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 247-2966	719 ⁺⁵⁶ ₋₅₂^[137]	NGC 247	Sculptor Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 55-245	717 ⁺⁵⁵ ₋₅₀^[137]	NGC 55	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-1068	716 ⁺⁶⁴ ₋₅₈^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
NGC 300-1081	712 ⁺⁵⁴ ₋₅₁^[137]	NGC 300	NGC 55 Group	L/T_eff	Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.^[137]
The following well-known stars are listed for the purpose of comparison.
NGC 2363-V1	194–356^[141]	NGC 2366	M81 Group	L/T_eff

Outside the Virgo supercluster

Note that this list does not include the candidate JWST dark stars, with estimated radii of up to 61 astronomical units (13,000 R_☉)^[142] or Quasi-stars, with theoretical models suggesting that they could reach radii of up to 40,700 solar radii (189 au).^[143]

Star name	Solar radii (Sun = 1)	Galaxy	Method^[a]	Notes
Quyllur	965^[144]		L/T_eff	Likely the first red supergiant star at cosmological distances and is also discovered by James Webb Space Telescope.
The following well-known stars are listed for the purpose of comparison.
Godzilla	430–2,365^[145]	Sunburst galaxy	L/T_eff	The most luminous known star.^[146]
Mothra	271^[147]	LS1	L/T_eff	A binary star at cosmological distances.

Transient events

During some transient events, such as red novae or LBV eruptions the star's radius can increase by a significant amount.

List of largest stars during transient events
Star or transient event name	Solar radii (Sun = 1)	Year	Galaxy	Group	Method	Notes
AT 2017jfs	33,000^[148]	2017	NGC 4470		L/T_eff
SNhunt151	16,700^[149]	2014	UGC 3165	LDC 331	L/T_eff
SN 2015bh	16,400±2,600^[150]	2015	NGC 2770	LDC 616	L/T_eff
AT 2018hso	10,350^[151]	2018	NGC 3729	M109 Group	L/T_eff
AT 2023clx	6,800^[152]	2023	NGC 3799	nest 101314	L/T_eff
M51 OT2019-1	5,500^[153]	2019	Whirlpool Galaxy	M51 Group	L/T_eff
η Carinae	4,319 – 6,032^[94]	1845	Milky Way	Local Group	L/T_eff	During the outburst, the star became the second brightest star in sky, reaching an apparent magnitude of between −0.8 and −1.0.^[154]
AT 2010dn	4,130^[155]	2010	NGC 3180	LDC 743	L/T_eff
SN 2011fh	3,980^[156]	2011	NGC 4806	Abell 3528	L/T_eff
AT 2014ej	3,600^[157]	2014	NGC 7552	Grus Quartet	L/T_eff
V838 Monocerotis	3,190^[84]	2002	Milky Way	Local Group	L/T_eff
SN2008S	3,020^[155]	2008	NGC 6946	NGC 6946 Group	L/T_eff
SNhunt120	2,900^[158]^[157]	2012	NGC 5775	Virgo Cluster	L/T_eff
AT 2017be	2,000^[159]	2017	NGC 2537		L/T_eff
WOH G64 (For comparison)	1,540^[9]^[10]^[11]^[12]^[13] ± 77^[9]		Large Magellanic Cloud		L/T_eff	Located in the Large Magellanic Cloud. The largest known star with a well-defined radius.^[9]^[10]^[14]^[11]
PHL 293B star	1,348 – 1,463^[160]	2002	PHL 293B		L/T_eff
SNhunt248	~850^[161]	2014	NGC 5806	NGC 5846 Group	L/T_eff
R71	500^[162]	2012	Large Magellanic Cloud	Local Group	L/T_eff
SN 2000ch	500^[163]	2000	NGC 3432	LDC 743	L/T_eff
Godzilla	430 – 2,365^[145]	2015	Sunburst galaxy		?
AT 2016blu	~330^[164]	2012 – 2022	NGC 4559	Coma I Group	L/T_eff	19 outbursts were detected between 2012 and 2022. The star was likely relatively stable the decade before since no outbursts were detected from 1999 – 2009.^[164]

SN Progenitors

List of largest supernova progenitors
Star or supernova name	Solar radii (Sun = 1)	Year	Galaxy	Group	Method	Notes
SN 2020faa	1,000^[165]	2020	2MASS J14470904+7244157		L/T_eff
SN 2023ixf	912+227 −222^[166]–1,060±30^[167]	2023	Pinwheel galaxy	M101 Group	L/T_eff
SN 2020jfo	700±10^[168]	2020	Messier 61	Virgo Cluster	L/T_eff
SN 2023axu	417±28^[169]	2023	NGC 2283		L/T_eff
SN 2021agco	78.37+25.59 −19.94^[170]	2021	UGC 3855	LDC 506	L/T_eff	Nearest ultrastripped supernova known.

Largest stars by apparent size

The following list include the largest stars by their apparent size (angular diameter) as seen from Earth. The unit of measurement is the milliarcsecond (mas), equivalent to 10×10⁻³ arcseconds. Stars with angular diameters larger than 13 milliarcseconds are included.

List of largest stars by apparent size (angular diameter)
Name	Angular diameter (mas)	Angular diameter type^[h]	Distance (light-years)	Spectral type^[171]	Notes
Sun	2,000,000		0.000016	G2V	The largest star by angular diameter.
R Doradus	51.18±1.24^[88]	LD	179±10^[88]	M8III:e	The largest star by angular diameter apart from the Sun.
Betelgeuse (α Orionis)	42.28±0.43^[75]	LD	408–540⁺⁹⁸ ₋₄₉^[75]	M1-M2Ia-Iab
Antares (α Scorpii A)	37.31±0.09^[172]	LD	553.5±93.9^[173]	M1.5Iab
Mira (ο Ceti)	28.9±0.3 – 34.9±0.4^[174]	Ross	299±33^[173]	M5-M9IIIe	The angular diameter vary during Mira's pulsations.
Gacrux (γ Crucis)	24.7^[99]	?	88.6±0.4^[173]	M3.5III
Rasalgethi (α Herculis)	23.95±5.03^[89]	Est	359±52^[173]	M5Ib-II
R Hydrae	23.7±1^[23]	?	482±33^[23]	M6-9e
Arcturus (α Boötis)	21.06±0.17^[175]	LD	36.8^[175]	K1.5IIIFe-0.5
π¹ Gruis	21^[176]	?	535^[176]	S5,7
Aldebaran (α Tauri)	20.58^[177]–21.1^[178]	LD	65.3±1^[179]	K5+III
GY Aquilae	20.46^[23]	?	1108±98^[23]	M8
R Lyrae	18.016±0.224^[178]	LD	310⁺¹⁰ ₋₇^[180]	M4.5III
Scheat (β Pegasi)	16.75±0.24^[181]	Ross	196±2^[173]	M2.5II-III
Gorgonea Tertia (ρ Persei)	16.555±0.166^[178]	LD	308±7^[173]	M4+IIIa
SW Virginis	16.11±0.13–16.8±0.34^[182]	UD	527±46.9^[183]	M7III:
R Aquarii	15.61±0.8 – 16.59±1.03^[182]	LD	711⁺³⁹ ₋₃₆^[184]	M6.5–M8.5e
g Herculis	15.2±0.5 – 19.09±0.19^[182]	LD	385±10^[180]	M6-III
RS Cancri	15.1±0.5 – 17.2±0.4^[178]	LD	490±40^[185]	M6S
Tejat (μ Geminorum)	15.118±0.151^[178]	LD	230±10^[173]	M3IIIab
R Leonis Minoris	14.4±0.87^[182]	LD	942⁺³³ ₋₄₇^[180]	M6.5-9e
S Cephei	14.29±2.28^[182]	LD	1591⁺⁴⁹ ₋₄₆^[180]	C7,3e
T Cassiopeiae	14.22±0.73^[182]	LD	893⁺⁴⁹ ₋₄₆^[180]	M7-9e
μ Cephei (Herschel's Garnet Star)	14.11 ± 0.6^[186]		3060⁺⁴⁶⁰ ₋₁₃₀^[187]	M2Ia
Mirach (β Andromedae)	13.749±0.137^[178]	LD	199±9^[188]	M0+IIIa
Menkar (α Ceti)	13.238±0.056^[178]	LD	249±8^[173]	M1.5IIIa	Another measurents include 12.2±0.04 mas.^[189]
V Cygni	13.1±0.208 – 14.84±2.37^[182]	LD	1747⁺¹⁶³ ₋₁₃₇^[180]	C7,4eJ

Notes

^ ^a ^b ^c ^d ^e ^f
Methods for calculating the radius:
- AD: radius calculated from angular diameter and distance
- L/T_eff: radius calculated from bolometric luminosity and effective temperature
- SEIS: radius obtained from seismic data
- OD: radius obtained from optical depth
^ ^a ^b ^c ^d ^e ^f At the J2000 epoch
^ ^[9]^[10]^[11]^[12]^[13]
^ Using an angular diameter of 7.8±0.64 milliarcseconds^[27] and a distance of 1610+130
−110 parsecs.^[28]
^ Luminosities are calculated using the apparent bolometric magnitude and distances in the following equation:
10^{0.4 • (4.74−(m_bol+5−5 • log(dist)))}
^ Using an angular diameter of 14.11±0.6 milliarcseconds and a distance of 940+140
−40 parsecs.
^ Calculated using a distance of 432 parsecs and an angular diameter of 2.31 milliarcseconds.
^ Legend:
UD=Uniform disk diameter
LD=Limb-darkened diameter
Ross=Rosseland diameter
Est = Estimated using distance and physical radius

References

^ Mamajek, E. E.; Prsa, A.; Torres, G.; Harmanec, P.; Asplund, M.; Bennett, P. D.; Capitaine, N.; Christensen-Dalsgaard, J.; Depagne, E.; Folkner, W. M.; Haberreiter, M. (October 2015). "IAU 2015 Resolution B3 on Recommended Nominal Conversion Constants for Selected Solar and Planetary Properties". arXiv:1510.07674 [astro-ph.SR].
^ Rau, A.; Kulkarni, S. R.; Ofek, E. O.; Yan, L. (2007). "Spitzer Observations of the New Luminous Red Nova M85 OT2006-1". The Astrophysical Journal. 659 (2): 1536–1540. arXiv:astro-ph/0612161. Bibcode:2007ApJ...659.1536R. doi:10.1086/512672. S2CID 8913778.
^ Haemmerlé, Lionel; Woods, T. E.; Klessen, Ralf S.; Heger, Alexander; Whalen, Daniel J. (2018). "The evolution of supermassive Population III stars". Monthly Notices of the Royal Astronomical Society. 474 (2): 2757–2773. arXiv:1705.09301. doi:10.1093/mnras/stx2919.
^ Herrington, Nicholas P.; Whalen, Daniel J.; Woods, Tyrone E. (2023). "Modelling supermassive primordial stars with <SCP>mesa</SCP>". Monthly Notices of the Royal Astronomical Society. 521: 463–473. arXiv:2208.00008. doi:10.1093/mnras/stad572.
^ Haemmerlé, L.; Klessen, R. S.; Mayer, L.; Zwick, L. (2021). "Maximum accretion rate of supermassive stars". Astronomy & Astrophysics. 652: L7. arXiv:2105.13373. Bibcode:2021A&A...652L...7H. doi:10.1051/0004-6361/202141376. S2CID 235247984.
^ Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Meynet, Georges; Maeder, Andre (July 2006). "The Effective Temperatures and Physical Properties of Magellanic Cloud Red Supergiants: The Effects of Metallicity". The Astrophysical Journal. 645 (2): 1102–1117. arXiv:astro-ph/0603596. Bibcode:2006ApJ...645.1102L. doi:10.1086/504417. ISSN 0004-637X. S2CID 5150686.
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^ ^a ^b ^c ^d ^e ^f ^g Richichi, A.; Percheron, I.; Khristoforova, M. (1 February 2005). "CHARM2: An updated Catalog of High Angular Resolution Measurements". Astronomy and Astrophysics. 431 (2): 773–777. Bibcode:2005A&A...431..773R. doi:10.1051/0004-6361:20042039. ISSN 0004-6361.
^ Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
^ Min, Cheulhong; Matsumoto, Naoko; Kim, Mi Kyoung; Hirota, Tomoya; Shibata, Katsunori M.; Cho, Se-Hyung; Shizugami, Makoto; Honma, Mareki (1 April 2014). "Accurate Parallax Measurement toward the Symbiotic Star R Aquarii". Publications of the Astronomical Society of Japan. 66 (2): 38. arXiv:1401.5574. doi:10.1093/pasj/psu003. ISSN 2053-051X.
^ Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
^ Perrin, G.; Ridgway, S. T.; Verhoelst, T.; Schuller, P. A.; Traub, W. A.; Millan-Gabet, R.; Lacasse, M. G. (1 June 2005). "Study of molecular layers in the atmosphere of the supergiant star μ Cep by interferometry in the K band". Astronomy & Astrophysics. 436 (1): 317–324. arXiv:astro-ph/0502415. Bibcode:2005A&A...436..317P. doi:10.1051/0004-6361:20042313. ISSN 0004-6361.
^ Davies, Ben; Beasor, Emma R. (2020). "The 'red supergiant problem': The upper luminosity boundary of Type II supernova progenitors". Monthly Notices of the Royal Astronomical Society. 493: 468–476. arXiv:2001.06020. doi:10.1093/mnras/staa174. Retrieved 3 October 2024.
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External links

Giant Stars An interactive website comparing the Earth and the Sun to some of the largest known stars
Three largest stars identified BBC News
What is the Biggest Star in the Universe? Universe Today

[methods-8] ^ ^a ^b ^c ^d ^e ^f Methods for calculating the radius:
AD: radius calculated from angular diameter and distance

L/T_eff: radius calculated from bolometric luminosity and effective temperature

SEIS: radius obtained from seismic data

OD: radius obtained from optical depth

[2] AD: radius calculated from angular diameter and distance

[3] L/T_eff: radius calculated from bolometric luminosity and effective temperature

[4] SEIS: radius obtained from seismic data

[5] OD: radius obtained from optical depth

[J2000-10] ^ ^a ^b ^c ^d ^e ^f At the J2000 epoch

[16] [9]^[10]^[11]^[12]^[13]

[32] Using an angular diameter of 7.8±0.64 milliarcseconds^[27] and a distance of 1610+130
−110 parsecs.^[28]

[L1-54] Luminosities are calculated using the apparent bolometric magnitude and distances in the following equation:
10^{0.4 • (4.74−(m_bol+5−5 • log(dist)))}

[e-65] Using an angular diameter of 14.11±0.6 milliarcseconds and a distance of 940+140
−40 parsecs.

[102] Calculated using a distance of 432 parsecs and an angular diameter of 2.31 milliarcseconds.

[178] Legend:
UD=Uniform disk diameter
LD=Limb-darkened diameter
Ross=Rosseland diameter
Est = Estimated using distance and physical radius

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[Cai2018-166] Cai, Y. -Z; Pastorello, A.; Fraser, M.; Botticella, M. T.; Gall, C.; Arcavi, I.; Benetti, S.; Cappellaro, E.; Elias-Rosa, N.; Harmanen, J.; Hosseinzadeh, G.; Howell, D. A.; Isern, J.; Kangas, T.; Kankare, E.; Kuncarayakti, H.; Lundqvist, P.; Mattila, S.; McCully, C.; Reynolds, T. M.; Somero, A.; Stritzinger, M. D.; Terreran, G. (1 August 2018). "AT 2017be – a new member of the class of intermediate-luminosity red transients". Monthly Notices of the Royal Astronomical Society. 480 (3): 3424–3445. arXiv:1807.11676. Bibcode:2018MNRAS.480.3424C. doi:10.1093/mnras/sty2070. ISSN 0035-8711. S2CID 118946285.

[allan2020-167] Allan, Andrew P; Groh, Jose H; Mehner, Andrea; Smith, Nathan; Boian, Ioana; Farrell, Eoin J; Andrews, Jennifer E (1 August 2020). "The possible disappearance of a massive star in the low-metallicity galaxy PHL 293B". Monthly Notices of the Royal Astronomical Society. 496 (2): 1902–1908. arXiv:2003.02242. doi:10.1093/mnras/staa1629. ISSN 0035-8711.

[Kankare2015-168] Kankare, E.; Kotak, R.; Pastorello, A.; Fraser, M; Mattila, S.; Smartt, S. J.; Bruce, A.; Chambers, K. C.; Elias-Rosa, N.; Flewelling, H.; Fremling, C.; Harmanen, J.; Huber, M.; Jerkstand, A.; Kangas, T.; Kuncarayakti, H.; Magee, M.; Magnier, E.; Polshaw, J.; Smith, K. W.; Sollerman, J.; Tomasella, L. (7 September 2015). "On the triple peaks of SNHunt248 in NGC 5806". Astronomy & Astrophysics. 581: 7. arXiv:1508.04730. Bibcode:2015A&A...581L...4K. doi:10.1051/0004-6361/201526631. ISSN 0004-6361. S2CID 85321.

[mehner2013-169] Mehner, A.; Baade, D.; Rivinius, T.; Lennon, D. J.; Martayan, C.; Stahl, O.; Štefl, S. (July 2013). "Broad-band spectroscopy of the ongoing large eruption of the luminous blue variable R71". Astronomy & Astrophysics. 555: A116. arXiv:1303.1367. Bibcode:2013A&A...555A.116M. doi:10.1051/0004-6361/201321323. ISSN 0004-6361. S2CID 67775752.

[Aghakhanloo2023-170] Aghakhanloo, Mojgan; Smith, Nathan; Milne, Peter; Andrews, Jennifer E.; Filippenko, Alexei V.; Jencson, Jacob E.; Sand, David J.; Van Dyk, Schuyler D.; Wyatt, Samuel; Zheng, WeiKang (28 February 2023). "Repeating periodic eruptions of the supernova impostor SN 2000ch". Monthly Notices of the Royal Astronomical Society. 521 (2): 1941–1957. arXiv:2212.00113. Bibcode:2023MNRAS.521.1941A. doi:10.1093/mnras/stad630. ISSN 0035-8711. S2CID 254125316.

[Smith2023-171] Aghakhanloo, Mojgan; Smith, Nathan; Milne, Peter; Andrews, Jennifer E.; Van Dyck, Schuyler D.; Filippenko, Alexei V.; Jencson, Jacob E.; Lau, Ryan N.; Sand, David J.; Wyatt, Samuel; Zhang, WeiKang (7 September 2023). "Recurring outbursts of the supernova impostor AT 2016blu in NGC 4559". Monthly Notices of the Royal Astronomical Society. 526 (1): 456–472. arXiv:2212.09708. Bibcode:2023MNRAS.526..456A. doi:10.1093/mnras/stad2702. ISSN 0035-8711. S2CID 254854145.

[Salmaso2023-172] Salmaso, I.; Cappellaro, E.; Tartaglia, L.; Benetti, S.; Botticella, M. T.; Elias-Rosa, M.; Pastorello, A.; Patat, F.; Reguitti, A.; Tomasella, L.; Valerin, G.; Yang, S. (May 2023). "Hidden shock powering the peak of SN 2020faa". Astronomy & Astrophysics. 673: 14. arXiv:2302.12527. Bibcode:2023A&A...673A.127S. doi:10.1051/0004-6361/202245781. ISSN 0004-6361. S2CID 257205910.

[SN2023ixf-173] "Papers with Code - The Dusty and Extremely Red Progenitor of the Type II Supernova 2023ixf in Messier 101". astro.paperswithcode.com. Retrieved 25 November 2023.

[Qin2023-174] Qin, Y.; Zhang, Keming; Bloom, J.; Sollerman, J.; Zimmerman, E.; Irani, I.; Schulze, S.; Gal-yam, A.; Kasliwal, M.; Coughlin, M.; Perley, D.; Fremling, C.; Kulkarni, S. (2024). "The Progenitor Star of SN 2023ixf: A Massive Red Supergiant with Enhanced, Episodic Pre-Supernova Mass Loss". Monthly Notices of the Royal Astronomical Society. 534: 271–280. arXiv:2309.10022. doi:10.1093/mnras/stae2012. S2CID 262054068.

[Kilpatrick2023-175] Kilpatrick, Charles D.; et al. (29 June 2023). "EType II-P supernova progenitor star initial masses and SN 2020jfo: direct detection, light-curve properties, nebular spectroscopy, and local environment". Monthly Notices of the Royal Astronomical Society. 524 (2): 2161–2185. arXiv:2307.00550. Bibcode:2023MNRAS.524.2161K. doi:10.1093/mnras/stad1954. ISSN 0035-8711. S2CID 259306203.

[Shrestha2023-176] Shrestha, Manisha; et al. (2024). "Evidence of weak circumstellar medium interaction in the Type II SN 2023axu". The Astrophysical Journal. 961 (2): 247. arXiv:2310.00162. Bibcode:2024ApJ...961..247S. doi:10.3847/1538-4357/ad11e1.

[Yan2023-177] Yan, Shengyu; Wang, Xiaofeng; Gao, Xing; Zhang, Jujia; Brink, Thomas G.; Mo, Jun; Lin, Weili; Xiang, Danfeng; Ma, Xiaoran; Guo, Fangzhou; Tomasella, Lina; Benetti, Stefano; Cai, Yongzhi; Cappellaro, Enrico; Chen, Zhihao; Li, Zhitong; Pastorello, Andrea; Zhang, Tiangmeng (7 October 2023). "Discovery of the Closest Ultrastripped Supernova: SN 2021agco in UGC 3855". The Astrophysical Journal. 959 (2): L32. arXiv:2310.04827. Bibcode:2023ApJ...959L..32Y. doi:10.3847/2041-8213/ad0cc3.

[s01wO-179] SIMBAD.

[9Oc05-180] Ohnaka, K.; Hofmann, K. -H.; Schertl, D.; Weigelt, G.; Baffa, C.; Chelli, A.; Petrov, R.; Robbe-Dubois, S. (1 July 2013). "High spectral resolution imaging of the dynamical atmosphere of the red supergiant Antares in the CO first overtone lines with VLTI/AMBER". Astronomy and Astrophysics. 555: A24. arXiv:1304.4800. Bibcode:2013A&A...555A..24O. doi:10.1051/0004-6361/201321063. ISSN 0004-6361.

[hip-181] ^ ^a ^b ^c ^d ^e ^f ^g ^h van Leeuwen, F. (1 November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. ISSN 0004-6361.

[lrxV5-182] Woodruff, H. C.; Eberhardt, M.; Driebe, T.; Hofmann, K. -H.; Ohnaka, K.; Richichi, A.; Schertl, D.; Schöller, M.; Scholz, M.; Weigelt, G.; Wittkowski, M.; Wood, P. R. (1 July 2004). "Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared". Astronomy and Astrophysics. 421 (2): 703–714. arXiv:astro-ph/0404248. Bibcode:2004A&A...421..703W. doi:10.1051/0004-6361:20035826. ISSN 0004-6361.

[arcturus-183] Ramírez, I.; Allende Prieto, C. (1 December 2011). "Fundamental Parameters and Chemical Composition of Arcturus". The Astrophysical Journal. 743 (2): 135. arXiv:1109.4425. Bibcode:2011ApJ...743..135R. doi:10.1088/0004-637X/743/2/135. ISSN 0004-637X.

[wallstrom-184] Wallstrom, S. H. J.; Danilovich, T.; Muller, H. S. P.; Gottlieb, C. A.; Maes, S.; Van de Sande, M.; Decin, L.; Richards, A. M. S.; Baudry, A.; Bolte, J.; Ceulemans, T.; De Ceuster, F.; de Koter, A.; Mellah, I. El; Esseldeurs, M. (6 December 2023). "ATOMIUM: Molecular inventory of 17 oxygen-rich evolved stars observed with ALMA". Astronomy & Astrophysics. 681: A50. arXiv:2312.03467. doi:10.1051/0004-6361/202347632. ISSN 0004-6361.

[mdhfs-185] Soubiran, C.; Creevey, O. L.; Lagarde, N.; Brouillet, N.; Jofré, P.; Casamiquela, L.; Heiter, U.; Aguilera-Gómez, C.; Vitali, S.; Worley, C.; de Brito Silva, D. (1 February 2024). "Gaia FGK benchmark stars: Fundamental Teff and log g of the third version". Astronomy and Astrophysics. 682: A145. arXiv:2310.11302. Bibcode:2024A&A...682A.145S. doi:10.1051/0004-6361/202347136. ISSN 0004-6361. Note: See VizieR catalogue

[mark_iii-186] ^ ^a ^b ^c ^d ^e ^f ^g Mozurkewich, D.; Armstrong, J. T.; Hindsley, R. B.; Quirrenbach, A.; Hummel, C. A.; Hutter, D. J.; Johnston, K. J.; Hajian, A. R.; Elias II, Nicholas M.; Buscher, D. F.; Simon, R. S. (November 2003). "Angular Diameters of Stars from the Mark III Optical Interferometer". The Astronomical Journal. 126 (5): 2502–2520. Bibcode:2003AJ....126.2502M. doi:10.1086/378596. ISSN 0004-6256.

[I6LO9-187] Gatewood, George (1 July 2008). "Astrometric Studies of Aldebaran, Arcturus, Vega, the Hyades, and Other Regions". The Astronomical Journal. 136 (1): 452–460. Bibcode:2008AJ....136..452G. doi:10.1088/0004-6256/136/1/452. ISSN 0004-6256.

[b-j-188] ^ ^a ^b ^c ^d ^e ^f Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (2021). "Estimating Distances from Parallaxes. V. Geometric and Photogeometric Distances to 1.47 Billion Stars in Gaia Early Data Release 3". The Astronomical Journal. 161 (3): 147. arXiv:2012.05220. Bibcode:2021AJ....161..147B. doi:10.3847/1538-3881/abd806. S2CID 228063812. Data about this star can be seen here.

[ArroyoTorres2014-189] Arroyo-Torres, B.; et al. (June 2014). "VLTI/AMBER observations of cold giant stars: atmospheric structures and fundamental parameters". Astronomy & Astrophysics. 566: 11. arXiv:1404.7384. Bibcode:2014A&A...566A..88A. doi:10.1051/0004-6361/201323264. S2CID 16778588. A88.

[charm2-190] ^ ^a ^b ^c ^d ^e ^f ^g Richichi, A.; Percheron, I.; Khristoforova, M. (1 February 2005). "CHARM2: An updated Catalog of High Angular Resolution Measurements". Astronomy and Astrophysics. 431 (2): 773–777. Bibcode:2005A&A...431..773R. doi:10.1051/0004-6361:20042039. ISSN 0004-6361.

[9moRd-191] Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.

[UPZZm-192] Min, Cheulhong; Matsumoto, Naoko; Kim, Mi Kyoung; Hirota, Tomoya; Shibata, Katsunori M.; Cho, Se-Hyung; Shizugami, Makoto; Honma, Mareki (1 April 2014). "Accurate Parallax Measurement toward the Symbiotic Star R Aquarii". Publications of the Astronomical Society of Japan. 66 (2): 38. arXiv:1401.5574. doi:10.1093/pasj/psu003. ISSN 2053-051X.

[YsDnt-193] Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.

[194] Perrin, G.; Ridgway, S. T.; Verhoelst, T.; Schuller, P. A.; Traub, W. A.; Millan-Gabet, R.; Lacasse, M. G. (1 June 2005). "Study of molecular layers in the atmosphere of the supergiant star μ Cep by interferometry in the K band". Astronomy & Astrophysics. 436 (1): 317–324. arXiv:astro-ph/0502415. Bibcode:2005A&A...436..317P. doi:10.1051/0004-6361:20042313. ISSN 0004-6361.

[195] Davies, Ben; Beasor, Emma R. (2020). "The 'red supergiant problem': The upper luminosity boundary of Type II supernova progenitors". Monthly Notices of the Royal Astronomical Society. 493: 468–476. arXiv:2001.06020. doi:10.1093/mnras/staa174. Retrieved 3 October 2024.

[ropq1-196] "HD 6860 Overview". NASA Exoplanet Archive. Retrieved 7 June 2024.

[aaa460_3_855-197] Wittkowski, M.; et al. (December 2006), "Tests of stellar model atmospheres by optical interferometry. IV. VINCI interferometry and UVES spectroscopy of Menkar", Astronomy and Astrophysics, 460 (3): 855–864, arXiv:astro-ph/0610150, Bibcode:2006A&A...460..855W, doi:10.1051/0004-6361:20066032, S2CID 16525827

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