{{위키데이터 속성 추적}}
아래 목록은 '''[[광도 (천문학)|광도]] 순서로 밝은 별부터 어두운 별까지 나열한 것'''이다. 절대등급은 어떤 별을 10[[파섹]] 거리에 두고 바라보았을 때의 밝기이다.

절대등급 순서로 별을 나열할 경우 높은 순위를 차지하는 것은 [[질량]]이 큰 [[초거성]]들이다. 이들은 매우 희귀하며 지구에서 멀리 떨어져 있기 때문에 정확한 자료를 도출하는 데 한계가 있다. 따라서 같은 별을 놓고 [[천문학자]]들이 제각기 다른 관측값을 내놓기도 한다.

표에 따르면 현재까지 관측된 별 중 가장 밝은 것은 태양광도의 794만 배로 빛나는 [[궁수자리 V4650]]이다. 그러나 [[외부은하 천체]]인 [[퀘이사]](Quasar)를 포함시킬 경우 순위는 바뀐다. 현재 발견된 퀘이사 중 가장 밝은 것은 [[돛자리]] 구역에서 발견된 [[3C 273]]이다. 이 퀘이사의 [[겉보기 등급]]은 12.8로 맨눈으로 볼 수는 없으나, [[절대등급]]은 -26.7에 달한다. 만약 이 퀘이사를 [[지구]]로부터 10파섹 떨어진 곳에 옮겨다 놓는다고 가정하면, 태양과 똑같은 밝기로 지구인들의 눈에 보일 것이다. 여기서 퀘이사는 태양보다 약 2[[1000000000000|조]] 배 더 밝다는 계산이 나온다. 이 정도 밝기는 [[우리 은하]] 전체 밝기의 약 100배에 해당하는 값이다. 그러나 퀘이사의 광도는 시간에 따라 차이를 보인다.

[[감마선]] 영역만 놓고 보면 [[SGR 1806-20]]이라는 [[마그네타]]([[중성자 별]]의 일종)는 관측된 [[태양계]] 외부 천체 중에서 가장 밝았다. [[2004년]] [[12월 27일]] 이 별은 강력한 [[감마선 폭발]]을 일으켰다. 만약 인간이 감마선을 볼 수 있고, 이 별에서 32.6광년 떨어진 곳에 자리잡고 있다고 가정하면 폭발 순간의 밝기는 -29였을 것이다. 이는 태양보다 밝다. (3.2{{e|15}}~10<sup>16</sup> {{태양광도}})

[[1998년]] 관측된 [[GRB 971214 감마선 폭발]]의 경우 [[초신성]] 수백 개의 폭발과 맞먹는 빛을 발산했다. 이후 연구를 통해 이 에너지는 초신성 1개에서 지구를 향해 뿜어져 나온 것으로 알려졌다.

{| class="wikitable floatright" style="width: 170px;"
|+범례
| style="background: {{항성-색깔|WC}};" align="center" | [[볼프-레이에별]]
|-
| style="background: {{항성-색깔|WN}};" align="center" | [[밝은 청색변광성]]
|-
| style="background: {{항성-색깔|O}};"  align="center" | [[O형 항성]]
|-
| style="background: {{항성-색깔|B}};"  align="center" | [[B형 주계열성|B형 항성]]
|-
| style="background: {{항성-색깔|A}};"  align="center" | [[A형 주계열성|A형 항성]]
|-
| style="background: {{항성-색깔|F}};"  align="center" | [[F형 주계열성|F형 항성]]
|}

{| class="wikitable sortable"
|+1,000,000 {{solar luminosity|link=y}} 이상의 항성들
! 항성 이름
! [[광도 (천문학)|복사광도]]
({{태양광도|link=y}}, [[태양]] = 1)
! [[절대등급|절대복사등급]]
! 대략 태양계로부터의 거리([[광년]])
! [[겉보기등급]]
! [[표면온도|유효온도]] ([[켈빈|K]])
!링크
!참고문헌

|-
| style="background: {{항성-색깔|WN}};"|[[궁수자리 V4650]] ([[다섯쌍둥이 성단]]에 존재)
| 7,943,000
| −12.5
| 25,000
| 12.31 (J 대역)
| 11,300
|{{SIMBAD link|V4650+Sagittarii|SIMBAD}}
|<ref name="mauerhan" /><ref name="qc" />
|-
| style="background: {{항성-색깔|WC}};" | [[BAT99-98]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 5,012,000
| -12.01
| 165,000
| 13.38
| 45,000
|{{SIMBAD link|BAT99+98|SIMBAD}}
|<ref name="Hainich2014">{{저널 인용|last1=Hainich|first1=R.|last2=Rühling|first2=U.|last3=Todt|first3=H.|last4=Oskinova|first4=L. M.|last5=Liermann|first5=A.|last6=Gräfener|first6=G.|last7=Foellmi|first7=C.|last8=Schnurr|first8=O.|last9=Hamann|first9=W. -R.|year=2014|title=The Wolf-Rayet stars in the Large Magellanic Cloud|journal=Astronomy & Astrophysics|volume=565|page=A27|arxiv=1401.5474|bibcode=2014A&A...565A..27H|doi=10.1051/0004-6361/201322696|s2cid=55123954}}</ref><ref name="Doran2013">{{저널 인용 |last1=Doran |first1=E. I. |last2=Crowther |first2=P. A. |last3=de Koter |first3=A. |last4=Evans |first4=C. J. |last5=McEvoy |first5=C. |last6=Walborn |first6=N. R. |last7=Bastian |first7=N. |last8=Bestenlehner |first8=J. M. |last9=Gräfener |first9=G. |last10=Herrero |first10=A. |last11=Köhler |first11=K. |date=2013 |title=The VLT-FLAMES Tarantula Survey. XI. A census of the hot luminous stars and their feedback in 30 Doradus |journal=Astronomy & Astrophysics |volume=558 |issue=134 |page=30 |arxiv=1308.3412 |bibcode=2013A&A...558A.134D |doi=10.1051/0004-6361/201321824 |last19=Vink |last18=van Loon |last16=Schneider |last15=Sana |first12=J. |first13=F. |first14=J. |first15=H. |first16=F. R. N. |first17=W. D. |first18=J. Th. |first19=J. S. |last14=Puls |last13=Najarro |last12=Maíz Apellániz |last17=Taylor |s2cid=118510909}}</ref>
|-
| style="background: {{항성-색깔|WC}};" | [[G0.238-0.071]] ([[은하중심]]에 존재)
| 5,012,000
| -12.01
| 26,000
|14.37 (J 대역)
|39,500-44,000
|{{SIMBAD link|MCD2010+G0.238-0.071|SIMBAD}}
|<ref name="mcd2010">{{저널 인용|last1=Mauerhan|first1=J. C.|last2=Cotera|first2=A.|last3=Dong|first3=H.|last4=Morris|first4=M. R.|last5=Wang|first5=Q. D.|last6=Stolovy|first6=S. R.|last7=Lang|first7=C.|year=2010|title=Isolated Wolf-Rayet Stars and O Supergiants in the Galactic Center Region Identified Via Paschen-α Excess|journal=The Astrophysical Journal|volume=725|issue=1|pages=188–199|arxiv=1009.2769|bibcode=2010ApJ...725..188M|doi=10.1088/0004-637X/725/1/188|s2cid=20968628}}</ref><ref name=HBSP>{{저널 인용|last1=Dong|first1=H.|last2=Wang|first2=Q. D.|last3=Cotera|first3=A.|last4=Stolovy|first4=S.|last5=Morris|first5=M. R.|last6=Mauerhan|first6=J.|last7=Mills|first7=E. A.|last8=Schneider|first8=G.|last9=Calzetti|first9=D.|last10=Lang|first10=C.|date=2011-10-11|title=Hubble Space Telescope Paschen α survey of the Galactic Centre: data reduction and products: HST/NICMOS Paschen α survey of the GC|journal=Monthly Notices of the Royal Astronomical Society|volume=417|issue=1|pages=114–135|arxiv=1105.1703|bibcode=2011MNRAS.417..114D|doi=10.1111/j.1365-2966.2011.19013.x|s2cid=11060463}}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[BMS2003 867|[BMS2003] 867]] A ([[삼각형자리 은하]]의 [[NGC 604]]에 존재)
| 4,932,000
| -12
| 2,700,000
| 16.29 (연성계 전체)
| 42,400
| [https://simbad.cds.unistra.fr/simbad/sim-id?Ident=%5BBMS2003%5D+867A&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id SIMBAD]
|<ref name=":0">{{저널 인용 |last=Bruhweiler |first=Fred C. |last2=Miskey |first2=Cherie L. |last3=Smith Neubig |first3=Margaret |date=June 2003 |title=STIS Spectral Imagery of the OB Stars in NGC 604. II. The Most Luminous Stars |url=https://iopscience.iop.org/article/10.1086/374988 |journal=The Astronomical Journal |volume=125 |issue=6 |pages=3082–3096 |doi=10.1086/374988 |issn=0004-6256|doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|WC}};" | [[R136a1]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 4,677,000
| -11.94
| 163,000
| 12.28
| 46,000
|{{SIMBAD link|RMC136a1|SIMBAD}}
|<ref name=":02">{{저널 인용 |last1=Bestenlehner |first1=Joachim M. |last2=Crowther |first2=Paul A. |last3=Caballero-Nieves |first3=Saida M. |last4=Schneider |first4=Fabian R. N. |last5=Simón-Díaz |first5=Sergio |last6=Brands |first6=Sarah A. |last7=de Koter |first7=Alex |last8=Gräfener |first8=Götz |last9=Herrero |first9=Artemio |last10=Langer |first10=Norbert |last11=Lennon |first11=Daniel J. |date=2020-12-01 |title=The R136 star cluster dissected with Hubble Space Telescope/STIS - II. Physical properties of the most massive stars in R136 |journal=Monthly Notices of the Royal Astronomical Society |volume=499 |issue=2 |pages=1918–1936 |doi=10.1093/mnras/staa2801 |arxiv=2009.05136 |bibcode=2020MNRAS.499.1918B |issn=0035-8711}}</ref><ref name=":12">{{저널 인용 |bibcode=2022ApJ...935..162K |title=Resolving the Core of R136 in the Optical |last1=Kalari |first1=Venu M. |last2=Horch |first2=Elliott P. |last3=Salinas |first3=Ricardo |last4=Vink |first4=Jorick S. |last5=Andersen |first5=Morten |last6=Bestenlehner |first6=Joachim M. |last7=Rubio |first7=Monica |journal=The Astrophysical Journal |year=2022 |volume=935 |issue=2 |page=162 |doi=10.3847/1538-4357/ac8424 |arxiv=2207.13078 |s2cid=251067072 |doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|O}};" |[[M33-013406.63]] A ([[삼각형자리 은하]]에 존재)
| 4,677,000
| -11.935
| 3,000,000
|16.084 (연성계 전체)
| 30,000
|{{SIMBAD link|LGGS+J013406.63%2B304147.8|SIMBAD}}
|<ref name=Kourniotis>{{저널 인용|last1=Kourniotis|first1=M|last2=Kraus|first2=M|last3=Arias|first3=M L|last4=Cidale|first4=L|last5=Torres|first5=A F|date=2018-11-01|title=On the evolutionary state of massive stars in transition phases in M33|journal=Monthly Notices of the Royal Astronomical Society|volume=480|issue=3|pages=3706–3717|arxiv=1808.00008|bibcode=2018MNRAS.480.3706K|doi=10.1093/mnras/sty2087|issn=0035-8711}}</ref><ref name=Massey2006>{{저널 인용|last1=Massey|first1=Philip|last2=Olsen|first2=K. A. G.|last3=Hodge|first3=Paul W.|last4=Strong|first4=Shay B.|last5=Jacoby|first5=George H.|last6=Schlingman|first6=Wayne|last7=Smith|first7=R. C.|date=2006|title=A Survey of Local Group Galaxies Currently Forming Stars. I. UBVRI Photometry of Stars in M31 and M33|journal=The Astronomical Journal|volume=131|issue=5|pages=2478–2496|arxiv=astro-ph/0602128|bibcode=2006AJ....131.2478M|doi=10.1086/503256|s2cid=118865956|issn=0004-6256}}</ref><ref group="lower-alpha">M33-013406.63, LGGS J013406.63+304147.8 이라고도 불리는 별은 원래 태양의 8,000,000배 이상의 광도를 가진다고 생각되었으나 새 문헌이 M33-013406.63이 쌍성일 가능성을 제시했고 이 경우 광도는 태양의 약 4,500,000배로 감소한다.</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[BMS2003 867|[BMS2003] 867]] B ([[삼각형자리 은하]]의 [[NGC 604]]에 존재)
| 4,395,000
| -11.87
| 2,700,00
| 16.29 (연성계 전체)
| 42,400
| [https://simbad.cds.unistra.fr/simbad/sim-id?Ident=%5BBMS2003%5D+867B&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id SIMBAD]
|<ref name=":0" />
|-
| style="background: {{항성-색깔|O}};" |[[웨스터하우트 49-2]] ([[웨스터하우트 49]]에 존재)
| 4,365,000
| -11.86
| 36,200
| 18.246 (J 대역)
| 35,500
| {{SIMBAD link|%5BWBB2016%5D%202|SIMBAD}}
|<ref name=Wu2016>{{저널 인용|last1=Wu|first1=Shi-Wei|last2=Bik|first2=Arjan|last3=Bestenlehner|first3=Joachim M.|last4=Henning|first4=Thomas|last5=Pasquali|first5=Anna|last6=Brandner|first6=Wolfgang|last7=Stolte|first7=Andrea|date=May 2016|title=The massive stellar population of W49: A spectroscopic survey|journal=Astronomy & Astrophysics|volume=589|pages=A16|arxiv=1602.05190|bibcode=2016A&A...589A..16W|doi=10.1051/0004-6361/201527823|issn=0004-6361|s2cid=59425112}}</ref><ref name=2MASS>{{저널 인용 |bibcode=2003yCat.2246....0C |title=VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) |journal=CDS/ADC Collection of Electronic Catalogues |pages=II/246 |volume=2246 |last1=Cutri |first1=Roc M. |last2=Skrutskie |first2=Michael F. |last3=Van Dyk |first3=Schuyler D. |last4=Beichman |first4=Charles A. |last5=Carpenter |first5=John M. |last6=Chester |first6=Thomas |last7=Cambresy |first7=Laurent |last8=Evans |first8=Tracey E. |last9=Fowler |first9=John W. |last10=Gizis |first10=John E. |last11=Howard |first11=Elizabeth V. |last12=Huchra |first12=John P. |last13=Jarrett |first13=Thomas H. |last14=Kopan |first14=Eugene L. |last15=Kirkpatrick |first15=J. Davy |last16=Light |first16=Robert M. |last17=Marsh |first17=Kenneth A. |last18=McCallon |first18=Howard L. |last19=Schneider |first19=Stephen E. |last20=Stiening |first20=Rae |last21=Sykes |first21=Matthew J. |last22=Weinberg |first22=Martin D. |last23=Wheaton |first23=William A. |last24=Wheelock |first24=Sherry L. |last25=Zacarias |first25=N. |year=2003 |url=http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246 |s2cid=115529446}}</ref>
|-
| style="background: {{항성-색깔|WN}};" |[[HD 37836]] ([[대마젤란 은하]]에 존재)
| 4,169,000
| -11.81
| 163,000
| 10.55
| 28,200
| [https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+37836 SIMBAD]
|<ref name=":2">{{저널 인용 |last=Martin |first=John C. |last2=Humphreys |first2=Roberta M. |date=2023-11-01 |title=A Census of the Most Luminous Stars. I. The Upper HR Diagram for the Large Magellanic Cloud |url=https://iopscience.iop.org/article/10.3847/1538-3881/ad011e |journal=The Astronomical Journal |volume=166 |issue=5 |pages=214 |doi=10.3847/1538-3881/ad011e |issn=0004-6256|doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|O}};" |[[Sk -69° 249]] A ([[대마젤란 은하]]의 [[NGC 2074]]에 존재)
| 4,130,000
| -11.8
| 160,000
| 10.68
| 38,900
| {{SIMBAD link|Sk+-69+249|SIMBAD}}
|<ref name=":42">{{저널 인용|last1=Massey|first1=Philip|last2=Waterhouse|first2=Elizabeth|last3=DeGioia-Eastwood|first3=Kathleen|author3-link=Kathy Eastwood|date=May 2000|title=The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. I. Results from 19 OB Associations in the Magellanic Clouds|journal=The Astronomical Journal|volume=119|issue=5|pages=2214–2241|arxiv=astro-ph/0002233|bibcode=2000AJ....119.2214M|doi=10.1086/301345|s2cid=16891188}}</ref><ref name="zacharias">{{저널 인용 |last1=Zacharias |first1=N. |last2=Finch |first2=C. T. |last3=Girard |first3=T. M. |last4=Henden |first4=A. |last5=Bartlett |first5=J. L. |author5-link=Jennifer Bartlett (astronomer) |last6=Monet |first6=D. G. |last7=Zacharias |first7=M. I. |display-authors=5 |date=July 2012 |title=VizieR On-line Data Catalog: UCAC4 Catalogue |journal=VizieR On-line Data Catalog: I/322A |volume=1322 |bibcode=2012yCat.1322....0Z}}</ref>
|-
| style="background: {{항성-색깔|WN}};" | [[용골자리 에타]] A ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
| 4,000,000
| -11.77
| 7,500
| style="background: lightblue;" | 4.3 (연성계 전체)
| 9,400-35,200
|{{SIMBAD link|Eta+Carinae|SIMBAD}}
|<ref name="mehner2019">{{저널 인용|last1=Mehner|first1=A.|last2=De Wit|first2=W.-J.|last3=Asmus|first3=D.|last4=Morris|first4=P. W.|last5=Agliozzo|first5=C.|last6=Barlow|first6=M. J.|last7=Gull|first7=T. R.|last8=Hillier|first8=D. J.|last9=Weigelt|first9=G.|year=2019|title=Mid-infrared evolution of η Carinae from 1968 to 2018|journal=Astronomy & Astrophysics|volume=630|page=L6|arxiv=1908.09154|bibcode=2019A&A...630L...6M|doi=10.1051/0004-6361/201936277|s2cid=202149820}}</ref><ref name="2018-07-02_NAL">{{저널 인용|last1=Hamaguchi|first1=Kenji|last2=Corcoran|first2=Michael F|last3=Pittard|first3=Julian M|last4=Sharma|first4=Neetika|last5=Takahashi|first5=Hiromitsu|last6=Russell|first6=Christopher M. P|last7=Grefenstette|first7=Brian W|last8=Wik|first8=Daniel R|last9=Gull|first9=Theodore R|last10=Richardson|first10=Noel D|last11=Madura|first11=Thomas I|year=2018|title=Non-thermal X-rays from colliding wind shock acceleration in the massive binary Eta Carinae|journal=Nature Astronomy|volume=2|issue=9|pages=731–736|arxiv=1904.09219|bibcode=2018NatAs...2..731H|doi=10.1038/s41550-018-0505-1|s2cid=126188024|first12=Anthony F. J|last12=Moffat}}</ref><ref>{{저널 인용 |last=Damineli |first=Augusto |last2=Hillier |first2=Desmond J. |last3=Navarete |first3=Felipe |last4=Moffat |first4=Anthony F. J. |last5=Weigelt |first5=Gerd |last6=Corcoran |first6=Michael F. |last7=Gull |first7=Theodore R. |last8=Richardson |first8=Noel D. |last9=Ho |first9=Peter |last10=Madura |first10=Thomas I. |last11=Espinoza-Galeas |first11=David |last12=Hartman |first12=Henrik |last13=Morris |first13=Patrick |last14=Pickett |first14=Connor S. |last15=Stevens |first15=Ian R. |date=August 2023 |title=The Long-term Spectral Changes of Eta Carinae: Are they Caused by a Dissipating Occulter as Indicated by cmfgen Models? |url=https://dx.doi.org/10.3847/1538-4357/ace596 |journal=The Astrophysical Journal |language=en |volume=954 |issue=1 |pages=65 |doi=10.3847/1538-4357/ace596 |issn=0004-637X|doi-access=free }}</ref><ref group=lower-alpha>쌍성계로 알려져 있다. 삼연성계일 가능성도 있다. 동반성의 광도도 태양의 1,000,000배에 달하지만 주성의 밝기에 묻힌다.</ref>
|-
| style="background: {{항성-색깔|WN}};" |[[궁수자리 V4998]] ([[다섯쌍둥이 성단]]에 존재)
| 3,981,000
| -11.76
| 25,000
| 12.534 (J 대역)
| 12,000
| {{SIMBAD link|V4998+Sagittarii|SIMBAD}}
|<ref name="mauerhan">{{저널 인용|last1=Mauerhan|first1=J. C.|last2=Morris|first2=M. R.|last3=Cotera|first3=A.|last4=Dong|first4=H.|last5=Wang|first5=Q. D.|last6=Stolovy|first6=S. R.|last7=Lang|first7=C.|last8=Glass|first8=I. S.|year=2010|title=Discovery of a Luminous Blue Variable with an Ejection Nebula Near the Quintuplet Cluster|journal=The Astrophysical Journal|volume=713|issue=1|pages=L33–L36|arxiv=1002.3379|bibcode=2010ApJ...713L..33M|doi=10.1088/2041-8205/713/1/L33|s2cid=42696538}}</ref><ref name=2MASS/>
|-
| style="background: {{항성-색깔|WC}};" |[[R136c]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 3,802,000
| -11.71
| 163,000
| 13.43
| 51,000
| {{SIMBAD link|RMC136c|SIMBAD}}
|<ref name="schneider2018">{{저널 인용|last1=Schneider|first1=F. R. N.|last2=Sana|first2=H.|last3=Evans|first3=C. J.|last4=Bestenlehner|first4=J. M.|last5=Castro|first5=N.|last6=Fossati|first6=L.|last7=Gräfener|first7=G.|last8=Langer|first8=N.|last9=Ramírez-Agudelo|first9=O. H.|last10=Sabín-Sanjulián|first10=C.|last11=Simón-Díaz|first11=S.|year=2018|title=An excess of massive stars in the local 30 Doradus starburst|journal=Science|volume=359|issue=6371|pages=69–71|arxiv=1801.03107|bibcode=2018Sci...359...69S|doi=10.1126/science.aan0106|first27=Ph.|first23=D. J.|last24=Maíz Apellániz|first24=J.|last25=Markova|first25=N.|last26=Najarro|first26=F.|last27=Podsiadlowski|first29=W. D.|last28=Puls|first28=J.|last29=Taylor|first22=V.|last30=van Loon|first30=J. Th.|last31=Vink|first31=J. S.|last32=Norman|last23=Lennon|first14=A.|last22=Kalari|first16=P. L.|last12=Tramper|first12=F.|last13=Crowther|first13=P. A.|last14=de Koter|last15=de Mink|first15=S. E.|last16=Dufton|last17=Garcia|first21=R. G.|first17=M.|last18=Gieles|first18=M.|last19=Hénault-Brunet|first19=V.|last20=Herrero|first20=A.|last21=Izzard|first32=C.|pmid=29302009|s2cid=206658504}}</ref><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[아치스 성단|아치스]]-F7 ([[아치스 성단]]에 존재하는 WR 102aj)
| 3,802,000
| -11.71
| 25,000
| 15.74 (J 대역)
| 32,900
| {{SIMBAD link|FNG2002+7|SIMBAD}}
|<ref name="martins" /><ref name=":21" />
|-
| style="background: {{항성-색깔|WC}};" |[[R136a3]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 3,631,000
| -11.66
| 163,000
| 12.97
| 50,000
| {{SIMBAD link|RMC136a3|SIMBAD}}
|<ref name=":02" /><ref name=":12" />
|-
| style="background: {{항성-색깔|O}};" |[[멜닉 42]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 3,631,000
| -11.66
| 163,000
| 12.78
| 47,300
| {{SIMBAD link|Cl*+NGC+2070+MEL+42|SIMBAD}}
|<ref name="best">{{저널 인용|last1=Bestenlehner|first1=J. M.|last2=Gräfener|first2=G.|last3=Vink|first3=J. S.|last4=Najarro|first4=F.|last5=De Koter|first5=A.|last6=Sana|first6=H.|last7=Evans|first7=C. J.|last8=Crowther|first8=P. A.|last9=Hénault-Brunet|first9=V.|last10=Herrero|first10=A.|last11=Langer|first11=N.|year=2014|title=The VLT-FLAMES Tarantula Survey. XVII. Physical and wind properties of massive stars at the top of the main sequence|journal=Astronomy & Astrophysics|volume=570|page=A38|arxiv=1407.1837|bibcode=2014A&A...570A..38B|doi=10.1051/0004-6361/201423643|last13=Simón-Díaz|first13=S.|last14=Taylor|first14=W. D.|last15=Walborn|first15=N. R.|first12=F. R. N.|last12=Schneider|s2cid=118606369}}</ref><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[머서 23]]-2 ([[은하면]]의 [[머서 23]]에 존재하는 WR 125–3)
|3,631,000
| -11.66
|21,200
|8.646 (J 대역)
|38,000
|{{SIMBAD link|HKB2010b+Obj2|SIMBAD}}
|<ref name=":20">{{저널 인용|last1=Hanson|first1=M. M.|last2=Kurtev|first2=R.|last3=Borissova|first3=J.|last4=Georgiev|first4=L.|last5=Ivanov|first5=V. D.|last6=Hillier|first6=D. J.|last7=Minniti|first7=D.|date=June 2010|title=Obscured clusters: III. Follow-up observations of Mercer 23|journal=Astronomy and Astrophysics|volume=516|page=A35|bibcode=2010A&A...516A..35H|doi=10.1051/0004-6361/200913122|issn=0004-6361|s2cid=53705451|doi-access=free}}</ref><ref name=2MASS/><ref group="lower-alpha" name="Mc23">Mercer 23은 은하면 근처의 산개성단이다.</ref>
|-
| style="background: {{항성-색깔|WC}};" | [[R136a2]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 3,548,000
| -11.64
| 163,000
| 12.34
| 50,000
| {{SIMBAD link|RMC136a2|SIMBAD}}
|<ref name=":02" /><ref name=":12" />
|-
| style="background: {{항성-색깔|F}};" | [[NGC 2403 V14]] ([[NGC 2403]]에 존재)
| 3,436,000
| -11.6
| 10,314,000
| 18.83
| 7,000
|{{SIMBAD link|%5BHSG2019%5D%2010182-pr-2|SIMBAD}}
|<ref name="humphreys2019">{{저널 인용 |last1=Humphreys |first1=Roberta M. |last2=Stangl |first2=Sarah |last3=Gordon |first3=Michael S. |last4=Davidson |first4=Kris |last5=Grammer |first5=Skyler H. |date=January 2019 |title=Luminous and Variable Stars in NGC 2403 and M81 |journal=[[The Astronomical Journal]] |volume=157 |issue=1 |pages=22 |arxiv=1811.06559 |bibcode=2019AJ....157...22H |doi=10.3847/1538-3881/aaf1ac |s2cid=119379139 |issn=0004-6256 |doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|O}};" |[[G0.070+0.025]] ([[은하중심]]에 존재)
| 3,311,000
| -11.56
| 26,000
| 14.799 (J 대역)
| 45,000
|{{SIMBAD link|MCD2010+G0.070%2B0.025|SIMBAD}}
|<ref name="mcd2010" />
|-
| style="background: {{항성-색깔|WN}};" |[[피스톨별]] ([[다섯쌍둥이 성단]]에 존재하는 궁수자리 V4647)
| 3,300,000
| -11.556
| 25,000
| 11.79 (J 대역)
| 11,800
| {{SIMBAD link|Pistol+Star|SIMBAD}}
|<ref name="ryan">{{저널 인용|last1=Lau|first1=R. M.|last2=Herter|first2=T. L.|last3=Morris|first3=M. R.|last4=Adams|first4=J. D.|year=2014|title=Nature Versus Nurture: Luminous Blue Variable Nebulae in and Near Massive Stellar Clusters at the Galactic Center|journal=The Astrophysical Journal|volume=785|issue=2|page=120|arxiv=1403.5298|bibcode=2014ApJ...785..120L|doi=10.1088/0004-637X/785/2/120|s2cid=118447462}}</ref><ref name=qc>{{저널 인용|last1=Clark|first1=J. S.|last2=Lohr|first2=M. E.|last3=Patrick|first3=L. R.|last4=Najarro|first4=F.|last5=Dong|first5=H.|last6=Figer|first6=D. F.|date=2018|title=An updated stellar census of the Quintuplet cluster|journal=Astronomy & Astrophysics|volume=618|page=A2|arxiv=1805.10139|bibcode=2018A&A...618A...2C|doi=10.1051/0004-6361/201833041|s2cid=53501337|issn=0004-6361}}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[머서 30]]-1 A ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재하는 WR 46-3 A)
|3,236,000
| -11.535
|40,000
|10.33 (J 대역)
|32,200
|{{SIMBAD link|DNB2016+Mc30-1|SIMBAD}}
|<ref name=":17">{{저널 인용|last1=de la Fuente|first1=D.|last2=Najarro|first2=F.|last3=Borissova|first3=J.|last4=Ramírez Alegría|first4=S.|last5=Hanson|first5=M. M.|last6=Trombley|first6=C.|last7=Figer|first7=D. F.|last8=Davies|first8=B.|last9=Garcia|first9=M.|last10=Kurtev|first10=R.|last11=Urbaneja|first11=M. A.|date=May 2016|title=Probing the Dragonfish star-forming complex: the ionizing population of the young massive cluster Mercer 30|journal=Astronomy & Astrophysics|volume=589|page=A69|arxiv=1602.02503|bibcode=2016A&A...589A..69D|doi=10.1051/0004-6361/201528004|issn=0004-6361|last12=Smith|first12=L. C.|last13=Lucas|first13=P. W.|last14=Herrero|first14=A.|s2cid=119096455}}</ref><ref group="lower-alpha" name="Mc30">머서 30은 드래곤피쉬 성운의 산개성단이다.</ref>
|-
| style="background: {{항성-색깔|WC}};" | [[VFTS 682]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 3,236,000
| -11.535
| 164,000
| 16.08
| 52,200
| {{SIMBAD link|VFTS+682|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 42e]] ([[NGC 3603]]의 [[HD 97950]]에 존재)
| 3,200,000
| -11.523
| 25,000
| 14.53
| 43,000
| {{SIMBAD link|WR+42e|SIMBAD}}
|<ref name="lopes">{{저널 인용|last1=Roman-Lopes|first1=A.|year=2012|title=A Galactic O2 If*/WN6 star possibly ejected from its birthplace in NGC 3603|journal=Monthly Notices of the Royal Astronomical Society Letters|volume=427|issue=1|pages=L65–L69|arxiv=1209.1598|bibcode=2012MNRAS.427L..65R|doi=10.1111/j.1745-3933.2012.01346.x|s2cid=118453639}}</ref><ref group=lower-alpha>절대복사등급이 실수로 &minus;11.5 대신 &minus;10.5로 적혀있다.</ref>
|-
| style="background: {{항성-색깔|WN}};" |[[R99]] ([[대마젤란 은하]]의 [[N44]]에 존재)
| 3,162,000
| -11.51
| 163,000
| 11.52
| 28,000
| {{SIMBAD link|RMC99|SIMBAD}}
|<ref name="Hainich2014" /><ref name=ducati>{{저널 인용|bibcode=2002yCat.2237....0D|title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system|journal=CDS/ADC Collection of Electronic Catalogues|volume=2237|page=0|last1=Ducati|first1=J. R.|year=2002}}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[VFTS 1022]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|3,020,000
| -11.46
|164,000
|13.47
|42,200
|{{SIMBAD link|VFTS+1022|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 24]] ([[용골자리 성운]]의 [[콜린더 228]]에 존재)
| 2,951,000
| -11.435
| 8,200
| style="background: lightblue;" | 6.48
| 50,100
|{{SIMBAD link|WR+24|SIMBAD}}
|<ref name="WN">{{저널 인용|last1=Sota|first1=A.|last2=Maíz Apellániz|first2=J.|last3=Morrell|first3=N. I.|last4=Barbá|first4=R. H.|last5=Walborn|first5=N. R.|last6=Gamen|first6=R. C.|last7=Arias|first7=J. I.|last8=Alfaro|first8=E. J.|last9=Oskinova|first9=L. M.|year=2019|title=The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters|journal=Astronomy & Astrophysics|volume=A57|page=625|arxiv=1904.04687|bibcode=2019A&A...625A..57H|doi=10.1051/0004-6361/201834850|s2cid=104292503}}</ref><ref name=gcvs>{{저널 인용|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S|volume=1|display-authors=etal|last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[WR 102ka]] ([[은하중심]]에 존재)
| 2,951,000
| -11.435
| 26,000
| 12.978 (J 대역)
| 25,100
| {{SIMBAD link|Peony+Star|SIMBAD}}
|<ref name=peony2>{{저널 인용 |last1=Oskinova |first1=L. M. |last2=Steinke |first2=M. |last3=Hamann |first3=W. -R. |last4=Sander |first4=A. |last5=Todt |first5=H. |last6=Liermann |first6=A. |date=2013-12-01 |title=One of the most massive stars in the Galaxy may have formed in isolation |journal=Monthly Notices of the Royal Astronomical Society |volume=436 |issue=4 |pages=3357–3365 |doi=10.1093/mnras/stt1817 |arxiv=1309.7651 |bibcode=2013MNRAS.436.3357O |issn=0035-8711|doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[CXOGC J174528.6-285605]] ( [[은하중심]]에 존재하는 WR 101–6
|2,884,000
| -11.41
|26,000
|14.46 (J 대역)
|30,000
|{{SIMBAD link|CXOGC+J174528.6-285605|SIMBAD}}
|<ref name=":21">{{저널 인용|last1=Mauerhan|first1=J. C.|last2=Muno|first2=M. P.|last3=Morris|first3=M. R.|last4=Stolovy|first4=S. R.|last5=Cotera|first5=A.|date=10 February 2010|title=Near-infrared Counterparts to Chandra X-ray Sources Toward the Galactic Center. II. Discovery of Wolf-Rayet Stars and O Supergiants|journal=The Astrophysical Journal|volume=710|issue=1|pages=706–728|arxiv=0912.1055|bibcode=2010ApJ...710..706M|doi=10.1088/0004-637X/710/1/706|issn=0004-637X|s2cid=32339182}}</ref>
|-
| style="background: {{항성-색깔|WN}};" | [[G0.059-0.068]] ([[은하중심]]에 존재)
| 2,884,000
| -11.41
| 26,000
| 13.337 (J 대역)
| 39,500-44,000
| {{SIMBAD link|MCD2010+G0.059-0.068|SIMBAD}}
|<ref name="mcd2010" /><ref name=HBSP/>
|-
| style="background: {{항성-색깔|WC}};" |[[NGC 3603-B|HD 97950 B]] ([[NGC 3603]]의 [[HD 97950]]에 존재하는 WR 43b)
| 2,884,000
| -11.41
| 24,000
| 11.33
| 42,000
| {{SIMBAD link|HD+97950B|SIMBAD}}
|<ref name="crowther">{{저널 인용|last1=Crowther|first1=P. A.|last2=Schnurr|first2=O.|last3=Hirschi|first3=R.|last4=Yusof|first4=N.|last5=Parker|first5=R. J.|last6=Goodwin|first6=S. P.|last7=Kassim|first7=H. A.|year=2010|title=The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M<sub>⊙</sub> stellar mass limit|journal=[[Monthly Notices of the Royal Astronomical Society]]|volume=408|issue=2|pages=731–751|arxiv=1007.3284|bibcode=2010MNRAS.408..731C|doi=10.1111/j.1365-2966.2010.17167.x|s2cid=53001712}}</ref><ref name=melena2008>{{저널 인용|last1=Melena|first1=Nicholas W.|last2=Massey|first2=Philip|last3=Morrell|first3=Nidia I.|last4=Zangari|first4=Amanda M.|title=The Massive Star Content of NGC 3603|journal=The Astronomical Journal|volume=135|issue=3|year=2008|pages=878–891|issn=0004-6256|doi=10.1088/0004-6256/135/3/878|bibcode=2008AJ....135..878M|arxiv = 0712.2621 |s2cid=16765414}}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[HD 38282]] A ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|2,754,000
| -11.35
| 163,000
| 11.11 (연성계 전체)
| 50,000
| [https://simbad.cds.unistra.fr/simbad/sim-id?Ident=HD+38282 SIMBAD]
|<ref name=":1">{{저널 인용 |last=Shenar |first=T. |last2=Sana |first2=H. |last3=Marchant |first3=P. |last4=Pablo |first4=B. |last5=Richardson |first5=N. |last6=Moffat |first6=A. F. J. |last7=Reeth |first7=T. Van |last8=Barbá |first8=R. H. |last9=Bowman |first9=D. M. |last10=Broos |first10=P. |last11=Crowther |first11=P. A. |last12=Clark |first12=J. S. |last13=Koter |first13=A. de |last14=Mink |first14=S. E. de |last15=Dsilva |first15=K. |date=2021-06-01 |title=The Tarantula Massive Binary Monitoring - V. R 144: a wind-eclipsing binary with a total mass ≳140 M⊙ |url=https://www.aanda.org/articles/aa/abs/2021/06/aa40693-21/aa40693-21.html |journal=Astronomy & Astrophysics |language=en |volume=650 |pages=A147 |doi=10.1051/0004-6361/202140693 |issn=0004-6361|doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|WC}};" | [[멜닉 34]] A ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 2,692,000
| -11.335
| 163,000
| 13.09 (연성계 전체)
| 53,000
|{{SIMBAD link|Cl*+NGC+2070+MEL+34|SIMBAD}}
|<ref name="tehrani">{{저널 인용|last1=Tehrani|first1=Katie A.|last2=Crowther|first2=Paul A.|last3=Bestenlehner|first3=Joachim M.|last4=Littlefair|first4=Stuart P.|last5=Pollock|first5=A M T.|last6=Parker|first6=Richard J.|last7=Schnurr|first7=Olivier|year=2019|title=Weighing Melnick 34: The most massive binary system known|journal=Monthly Notices of the Royal Astronomical Society|volume=484|issue=2|pages=2692–2710|arxiv=1901.04769|bibcode=2019MNRAS.484.2692T|doi=10.1093/mnras/stz147|s2cid=119069481}}</ref><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 102hb]] ([[다섯쌍둥이 성단]]에 존재)
| 2,630,000
| -11.31
| 26,000
| 13.9  (J 대역)
| 25,100
| {{SIMBAD link|WR+102hb|SIMBAD}}
|<ref name="quintuplet">{{저널 인용|last1=Liermann|first1=A.|last2=Hamann|first2=W. -R.|last3=Oskinova|first3=L. M.|last4=Todt|first4=H.|last5=Butler|first5=K.|year=2010|title=The Quintuplet cluster|journal=Astronomy & Astrophysics|volume=524|page=A82|arxiv=1011.5796|bibcode=2010A&A...524A..82L|doi=10.1051/0004-6361/200912612|s2cid=30091594}}</ref><ref name=qc/>
|-
| style="background: {{항성-색깔|WC}};" |[[BMS2003 578|[BMS2003] 578]] C ([[삼각형자리 은하]]의 [[NGC 604]]에 존재)
|2,564,000
| -11.28
|2,700,000
|15.97 (연성계 전체)
|34,000
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=%5BBMS2003%5D+578C&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id SIMBAD]
|<ref name=":0" />
|-
| style="background: {{항성-색깔|WC}};" |[[BAT99-80]] A ([[대마젤란 은하]]의 [[NGC 2044]]에 존재)
|2,512,000
| -11.26
|165,000
|13 (연성계 전체)
|45,000
|{{SIMBAD link|BAT99+80|SIMBAD}}
|<ref name="Hainich2014" /><ref name=Schild>{{저널 인용|last1=Schild|first1=H.|last2=Testor|first2=G.|date=March 1992|title=Spectral types and UBV magnitudes of stars in the 30 Doradus complex.|journal=Astronomy and Astrophysics Supplement Series|volume=92|pages=729–748|bibcode=1992A&AS...92..729S|s2cid=115371295}}</ref>
|-
| style="background: {{항성-색깔|WC}};" | [[R146]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 2,512,000
| -11.26
| 164,000
| 13.11
|63,000
|{{SIMBAD link|RMC146|SIMBAD}}
|<ref name="Hainich2014" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[VFTS 482]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|2,512,000
| -11.26
|164,000
|12.95
|42,200
|{{SIMBAD link|VFTS+482|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[NGC 3603-A1|HD 97950 A1a]] ([[NGC 3603]]의 [[HD 97950HD]]에 존재하는 WR 43a A)
| 2,455,000
| -11.235
| 24,000
| 11.18 (연성계 전체)
| 42,000
| {{SIMBAD link|Cl*+NGC+3603+BLW+A1|SIMBAD}}
|<ref name="crowther" /><ref name="melena2008" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 102ea]] ([[다섯쌍둥이 성단]]에 존재)
| 2,455,000
| -11.235
| 26,000
| 13.18 (J 대역)
| 25,100
| {{SIMBAD link|WR+102ea|SIMBAD}}
|<ref name="quintuplet" /><ref name="qc" />
|-
| style="background: {{항성-색깔|WC}};" |[[HD 38282]] B ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 2,455,000
| -11.235
| 163,000
| 11.11 (연성계 전체)
| 45,000
| [https://simbad.cds.unistra.fr/simbad/sim-id?Ident=HD+38282 SIMBAD]
|<ref name=":1" />
|-
| style="background: {{항성-색깔|WC}};" |[[CXOGC J174516.1-284909]] ([[은하중심]]에 존재하는 WR 101–2)
|2,399,000
| -11.21
|26,000
|11.49 (J 대역)
|20,000
|{{SIMBAD link|CXOGC+J174516.1-284909|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|WC}};" |[[CXOGC J174711.4-283006]] ([[은하중심]]에 존재하는 WR 102–9)
|2,399,000
| -11.21
|26,000
|16.56 (J 대역)
|30,000
|{{SIMBAD link|CXOGC+J174711.4-283006|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 25]] A ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
| 2,399,000
| -11.21
| 6,800
| 8.8 (연성계 전체)
| 50,100
| {{SIMBAD link|WR+25|SIMBAD}}
|<ref name="WN" /><ref name="ducati" /><ref group="lower-alpha" name="Binary">쌍성계지만 동반성이 주성에 비해 매우 어둡다.</ref>
|-
| style="background: {{항성-색깔|WN}};" | [[LGGS J004444.52+412804.0]] ([[안드로메다 은하]]에 존재)
| 2,377,000
| -11.2
|2,500,000
|18.1
| 7,000-18,000
|{{SIMBAD link|LGGS+J004444.52%2B412804.0|SIMBAD}}
|<ref name="m31">{{저널 인용|last1=Sholukhova|first1=O.|last2=Bizyaev|first2=D.|last3=Fabrika|first3=S.|last4=Sarkisyan|first4=A.|last5=Malanushenko|first5=V.|last6=Valeev|first6=A.|date=2014|title=New Luminous Blue Variables in the Andromeda galaxy|journal=Monthly Notices of the Royal Astronomical Society|volume=447|issue=3|pages=2459–2467|arxiv=1412.5319|bibcode=2015MNRAS.447.2459S|doi=10.1093/mnras/stu2597|s2cid=118374186}}</ref><ref>{{저널 인용|author-link1=Roberta M. Humphreys|last1=Humphreys|first1=Roberta M.|last2=Weis|first2=Kerstin|last3=Davidson|first3=Kris|last4=Bomans|first4=D. J.|last5=Burggraf|first5=Birgitta|date=2014-07-02|title=LUMINOUS AND VARIABLE STARS IN M31 AND M33. II. LUMINOUS BLUE VARIABLES, CANDIDATE LBVs, Fe II EMISSION LINE STARS, AND OTHER SUPERGIANTS|journal=The Astrophysical Journal|volume=790|issue=1|page=48|arxiv=1407.2259|bibcode=2014ApJ...790...48H|doi=10.1088/0004-637X/790/1/48|s2cid=119177378|issn=0004-637X}}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[HD 269327]] ([[대마젤란 은하]]에 존재)
|2,377,000
| -11.2
|163,000
|10.74
|28,200
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+269327 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" |[[Sk -69° 212]] ([[대마젤란 은하]]의 [[NGC 2044]]에 존재)
|2,377,000
| -11.2
|160,000
|12.416
|45,400
|{{SIMBAD link|Sk+-69+212|SIMBAD}}
|<ref name=":42" /><ref name=Bonanos2009 />
|-
| style="background: {{항성-색깔|WC}};" |[[피스미스 24|WR 93]] ([[NGC 6357]]의 [[피스미스 24]]에 존재)
|2,377,000
| -11.2
|5,700
|10.68
|71,000
|{{SIMBAD link|WR+93|SIMBAD}}
|<ref name="Massey et al. 2001">{{저널 인용|last1=Massey|first1=P.|last2=Degioia-Eastwood|first2=K.|author2-link=Kathy Eastwood|last3=Waterhouse|first3=E.|year=2001|title=The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. II. Results from 12 Galactic Clusters and OB Associations|journal=The Astronomical Journal|volume=121|issue=2|pages=1050–1070|arxiv=astro-ph/0010654|bibcode=2001AJ....121.1050M|doi=10.1086/318769|s2cid=53345173}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|WC}};" |[[멜닉 34]] B ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 2,344,000
| -11.185
| 163,000
| 13.09 (연성계 전체)
| 53,000
| {{SIMBAD link|Cl*+NGC+2070+MEL+34|SIMBAD}}
|<ref name="tehrani" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[VVV CL041]]-8 ([[VVV CL041]]에 존재하는 WR 62–2)
|2,344,000
| -11.185
|13,700
|10.146 (J 대역)
|34,000
|{{SIMBAD link|CRB2015+VVV+CL041-8|SIMBAD}}
|<ref>{{저널 인용|last1=Chené|first1=A.-N.|last2=Ramírez Alegría|first2=S.|last3=Borissova|first3=J.|last4=O’Leary|first4=E.|last5=Martins|first5=F.|last6=Hervé|first6=A.|last7=Kuhn|first7=M.|last8=Kurtev|first8=R.|last9=Consuelo Amigo Fuentes|first9=P.|last10=Bonatto|first10=C.|last11=Minniti|first11=D.|date=December 2015|title=Massive open star clusters using the VVV survey: IV. WR 62-2, a new very massive star in the core of the VVV CL041 cluster|journal=Astronomy & Astrophysics|volume=584|page=A31|arxiv=1510.02539|bibcode=2015A&A...584A..31C|doi=10.1051/0004-6361/201525958|issn=0004-6361|s2cid=118707197}}</ref><ref name=2MASS/><ref group="lower-alpha">VVV CL041는 산개성단이다.</ref>
|-
| style="background: {{항성-색깔|O}};" |[[Cl 1813-178]] #16 ([[W33 분자운 복합체|W33 복합체]]의 [[Cl 1813-178]]에 존재)
|2,291,000
| -11.16
|15,300
|9.428 (J 대역)
|30,200
|{{SIMBAD link|MFD2008+16|SIMBAD}}
|<ref>{{저널 인용|last1=Messineo|first1=Maria|last2=Davies|first2=Ben|last3=Figer|first3=Donald F.|last4=Kudritzki|first4=R. P.|last5=Valenti|first5=Elena|last6=Trombley|first6=Christine|last7=Najarro|first7=F.|last8=Michael Rich|first8=R.|date=20 May 2011|title=Massive Stars in the Cl 1813-178 Cluster: An Episode Of Massive Star Formation in the W33 Complex|journal=The Astrophysical Journal|volume=733|issue=1|page=41|arxiv=1103.4975|bibcode=2011ApJ...733...41M|doi=10.1088/0004-637X/733/1/41|issn=0004-637X|s2cid=118576212}}</ref><ref name=2MASS/><ref group="lower-alpha">Cl 1813-178은 분자운 복합체 W33 복합체의 산개성단이다.</ref>
|-
| style="background: {{항성-색깔|O}};" | [[R136|R136a7]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 2,291,000
| -11.16
| 163,000
| 13.97
| 54,000
|{{SIMBAD link|RMC136a7|SIMBAD}}
|<ref name="Brands2022">{{저널 인용 |last1=Brands |first1=S. |last2=de Koter |first2=A. |last3=Bestenlehner |first3=J. |last4=Crowther |first4=P. |last5=Sundqvist |first5=J. |last6=Puls |first6=J. |last7=Caballero-Nieves |first7=S. |last8=Abdul-Masih |first8=M. |last9=Driessen |first9=F. |last10=Garcia |first10=M. |last11=Geen |first11=S. |date=7 April 2022 |title=The R136 star cluster dissected with Hubble Space Telescope/STIS. III. The most massive stars and their clumped winds |journal=Astronomy & Astrophysics |arxiv=2202.11080 |bibcode=2022A&A...663A..36B |doi=10.1051/0004-6361/202142742 |issn=0004-6361 |last12=Gräfener |first12=G. |last13=Hawcroft |first13=C. |last14=Kaper |first14=L. |last15=Keszthelyi |first15=Z. |last16=Langer |first16=N. |last17=Sana |first17=H. |last18=Schneider |first18=Fabian R. N. |last19=Shenar |first19=T. |last20=Vink |first20=Jorick S. |volume=663 |pages=A36 |s2cid=247025548}}</ref><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|B}};" |[[VVV CL074]]-12 ([[VVV CL074]]에 존재)
|2,291,000
| -11.16
|20,000
|12.34 (J 대역)
|22,500
|{{SIMBAD link|CBB2013+VVV+CL074+12|SIMBAD}}
|<ref name=Martins2019>{{저널 인용|last1=Martins|first1=F.|last2=Chené|first2=A.-N.|last3=Bouret|first3=J.-C.|last4=Borissova|first4=J.|last5=Groh|first5=J.|last6=Ramírez Alegría|first6=S.|last7=Minniti|first7=D.|date=2019|title=Massive stars in the young cluster VVV CL074|journal=Astronomy & Astrophysics|volume=627|page=A170|arxiv=1907.02357|bibcode=2019A&A...627A.170M|doi=10.1051/0004-6361/201935605|s2cid=195798873|issn=0004-6361}}</ref><ref group="lower-alpha" name="VVV">VVV CL074는 산개성단이다.</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[아치스 성단|아치스]]-F6 ([[아치스 성단]]에 존재하는 WR 102ah)
| 2,239,000
| -11.135
| 25,000
| 15.75 (J 대역)
| 33,900
| {{SIMBAD link|FNG2002+6|SIMBAD}}
|<ref name="martins">{{저널 인용 | last1 = Martins | first1 = F. | last2 = Hillier | first2 = D. J. | last3 = Paumard | first3 = T. | last4 = Eisenhauer | first4 = F. | last5 = Ott | first5 = T. | last6 = Genzel | first6 = R. | doi = 10.1051/0004-6361:20078469 | title = The most massive stars in the Arches cluster | journal = Astronomy and Astrophysics | volume = 478 | pages = 219–233 | date = 2008 | issue = 1 |arxiv = 0711.0657 |bibcode = 2008A&A...478..219M | s2cid = 7509876 }}</ref><ref name=Figer/>
|-
| style="background: {{항성-색깔|WC}};" |[[아치스 성단|아치스]]-F9 ([[아치스 성단]]에 존재하는 WR 102ae)
| 2,239,000
| -11.135
| 25,000
| 16.1 (J 대역)
| 36,600
| {{SIMBAD link|FNG2002+9|SIMBAD}}
|<ref name="martins" /><ref name=Figer>{{저널 인용|last1=Figer|first1=Donald F.|last2=Najarro|first2=Francisco|last3=Gilmore|first3=Diane|last4=Morris|first4=Mark|last5=Kim|first5=Sungsoo S.|last6=Serabyn|first6=Eugene|last7=McLean|first7=Ian S.|last8=Gilbert|first8=Andrea M.|last9=Graham|first9=James R.|last10=Larkin|first10=James E.|last11=Levenson|first11=N. A.|date=2002-12-10|title=Massive Stars in the Arches Cluster|journal=The Astrophysical Journal|volume=581|issue=1|pages=258–275|arxiv=astro-ph/0208145|bibcode=2002ApJ...581..258F|doi=10.1086/344154|s2cid=119002004|issn=0004-637X}}</ref>
|-
| style="background: {{항성-색깔|WN}};" |[[HD 5980]] A ([[소마젤란 은하]]의 [[NGC 346]]에 존재)
| 2,239,000
| -11.135
| 200,000
| 11.31 (연성계 전체)
| 21,000-53,000
|{{SIMBAD link|HD+5980|SIMBAD}}
|<ref name="shenar">{{저널 인용|last1=Shenar|first1=T.|last2=Hainich|first2=R.|last3=Todt|first3=H.|last4=Sander|first4=A.|last5=Hamann|first5=W.-R.|last6=Moffat|first6=A. F. J.|last7=Eldridge|first7=J. J.|last8=Pablo|first8=H.|last9=Oskinova|first9=L. M.|last10=Richardson|first10=N. D.|year=2016|title=Wolf-Rayet stars in the Small Magellanic Cloud: II. Analysis of the binaries|journal=Astronomy & Astrophysics|volume=1604|page=A22|arxiv=1604.01022|bibcode=2016A&A...591A..22S|doi=10.1051/0004-6361/201527916|s2cid=119255408}}</ref><ref name="tycho2" /><ref group="lower-alpha">변광성, 1994년 분출 당시에는 밝기가 5배 더 높았다.(태양의 10,000,000배)</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[NGC 3603-C|HD 97950 C]]1 ([[NGC 3603]]의 [[HD 97950]]에 존재하는 WR 43c A)
|2,239,000
| -11.135
|24,000
|11.89 (연성계 전체)
|44,000
|{{SIMBAD link|HD+97950C|SIMBAD}}
|<ref name="crowther" /><ref name="melena2008" /><ref group=lower-alpha name=Binary/>
|-
| style="background: {{항성-색깔|O}};" | [[R136|R136b]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 2,239,000
| -11.135
| 165,000
| 13.24
| 35,500
|{{SIMBAD link|RMC136b|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[R145]] A ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|2,239,000
| -11.135
|163,000
|12.04 (연성계 전체)
|50,000
|{{SIMBAD link|RMC145|SIMBAD}}
|<ref name="shenar2016">{{저널 인용|last1=Shenar|first1=T.|display-authors=etal|year=2016|title=The Tarantula Massive Binary Monitoring project: II. A first SB2 orbital and spectroscopic analysis for the Wolf-Rayet binary R145|journal=Astronomy & Astrophysics|volume=598|page=A85|arxiv=1610.07614|bibcode=2017A&A...598A..85S|doi=10.1051/0004-6361/201629621|s2cid=118546102}}</ref><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WN}};" | [[Var 83]] ([[삼각형자리 은하]]에 존재)
| 2,239,000
| -11.135
| 3,000,000
| 16.027
| 18,000-37,000
| {{SIMBAD link|VHK+83|SIMBAD}}
|<ref name="Szeifert et al. 1996">{{저널 인용|author-link2=Roberta M. Humphreys|last1=Szeifert|first1=T.|last2=Humphreys|first2=R. M.|last3=Davidson|first3=K.|last4=Jones|first4=T. J.|last5=Stahl|first5=O.|last6=Wolf|first6=B.|last7=Zickgraf|first7=F.-J.|date=1996|title=HST and groundbased observations of the 'Hubble-Sandage' variables in M 31 and M 33|journal=Astronomy and Astrophysics|volume=314|pages=131–145|bibcode=1996A&A...314..131S}}</ref><ref>{{저널 인용|last1=Massey|first1=Philip|last2=Neugent|first2=Kathryn F.|last3=Smart|first3=Brianna M.|title=A Spectroscopic Survey of Massive Stars in M31 and M33|date=2016-08-19|journal=The Astronomical Journal|volume=152|issue=3|page=62|arxiv=1604.00112|bibcode=2016AJ....152...62M|doi=10.3847/0004-6256/152/3/62|s2cid=35672588|issn=1538-3881 |doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[CXOGC J174712.2-283121]] ([[은하중심]]에 존재하는 WR 102–10)
|2,188,000
| -11.11
|26,000
|17.06 (J 대역)
|35,000
|{{SIMBAD link|CXOGC+J174712.2-283121|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 1021]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|2,188,000
| -11.11
|164,000
|13.35
|39,800
|{{SIMBAD link|VFTS+1021|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[ST5-31]] ([[대마젤란 은하]]의 [[NGC 2074]]에 존재)
|2,168,000
| -11.1
|160,000
|12.273
|50,700
|{{SIMBAD link|ST92+5-31|SIMBAD}}
|<ref name=":42" /><ref>{{저널 인용|last1=Zaritsky|first1=Dennis|last2=Harris|first2=Jason|last3=Thompson|first3=Ian B.|last4=Grebel|first4=Eva K.|date=October 2004|title=The Magellanic Clouds Photometric Survey: The Large Magellanic Cloud Stellar Catalog and Extinction Map|journal=The Astronomical Journal|volume=128|issue=4|pages=1606–1614|arxiv=astro-ph/0407006|bibcode=2004AJ....128.1606Z|doi=10.1086/423910|issn=0004-6256|s2cid=119532934}}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[HD 268804]] ([[대마젤란 은하]]에 존재)
|2,148,000
| -11.09
|163,000
|11.21
|28,200
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+268804 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" | [[G0.058+0.014]] ([[은하중심]]에 존재)
| 2,138,000
| -11.085
| 26,000
|14.704 (J 대역)
|45,000
|{{SIMBAD link|MCD2010+G0.058%2B0.014|SIMBAD}}
|<ref name="mcd2010" />
|-
| style="background: {{항성-색깔|WC}};" |[[R145]] B ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|2,138,000
| -11.085
|163,000
|12.04 (연성계 전체)
|43,000
|{{SIMBAD link|RMC145|SIMBAD}}
|<ref name="shenar2016" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 89]] ([[HM 1]]에 존재)
| 2,138,000
| -11.085
| 9,500
| 11.02
| 39,800
|{{SIMBAD link|WR+89|SIMBAD}}
|<ref name="WN" /><ref name=zacharias/>
|-
| style="background: {{항성-색깔|O}};" | [[R136|R136a5]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 2,089,000
| -11.06
| 163,000
| 13.71
| 48,000
| {{SIMBAD link|RMC136a5|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WN}};" | [[AFGL 2298]] ([[은하면]] 근처에 존재)
| 2,000,000
| -11.013
| 33,000
|12.164 (J 대역)
|15,500-26,000
|{{SIMBAD link|AFGL+2298|SIMBAD}}
|<ref name="afgl2298">{{저널 인용|last1=Clark|first1=J. S.|last2=Crowther|first2=P. A.|last3=Larionov|first3=V. M.|last4=Steele|first4=I. A.|last5=Ritchie|first5=B. W.|last6=Arkharov|first6=A. A.|year=2009|title=Bolometric luminosity variations in the luminous blue variable AFGL2298|journal=Astronomy and Astrophysics|volume=507|issue=3|pages=1555–1565|arxiv=0909.4160|bibcode=2009A&A...507.1555C|doi=10.1051/0004-6361/200912358|s2cid=119187994}}</ref><ref name=2MASS/><ref group="lower-alpha">밝은 청색변광성, 최고 광도 기준.</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[아치스 성단|아치스]]-F1 ([[아치스 성단]]에 존재하는 WR 102ad)
| 1,995,000
| -11.01
| 25,000
|16.3 (J 대역)
| 33,200
|{{SIMBAD link|FNG2002+1|SIMBAD}}
|<ref name="martins" /><ref name=Figer/>
|-
| style="background: {{항성-색깔|WC}};" |[[아치스 성단|아치스]]-F4 ([[아치스 성단]]에 존재하는 WR 102al)
| 1,995,000
| -11.01
| 25,000
|15.63 (J 대역)
| 36,800
|{{SIMBAD link|FNG2002+4|SIMBAD}}
|<ref name="martins" /><ref name=Figer/>
|-
| style="background: {{항성-색깔|WC}};" |[[CXOGC J174656.3-283232]] ([[은하중심]]에 존재하는 WR 102–8)
|1,995,000
| -11.01
|26,000
|16.74 (J 대역)
|30,000
|{{SIMBAD link|CXOGC+J174656.3-283232|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|WN}};" |[[LBV 1806-20]] ([[은하중심]]의 [[G10.0–0.3]]에 존재)
| 1,995,000
| -11.01
| 28,000
|13.66 (J 대역)
| 18,000-32,000
|{{SIMBAD link|LBV+1806-20|SIMBAD}}
|<ref name="abdalla">{{저널 인용|last1=Abdalla|first1=H.|last2=Abramowski|first2=A.|last3=Aharonian|first3=F.|last4=Ait Benkhali|first4=F.|last5=Akhperjanian|first5=A. G.|last6=Angüner|first6=E. O.|last7=Arrieta|first7=M.|last8=Aubert|first8=P.|last9=Backes|first9=M.|last10=Balzer|first10=A.|last11=Barnard|first11=M.|last12=Becherini|first12=Y.|last13=Becker Tjus|first13=J.|last14=Berge|first14=D.|last15=Bernhard|first15=S.|last16=Bernlöhr|first16=K.|last17=Birsin|first17=E.|last18=Blackwell|first18=R.|last19=Böttcher|first19=M.|last20=Boisson|first20=C.|last21=Bolmont|first21=J.|last22=Bordas|first22=P.|last23=Bregeon|first23=J.|last24=Brun|first24=F.|last25=Brun|first25=P.|last26=Bryan|first26=M.|last27=Bulik|first27=T.|last28=Capasso|first28=M.|last29=Carr|first29=J.|last30=Casanova|first30=S.|display-authors=29|year=2018|title=Extended VHE γ-ray emission towards SGR1806−20, LBV 1806−20, and stellar cluster Cl* 1806−20|journal=Astronomy & Astrophysics|volume=612|page=A11|arxiv=1606.05404|bibcode=2018A&A...612A..11H|doi=10.1051/0004-6361/201628695|s2cid=118345803}}</ref><ref name=2MASS/><ref group="lower-alpha">G10.0-0.3은 은하중심의 전파 성운이다..</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[머서 81]]-2 ([[G338.4+0.2]]의 [[머서 81]]에 존재하는 WR 76–7)
|1,995,000
| -11.01
|35,900
|13.25 (J 대역)
|36,000
|{{SIMBAD link|DDN2012+2|SIMBAD}}
|<ref>{{저널 인용|last1=Davies|first1=Ben|last2=de la Fuente|first2=Diego|last3=Najarro|first3=Francisco|last4=Hinton|first4=Jim A.|last5=Trombley|first5=Christine|last6=Figer|first6=Donald F.|last7=Puga|first7=Elena|date=21 January 2012|title=A newly discovered young massive star cluster at the far end of the Galactic Bar: A young cluster at the far end of the Bar|journal=Monthly Notices of the Royal Astronomical Society|volume=419|issue=3|pages=1860–1870|arxiv=1111.2630|bibcode=2012MNRAS.419.1860D|doi=10.1111/j.1365-2966.2011.19840.x|issn=0035-8711|s2cid=59405479}}</ref><ref group="lower-alpha">머서 81은 분자운 G338.4+0.2의 산개성단이다.</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[VFTS 545]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,995,000
| -11.01
|164,000
|13.32
|47,300
|{{SIMBAD link|VFTS+545|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 147|WR 147S]] ([[백조자리 OB2]]에 존재)
| 1,995,000
| -11.01
| 5,800
| 13.86
| 39,800
|{{SIMBAD link|WR+147|SIMBAD}}
|<ref name="WN" /><ref>{{저널 인용|last1=Niemela|first1=Virpi S.|last2=Shara|first2=Michael M.|last3=Wallace|first3=Debra J.|last4=Zurek|first4=David R.|last5=Moffat|first5=Anthony F. J.|date=1998|title=Hubble Space Telescope Detection of Optical Companions of WR 86, WR 146, and WR 147: Wind Collision Model Confirmed|journal=The Astronomical Journal|volume=115|issue=5|pages=2047–2052|bibcode=1998AJ....115.2047N|doi=10.1086/300320|s2cid=3606924 |doi-access=free}}</ref>
|-
| style="background: {{항성-색깔|B}};" | [[10584-9-1]] ([[메시에 81]]에 존재)
| 1,977,000
| -11.0
| 11,842,000
| 19.1
| 18,000
|{{SIMBAD link|%5BHSG2019%5D%2010584-9.1|SIMBAD}}
|<ref name="humphreys2019"/>
|-
|[[2MASS J04542610-6911022]] ([[대마젤란 은하]]에 존재)
|1,959,000
| -10.99
|163,000
|12.68
|37,200
|[http://simbad.cds.unistra.fr/simbad/sim-id?Ident=2MASS+J04542610-6911022 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|WC}};" |[[DBSB 179]]-15 ([[G347.6+0.2]]의 [[DBSB 179]]에 존재하는 WR 84–6)
|1,950,000
| -10.985
|25,800
|12.5 (J 대역)
|37,000
|{{SIMBAD link|BIH2008+obj15|SIMBAD}}
|<ref name=":18">{{저널 인용|last1=Borissova|first1=J.|last2=Georgiev|first2=L.|last3=Hanson|first3=M. M.|last4=Clarke|first4=J. R. A.|last5=Kurtev|first5=R.|last6=Ivanov|first6=V. D.|last7=Penaloza|first7=F.|last8=Hillier|first8=D. J.|last9=Zsargó|first9=J.|date=October 2012|title=Obscured clusters: IV. The most massive stars in [DBS2003] 179|journal=Astronomy & Astrophysics|volume=546|page=A110|arxiv=1209.6370|bibcode=2012A&A...546A.110B|doi=10.1051/0004-6361/201118348|issn=0004-6361|s2cid=119303823}}</ref><ref name=":19">{{저널 인용|last1=Borissova|first1=J.|last2=Ivanov|first2=V. D.|last3=Hanson|first3=M. M.|last4=Georgiev|first4=L.|last5=Minniti|first5=D.|last6=Kurtev|first6=R.|last7=Geisler|first7=D.|date=September 2008|title=The young Galactic star cluster [DBS2003] 179|journal=Astronomy & Astrophysics|volume=488|issue=1|pages=151–159|arxiv=0806.4584|bibcode=2008A&A...488..151B|doi=10.1051/0004-6361:20079255|issn=0004-6361|s2cid=14942349}}</ref><ref group="lower-alpha" name="DBSB179">DBSB 179는 분자운 G347.6+0.2의 산개성단이다.</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[G0.114+0.021]] ([[은하중심]]에 존재하는 WR 102–12)
| 1,950,000
| -10.985
| 26,000
|16.672 (J 대역)
|40,000
|{{SIMBAD link|MCD2010+G0.114%2B0.021|SIMBAD}}
|<ref name="mcd2010" />
|-
| style="background: {{항성-색깔|WC}};" |[[AB6 (항성)|AB6]] A ([[소마젤란 은하]]의 [[NGC 371]]에 존재)
|1,905,000
| -10.96
|197,000
|12.3 (연성계 전체)
|80,000
|{{SIMBAD link|SMC+AB+6|SIMBAD}}
|<ref name="shenar" /><ref name=Bonanos2010>{{저널 인용|last1=Bonanos|first1=A. Z.|last2=Lennon|first2=D. J.|last3=Köhlinger|first3=F.|last4=van Loon|first4=J. Th.|last5=Massa|first5=D. L.|last6=Sewilo|first6=M.|last7=Evans|first7=C. J.|last8=Panagia|first8=N.|last9=Babler|first9=B. L.|last10=Block|first10=M.|last11=Bracker|first11=S.|title=Spitzersage-SMC Infrared Photometry of Massive Stars in the Small Magellanic Cloud|date=2010-08-01|journal=The Astronomical Journal|volume=140|issue=2|pages=416–429|arxiv=1004.0949|bibcode=2010AJ....140..416B|doi=10.1088/0004-6256/140/2/416|hdl=1887/61635|s2cid=119290443|issn=0004-6256}}</ref>
|-
| style="background: {{항성-색깔|O}};" | [[R136|R136a4]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,905,000
| -10.96
| 163,000
| 13.41
| 50,000
| {{SIMBAD link|RMC136a4|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[웨스터하우트 49]]-1 ([[웨스터하우트 49]]에 존재)
| 1,905,000
| -10.96
| 36,200
| 15.531 (J 대역)
| 44,700
| {{SIMBAD link|WBB2016+1|SIMBAD}}
|<ref name="Wu2016" /><ref name=2MASS/>
|-
| style="background: {{항성-색깔|WC}};" |[[WR 22]] A ([[용골자리 성운]]의 [[보훔 10]]에 존재)
| 1,905,000
| -10.96
| 8,200
| style="background: lightblue;" | 6.42 (연성계 전체)
| 44,700
| {{SIMBAD link|WR+22|SIMBAD}}
|<ref name="WN" /><ref name="ducati" /><ref group="lower-alpha">보훔 10은 용골자리 성운의 산개성단이다.</ref>
|-
| style="background: {{항성-색깔|B}};" |[[HD 269219]] ([[대마젤란 은하]]에 존재)
| 1,888,000
| -10.95
| 163,000
| 10.87
| 28,200
| [https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+269219 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" | [[HSH95-36]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,862,000
| -10.935
| 163,000
| 14.41
| 49,500
| {{SIMBAD link|HSH95+36|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[Hen 3-519]] ([[푸른 거품 성운]]에 존재하는 WR 31a)
| 1,820,000
| -10.91
| 24,000
| 10.85
| 30,200
| {{SIMBAD link|Hen+3-519|SIMBAD}}
|<ref name=vangenderen>{{저널 인용 |bibcode=2001A&A...366..508V |title=S Doradus variables in the Galaxy and the Magellanic Clouds |journal=Astronomy and Astrophysics |volume=366 |issue=2 |pages=508–531 |last1=Van Genderen |first1=A. M. |year=2001 |doi=10.1051/0004-6361:20000022|doi-access=free }}[http://vizier.cfa.harvard.edu/viz-bin/VizieR-6?-out.form=%2bH&-source=33660508&-out.all&-corr=PFK=Name&-out.max=9999&Name==He3-519 Vizie database entry]</ref><ref name="tycho2">{{저널 인용|last1=Høg|first1=E.|last2=Fabricius|first2=C.|last3=Makarov|first3=V. V.|last4=Urban|first4=S.|last5=Corbin|first5=T.|last6=Wycoff|first6=G.|last7=Bastian|first7=U.|last8=Schwekendiek|first8=P.|last9=Wicenec|first9=A.|year=2000|title=The Tycho-2 catalogue of the 2.5 million brightest stars|journal=Astronomy and Astrophysics|volume=355|page=L27|bibcode=2000A&A...355L..27H|doi=10.1888/0333750888/2862|isbn=0333750888}}</ref><ref group="lower-alpha">푸른 거품 성운은 Hen 3-519 주변의 볼프-레이에 성운이다.</ref>
|-
| [[W61 3-20]] ([[대마젤란 은하]]에 존재)
| 1,820,000
| -10.91
| 163,000
| 13.55
| 39,800
| [https://simbad.cds.unistra.fr/simbad/sim-id?Ident=w61+3-20 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" |[[웨스터하우트 51]]-57 ([[웨스터하우트 51]]에 존재)
| 1,820,000
| -10.91
| 20,000
| 16.958 (J 대역)
| 42,700
| {{SIMBAD link|2MASS+J19233374&2B1429536|SIMBAD}}
|<ref name=":22">{{저널 인용|last1=Bik|first1=A.|last2=Henning|first2=Th.|last3=Wu|first3=S.-W.|last4=Zhang|first4=M.|last5=Brandner|first5=W.|last6=Pasquali|first6=A.|last7=Stolte|first7=A.|date=April 2019|title=Near-infrared spectroscopy of the massive stellar population of W51: evidence for multi-seeded star formation|journal=Astronomy & Astrophysics|volume=624|pages=A63|arxiv=1902.05460|bibcode=2019A&A...624A..63B|doi=10.1051/0004-6361/201935061|issn=0004-6361|s2cid=118711844}}</ref><ref name=2MASS/>
|-
| style="background: {{항성-색깔|WN}};" |[[LGGS J004051.59+403303.0]] ([[안드로메다 은하]]에 존재)
| 1,803,000
| -10.9
| 2,500,000
| 16.989
| 18,000-24,000
| {{SIMBAD link|LGGS+J004051.59%2B403303.0|SIMBAD}}
|<ref name="m31" /><ref name=Massey2006/>
|-
| style="background: {{항성-색깔|WN}};" |[[Wray 17-96|MSX5C G358.5391+00.1305]] ([[Wray 17-96]]에 존재)
| 1,800,000
| -10.898
| 15,000
| 15
| 13,000
| {{SIMBAD link|MSX5C+G358.5391%2B00.1305|SIMBAD}}
|<ref name=egan>{{저널 인용 |last=Egan |first=Michael P. |display-authors=etal |year=2002 |title=An Infrared Ring Nebula around MSX5C G358.5391+00.1305: The True Nature of Suspected Planetary Nebula Wray 17-96 Determined via Direct Imaging and Spectroscopy |journal=The Astrophysical Journal |volume=572 |issue=1 |pages=288–299 |doi=10.1086/340222 |bibcode=2002ApJ...572..288E|doi-access=free }}</ref><ref name="zacharias" /><ref group="lower-alpha">엄밀히 말하면 MSX5C G358.5391+00.1305가 별의 이름이고 Wray 17-96이 성운의 이름이다.</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[HD 5980]] B ([[소마젤란 은하]]의 [[NGC 346]]에 존재)
| 1,778,000
| -10.885
| 200,000
| 11.31 (연성계 전체)
| 45,000
|{{SIMBAD link|HD+5980|SIMBAD}}
|<ref name="shenar" /><ref name="melena2008" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 130]] ([[백조자리 OB3]]애 존재)
| 1,778,000
| -10.885
| 21,700
| 12.13
| 44,700
|{{SIMBAD link|WR+130|SIMBAD}}
|<ref name="WN" /><ref name="zacharias" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 21a]] A ([[웨스터룬드 2]]에 존재하는 [[폭주성]])
|1,778,000
| -10.885
|14,300
|12.661 (연성계 전체)
|45,000
|{{SIMBAD link|WR+21a|SIMBAD}}
|<ref name=tramper>{{저널 인용|bibcode=2016MNRAS.455.1275T|arxiv=1510.03609|title=The mass of the very massive binary WR21a|journal=Monthly Notices of the Royal Astronomical Society|volume=455|issue=2|pages=1275–1281|last1=Tramper|first1=F.|last2=Sana|first2=H.|last3=Fitzsimons|first3=N. E.|last4=De Koter|first4=A.|last5=Kaper|first5=L.|last6=Mahy|first6=L.|last7=Moffat|first7=A.|year=2016|doi=10.1093/mnras/stv2373|s2cid=44364798}}</ref><ref name="zacharias" />
|-
| style="background: {{항성-색깔|WC}};" |[[CXOGC J174536.1-285638]] ([[은하중심]]에 존재하는 WR 101–1)
| 1,738,000
| -10.86
| 26,000
| 15.55 (J 대역)
| 30,000
| {{SIMBAD link|CXOGC+J174536.1-285638|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|WC}};" |[[머서 30]]-7 A ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재하는 WR 46-5 A)
| 1,738,000
| -10.86
| 40,000
| 11.516 (J 대역)
| 41,400
| {{SIMBAD link|DNB2016+Mc30-7|SIMBAD}}
|<ref name=":17" /><ref group=lower-alpha name=Mc30/>
|-
| style="background: {{항성-색깔|O}};" | [[R136|R136a6]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,738,000
| -10.86
| 163,000
| 13.35
| 52,000
| {{SIMBAD link|RMC136a6|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" | [[VFTS 506]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,738,000
| -10.86
| 164,000
| 13.31
| 47,300
| {{SIMBAD link|VFTS+506|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|B}};" |[[HD 35342]] B ([[대마젤란 은하]]에 존재)
| 1,722,000
| -10.85
| 163,000
| 11.28
| 24,000
| [https://simbad.cds.unistra.fr/simbad/sim-id?Ident=HD+35342B SIMBAD]
|<ref name=":2" />
|-
| [[CPD -69 471]] ([[대마젤란 은하]]에 존재)
| 1,706,000
| -10.84
| 163,000
| 12.37
| 42,700
| [https://simbad.cds.unistra.fr/simbad/sim-id?Ident=cpd+-69+471 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|WC}};" |[[DBSB 179]]-20 ([[G347.6+0.2]]의 [[DBSB 179]]에 존재하는 WR 84–1)
| 1,698,000
| -10.835
| 25,800
| 12.37 (J 대역)
| 35,000
| {{SIMBAD link|BIH2008+obj20|SIMBAD}}
|<ref name=":18" /><ref name=":19" /><ref group=lower-alpha name=DBSB179/>
|-
| style="background: {{항성-색깔|WC}};" | [[R147]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,698,000
| -10.835
| 164,000
| 13.02
| 50,000
| {{SIMBAD link|RMC147|SIMBAD}}
|<ref name="Hainich2014" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" | [[VFTS 16]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,698,000
| -10.835
| 164,000
| 13.55
| 53,100
| {{SIMBAD link|VFTS+16|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|B}};" |[[백조자리 OB2-12|백조자리 OB2 #12]] A ([[백조자리 OB2]]에 존재)
| 1,660,000
| -10.81
| 5,000
| 11.702 (연성계 전체)
| 13,700
| {{SIMBAD link|Cyg+OB2+12|SIMBAD}}
|<ref name=oskinova>{{저널 인용|bibcode=2017ApJ...845...39O|title=On the Binary Nature of Massive Blue Hypergiants: High-resolution X-Ray Spectroscopy Suggests That Cyg OB2 12 is a Colliding Wind Binary|journal=The Astrophysical Journal|volume=845|issue=1|page=39|last1=Oskinova|first1=L. M.|last2=Huenemoerder|first2=D. P.|last3=Hamann|first3=W. -R.|last4=Shenar|first4=T.|last5=Sander|first5=A. A. C.|last6=Ignace|first6=R.|last7=Todt|first7=H.|last8=Hainich|first8=R.|year=2017|arxiv=1707.04473|doi=10.3847/1538-4357/aa7e79|s2cid=119537489 |doi-access=free }}</ref><ref name="Laur">{{저널 인용|last1=Laur|first1=Jaan|last2=Kolka|first2=Indrek|last3=Eenmäe|first3=Tõnis|last4=Tuvikene|first4=Taavi|last5=Leedjärv|first5=Laurits|date=2017|title=Variability survey of brightest stars in selected OB associations|journal=Astronomy & Astrophysics|volume=598|page=A108|arxiv=1611.02452|bibcode=2017A&A...598A.108L|doi=10.1051/0004-6361/201629395|s2cid=119076598|issn=0004-6361}}</ref><ref group=lower-alpha name=Binary/>
|-
| [[PGMW 3120]] ([[대마젤란 은하]]에 존재)
| 1,644,000
| -10.8
| 163,000
| 12.47
| 39,800
| [https://simbad.cds.unistra.fr/simbad/sim-id?Ident=pgmw+3120 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" |[[NGC 3603|Sher 18]] ([[HD 97950]]의 [[HD 97950]]에 존재)
| 1,644,000
| -10.8
| 25,000
| 12.51
| 39,500
| {{SIMBAD link|Cl*+NGC+3603+Sher+18|SIMBAD}}
|<ref name="melena2008" /><ref name=":16">{{저널 인용|last=Moffat|first=A. F. J.|date=October 1974|title=On the distance and reddening of the massive H II region NGC 3603|journal=Astronomy and Astrophysics|volume=35|page=315|bibcode=1974A&A....35..315M|issn=0004-6361|s2cid=115549707}}</ref>
|-
| style="background: {{항성-색깔|O}};" |[[NGC 3603|Sher 47]] ([[HD 97950]]의 [[HD 97950]]에 존재)
| 1,644,000
| -10.8
| 25,000
| 12.67
| 44,000
| {{SIMBAD link|Cl*+NGC+3603+Sher+47|SIMBAD}}
|<ref name="melena2008" /><ref name=":16" />
|-
| style="background: {{항성-색깔|O}};" |[[머서 23]]-1 ([[은하면]] 근처의 [[머서 23]]에 존재)
| 1,622,000
| -10.785
| 21,200
| 10.615 (J 대역)
| 35,000
| {{SIMBAD link|HKB2010b+Obj1|SIMBAD}}
|<ref name=":20" /><ref name=2MASS/><ref group=lower-alpha name=Mc23/>
|-
| style="background: {{항성-색깔|WC}};" |[[VFTS 1017]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,622,000
| -10.785
| 164,000
| 14.52
| 50,100
| {{SIMBAD link|VFTS+1017|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 87]] ([[HM 1]]에 존재)
| 1,622,000
| -10.785
| 9,500
| 11.83
| 44,700
|{{SIMBAD link|WR+87|SIMBAD}}
|<ref name="WN" /><ref name="zacharias" />
|-
|[[HD 269896]] ([[대마젤란 은하]]에 존재)
|1,600,000
| -10.77
|163,000
|11.36
|29,500
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+269896 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|WN}};" | [[안드로메다자리 AF]] ([[안드로메다 은하]]에 존재)
| 1,585,000
| -10.76
| 2,500,000
| 17.325
| 28,000
| {{SIMBAD link|AF+Andromedae|SIMBAD}}
|<ref name="Szeifert et al. 1996" /><ref name=Massey2006/>
|-
| style="background: {{항성-색깔|WC}};" |[[아치스 성단|아치스]]-F12 ([[아치스 성단]]에 존재하는 WR 102af)
| 1,585,000
| -10.76
| 25,000
| 16.4 (J 대역)
| 36,900
| {{SIMBAD link|FNG2002+12|SIMBAD}}
|<ref name="martins" /><ref name=Figer/>
|-
| style="background: {{항성-색깔|O}};" |[[HSH95-18]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,585,000
| -10.76
|163,000
|13.87
|47,000
|{{SIMBAD link|HSH95+18|SIMBAD}}
|<ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[다섯쌍둥이 성단|LHO 110]] ([[다섯쌍둥이 성단]]에 존재하는 WR 102df)
| 1,585,000
| -10.76
| 26,000
|13.87 (J 대역)
| 25,100
|{{SIMBAD link|LHO+110|SIMBAD}}
|<ref name="quintuplet" /><ref name="qc" />
|-
| style="background: {{항성-색깔|WC}};" |[[R140a1]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,585,000
| -10.76
|163,000
|12.12 (연성계 전체)
|34,000
|{{SIMBAD link|RMC140a1|SIMBAD}}
|<ref name="Doran2013" />
|-
|[[BI 265]] ([[대마젤란 은하]]에 존재)
|1,585,000
| -10.76
|163,000
|12.38
|40,700
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=bi+265 SIMBAD]
|
|-
| style="background: {{항성-색깔|WC}};" |[[VFTS 457]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,585,000
| -10.76
|164,000
|13.74
|39,800
|{{SIMBAD link|VFTS+457|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 107]] ([[궁수자리 OB1]]에 존재)
| 1,585,000
| -10.76
| 9,400
| 13.51
| 50,100
| {{SIMBAD link|WR+107|SIMBAD}}
|<ref name="WN" /><ref name="zacharias" />
|-
| style="background: {{항성-색깔|O}};" |[[WR 140]] B ([[백조자리 OB1]]에 존재)
| 1,585,000
| -10.76
| 5,300
| 6.85 (연성계 전체)
| 35,000
| {{SIMBAD link|WR+140|SIMBAD}}
|<ref>{{저널 인용|last=Williams|first=Peredur|date=2011|title=Results from the 2009 campaign on WR 140|journal=Société Royale des Sciences de Liège|volume=80|pages=595–609|bibcode=2011BSRSL..80..595W}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 148]] A ([[은하면]]의 [[폭주성]])
| 1,585,000
| -10.76
| 27,100
| 10.3 (연성계 전체)
| 39,800
|{{SIMBAD link|WR+148|SIMBAD}}
|<ref name="WN" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[CXOGC J174617.0-285131]] ([[은하중심]]에 존재)
|1,549,000
| -10.735
|26,000
|14.98 (J 대역)
|40,000
|{{SIMBAD link|CXOGC+J174617.0-285131|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|O}};" |[[CXOGC J174725.3-282709]] ([[은하중심]]에 존재)
|1,549,000
| -10.735
|26,000
|16.37 (J 대역)
|30,000
|{{SIMBAD link|CXOGC+J174725.3-282709|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|O}};" |[[Sk -68° 137]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,549,000
| -10.735
|160,000
|13.346
|55,000
|{{SIMBAD link|Sk+-68+137|SIMBAD}}
|<ref name="Walborn">{{저널 인용 |last1=Walborn |first1=N. R. |last2=Morrell |first2=N. I. |last3=Howarth |first3=I. D. |last4=Crowther |first4=P. A. |last5=Lennon |first5=D. J. |last6=Massey |first6=P. |last7=Arias |first7=J. I. |year=2004 |title=A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds |journal=The Astrophysical Journal |volume=608 |issue=2 |pages=1028–1038 |arxiv=astro-ph/0403557 |bibcode=2004ApJ...608.1028W |doi=10.1086/420761 |s2cid=16656083}}</ref><ref name=Bonanos2009>{저널 인용|last1=Bonanos|first1=A. Z.|last2=Massa|first2=D. L.|last3=Sewilo|first3=M.|last4=Lennon|first4=D. J.|last5=Panagia|first5=N.|last6=Smith|first6=L. J.|last7=Meixner|first7=M.|last8=Babler|first8=B. L.|last9=Bracker|first9=S.|last10=Meade|first10=M. R.|last11=Gordon|first11=K. D.|title=Spitzersage Infrared Photometry of Massive Stars in the Large Magellanic Cloud|date=2009-10-01|journal=The Astronomical Journal|volume=138|issue=4|pages=1003–1021|arxiv=0905.1328|bibcode=2009AJ....138.1003B|doi=10.1088/0004-6256/138/4/1003|s2cid=14056495|issn=0004-6256}}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[다섯쌍둥이 성단|WR 102i]] ([[다섯쌍둥이 성단]]에 존재)
| 1,549,000
| -10.735
| 26,000
|14.31 (J 대역)
| 31,600
|{{SIMBAD link|WR+102i|SIMBAD}}
|<ref name="quintuplet" /><ref name="qc" />
|-
| style="background: {{항성-색깔|WC}};" |[[NGC 3603-A1|HD 97950 A1b]] ([[NGC 3603]]의 [[HD 97950]]에 존재하는 WR 43a B)
| 1,514,000
| -10.71
| 24,000
| 11.18 (연성계 전체)
| 40,000
|{{SIMBAD link|Cl*+NGC+3603+BLW+A1|SIMBAD}}
|<ref name="crowther" /><ref name="melena2008" />
|-
| style="background: {{항성-색깔|O}};" |[[웨스터하우트 49]]-3 ([[웨스터하우트 49]]에 존재)
|1,514,000
| -10.71
|36,200
|16.689 (J 대역)
|40,700
|{{SIMBAD link|WBB2016+3|SIMBAD}}
|<ref name="Wu2016" /><ref name=2MASS/>
|-
| style="background: {{항성-색깔|WC}};" |[[Brey 21]] A ([[대마젤란 은하]]의 [[NGC 1910]]에 존재)
|1,500,000
| -10.7
|165,000
|11.29 (연성계 전체)
|71,000
|{{SIMBAD link|Brey+21|SIMBAD}}
|<ref name=":42" /><ref name="zacharias" />
|-
| style="background: {{항성-색깔|O}};" |[[HD 97950]] A2 ([[NGC 3603]]의 [[HD 97950]]에 존재 )
|1,500,000
| -10.7
|24,000
|12.53
|46,500
|{{SIMBAD link|Cl*+NGC+3603+BLW+A2|SIMBAD}}
|<ref name="melena2008" /><ref name=":16" />
|-
| style="background: {{항성-색깔|O}};" |[[HM 1]]-6 ([[HM 1]]에 존재)
|1,500,000
| -10.7
|11,000
|11.64
|44,700
|{{SIMBAD link|Cl+HM+1+6|SIMBAD}}
|<ref name="Massey et al. 2001" /><ref name=Reed>{{저널 인용|last=Reed|first=B. Cameron|date=2003|title=Catalog of Galactic OB Stars|journal=The Astronomical Journal|volume=125|issue=5|pages=2531–2533|bibcode=2003AJ....125.2531R|doi=10.1086/374771|s2cid=121285799 |issn=0004-6256|doi-access=free}}</ref>
|-
| style="background: {{항성-색깔|O}};" | [[LGGS J013245.41+303858.3]] ([[삼각형자리 은하]]에 존재)
| 1,500,000
| -10.7
| 3,000,000
|17.612
| 34,000
|{{SIMBAD link|LGGS+J013245.41%2B303858.3|SIMBAD}}
|<ref name="humphreys2017">{{저널 인용|author-link1=Roberta M. Humphreys|last1=Humphreys|first1=Roberta M.|last2=Davidson|first2=Kris|last3=Hahn|first3=David|last4=Martin|first4=John C.|last5=Weis|first5=Kerstin|date=2017-07-06|title=Luminous and Variable Stars in M31 and M33 V. The Upper HR Diagram|journal=The Astrophysical Journal|volume=844|issue=1|page=40|arxiv=1707.01916|bibcode=2017ApJ...844...40H|doi=10.3847/1538-4357/aa7cef|s2cid=119357524 |doi-access=free }}</ref><ref name=Massey2006/>
|-
| style="background: {{항성-색깔|O}};" |[[NGC 346]]-W1 ([[소마젤란 은하]]의 [[NGC 346]]에 존재)
|1,500,000
| -10.7
|200,000
|12.57
|43,400
|{{SIMBAD link|Cl*+NGC+346+W+1|SIMBAD}}
|<ref name=":42" /><ref name=Bonanos2010 />
|-
| style="background: {{항성-색깔|O}};" |[[Sk -65° 47]] ([[대마젤란 은하]]의 [[NGC 1923]]에 존재)
|1,500,000
| -10.7
|160,000
|12.466
|47,800
|{{SIMBAD link|Sk+-65+47|SIMBAD}}
|<ref name=":42" /><ref name=Bonanos2009 />
|-
| style="background: {{항성-색깔|O}};" |[[Sk 80]] ([[소마젤란 은하]]의 [[NGC 346]]에 존재)
| 1,500,000
| -10.7
| 200,000
| 12.31
| 38,900
| {{SIMBAD link|Sk+80|SIMBAD}}
|<ref name=":42" /><ref>{{저널 인용|last1=Evans|first1=C. J.|last2=Lennon|first2=D. J.|last3=Smartt|first3=S. J.|last4=Trundle|first4=C.|date=September 2006|title=The VLT-FLAMES survey of massive stars: observations centered on the Magellanic Cloud clusters NGC 330, NGC 346, NGC 2004, and the N11 region|journal=Astronomy & Astrophysics|volume=456|issue=2|pages=623–638|arxiv=astro-ph/0606405|bibcode=2006A&A...456..623E|doi=10.1051/0004-6361:20064988|issn=0004-6361|s2cid=13160849}}</ref>
|-
| style="background: {{항성-색깔|B}};" | [[10584-4-1]] ([[메시에 81]]에 존재)
| 1,500,000
| -10.7
| 11,842,000
| 19.68
| 19,671
|{{SIMBAD link|%5BHSG2019%5D%2010584-4.1|SIMBAD}}
|<ref name="humphreys2019"/>
|-
| style="background: {{항성-색깔|O}};" |[[HD 93129]] Aa ([[용골자리 성운]]의 [[트럼플러 14]]에 존재)
| 1,479,000
| -10.685
| 7,500
| 6.9 (연성계 전체)
| 42,500
| {{SIMBAD link|HD+93129A|SIMBAD}}
|<ref name=smith>{{저널 인용|bibcode=2006MNRAS.367..763S|arxiv=astro-ph/0601060|title=A census of the Carina Nebula - I. Cumulative energy input from massive stars|journal=Monthly Notices of the Royal Astronomical Society|volume=367|issue=2|pages=763–772|last1=Smith|first1=Nathan|year=2006|doi=10.1111/j.1365-2966.2006.10007.x|s2cid=14060690}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" | [[R136|R136a8]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,479,000
| -10.685
| 163,000
| 14.42
| 49,500
| {{SIMBAD link|RMC136a8|SIMBAD}}
|<ref name="Brands2022" /><ref name="crowther2016">{{저널 인용|last1=Crowther|first1=Paul A.|last2=Caballero-Nieves|first2=S. M.|last3=Bostroem|first3=K. A.|last4=Maíz Apellániz|first4=J.|last5=Schneider|first5=F. R. N.|last6=Walborn|first6=N. R.|last7=Angus|first7=C. R.|last8=Brott|first8=I.|last9=Bonanos|first9=A.|last10=De Koter|first10=A.|last11=De Mink|first11=S. E.|year=2016|title=The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of He II λ1640 in young star clusters|journal=Monthly Notices of the Royal Astronomical Society|volume=458|issue=1|pages=624–659|arxiv=1603.04994|bibcode=2016MNRAS.458..624C|doi=10.1093/mnras/stw273|first17=D. J.|author11-link=Selma de Mink|first20=J. S.|last20=Vink|first19=H.|last19=Sana|first18=J.|last18=Puls|last12=Evans|first12=C. J.|first16=N.|last16=Langer|first15=I. D.|last15=Howarth|first14=A.|last14=Herrero|first13=G.|last13=Gräfener|last17=Lennon}}</ref>
|-
|[[SK -67 150]] ([[대마젤란 은하]]에 존재)
|1,472,000
| -10.68
|163,000
|12.24
|41,700
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=sk+-67+150 SIMBAD]
|<ref name=":2" />
|-
|[[HCD2002 107|[HCD2002] 107]] ([[대마젤란 은하]]에 존재)
|1,445,000
| -10.66
|163,000
|13.79
|40,700
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=%5Bhcd2002%5D+107 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|WC}};" |[[VFTS 542]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,445,000
| -10.66
|164,000
|13.49
|44,700
|{{SIMBAD link|VFTS+542|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[AB8 (항성)|AB8]] A ([[소마젤란 은하]]의 [[NGC 602]]에 존재)
| 1,413,000
| -10.635
| 197,000
| 12.9 (연성계 전체)
| 141,000
|{{SIMBAD link|SMC+AB+8|SIMBAD}}
|<ref name="shenar" /><ref>{{저널 인용|last=Massey|first=Philip|date=July 2002|title=A UBVR CCD Survey of the Magellanic Clouds|journal=The Astrophysical Journal Supplement Series|volume=141|issue=1|pages=81–122|arxiv=astro-ph/0110531|bibcode=2002ApJS..141...81M|doi=10.1086/338286|s2cid=119447348|issn=0067-0049}}</ref>
|-
| style="background: {{항성-색깔|O}};" |[[아치스 성단|아치스]]-F15 ([[아치스 성단]]에 존재)
| 1,413,000
| -10.635
| 25,000
|16.12 (J 대역)
| 35,600
|{{SIMBAD link|FNG2002+15|SIMBAD}}
|<ref name="martins" /><ref name=Figer/>
|-
| style="background: {{항성-색깔|WC}};" |[[CXOGC J174550.2-284911]] ([[은하중심]]의 WR 102–4)
|1,413,000
| -10.635
|26,000
|15.24 (J 대역)
|30,000
|{{SIMBAD link|CXOGC+J174550.2-284911|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|WC}};" |[[DBSB 179]]-4 ([[G347.6+0.2]]의 [[DBSB 179]]에 존재하는 WR 84–7)
|1,413,000
| -10.635
|25,800
|12.25 (J 대역)
|30,000
|{{SIMBAD link|BIH2008+obj4|SIMBAD}}
|<ref name=":18" /><ref name=":19" /><ref group=lower-alpha name=DBSB179/>
|-
| style="background: {{항성-색깔|O}};" | [[LGGS J013235.25+303017.6]] ([[삼각형자리 은하]]에 존재)
| 1,413,000
| -10.635
|3,000,000
|18.007
|33,000
|{{SIMBAD link|LGGS+J013235.25%2B303017.6|SIMBAD}}
|<ref name=Kourniotis/><ref>{{저널 인용|last1=Massey|first1=Philip|last2=Olsen|first2=K. A. G.|last3=Hodge|first3=Paul W.|last4=Jacoby|first4=George H.|last5=McNeill|first5=Reagin T.|last6=Smith|first6=R. C.|last7=Strong|first7=Shay B.|date=2007|title=A Survey of Local Group Galaxies Currently Forming Stars. II. UBVRI Photometry of Stars in Seven Dwarfs and a Comparison of the Entire Sample|journal=The Astronomical Journal|volume=133|issue=5|pages=2393–2417|arxiv=astro-ph/0702236|bibcode=2007AJ....133.2393M|doi=10.1086/513319|s2cid=119456878|issn=0004-6256}}</ref>
|-
| style="background: {{항성-색깔|O}};" | [[멜닉 33Na]] A ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,413,000
| -10.635
|164,000
|13.79 (연성계 전체)
|50,000
|{{SIMBAD link|Cl*+NGC+2070+MH+887|SIMBAD}}
|<ref name=Bestenlehner2022>{{저널 인용|doi=10.1093/mnras/stab3521|title=Melnick 33Na: A very massive colliding-wind binary system in 30 Doradus|year=2022|last1=Bestenlehner|first1=Joachim M.|last2=Crowther|first2=Paul A.|last3=Broos|first3=Patrick S.|last4=Pollock|first4=Andrew M T.|last5=Townsley|first5=Leisa K.|journal=Monthly Notices of the Royal Astronomical Society|volume=510|issue=4|pages=6133–6149|bibcode=2022MNRAS.510.6133B|arxiv=2112.00022}}</ref><ref name=Castro2018>{{저널 인용|doi=10.1051/0004-6361/201732084|title=Mapping the core of the Tarantula Nebula with VLT-MUSE. I. Spectral and nebular content around R136|year=2018|author1=Castro, N.|author2=Crowther, P. A.|author3=Evans, C. J.|author4=Mackey, J.|author5=Castro-Rodriguez, N.|author6=Vink, J. S.|author7=Melnick, J.|author8=Selman, F.|journal=Astronomy & Astrophysics|volume=614|id=A147|pages=12|arxiv=1802.01597|bibcode=2018A&A...614A.147C|s2cid=119341920}}</ref>
|-
| style="background: {{항성-색깔|WC}};" | [[R134]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,413,000
| -10.635
| 164,000
| 12.58
| 47,000
|{{SIMBAD link|RMC134|SIMBAD}}
|<ref name="Hainich2014" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WN}};" |[[황새치자리 S]] ([[대마젤란 은하]]의 [[NGC 1910]]에 존재)
| 1,413,000
| -10.635
| 169,000
|10.25
| 20,000
|{{SIMBAD link|S+Doradus|SIMBAD}}
|<ref name="lamers1995">{{콘퍼런스 인용| last=Lamers | first=H. J. G. L. M. | contribution=Observations and Interpretation of Luminous Blue Variables | title=Proceedings of IAU Colloquium 155, Astrophysical applications of stellar pulsation | journal=Astrophysical Applications of Stellar Pulsation. Astronomical Society of the Pacific Conference Series | volume=83 | pages=176–191 | date=February 6–10, 1995 | location=Cape Town, South Africa | publisher=Astronomical Society of the Pacific | bibcode=1995ASPC...83..176L }}</ref><ref name="zacharias" />
|-
| style="background: {{항성-색깔|WC}};" | [[WR 66]] ([[컴퍼스자리 OB1]]에 존재)
| 1,413,000
| -10.635
| 16,900
| 11.34
| 44,700
|{{SIMBAD link|WR+66|SIMBAD}}
|<ref name="WN" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[HD 269846]] ([[대마젤란 은하]]에 존재)
|1,406,000
| -10.63
|163,000
|11.63
|28,200
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+269846 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|WN}};" |[[HD 37974]] ([[대마젤란 은하]]의 [[N135]]에 존재)
| 1,400,000
| -10.625
| 163,000
| 10.99
| 22,500
|{{SIMBAD link|HD+37974|SIMBAD}}
|<ref name="kastner">{{저널 인용| last1 = Kastner | first1 = J. H. | last2 = Buchanan | first2 = C. L. | last3 = Sargent | first3 = B. | last4 = Forrest | first4 = W. J. | title = SpitzerSpectroscopy of Dusty Disks around B\e] Hypergiants in the Large Magellanic Cloud | doi = 10.1086/500804 | journal = The Astrophysical Journal | volume = 638 | pages = L29–L32 | year = 2006 | issue = 1 |bibcode = 2006ApJ...638L..29K | doi-access = free }}</ref><ref name="zacharias" /><ref group="lower-alpha">N135은 대마젤란 은하의 방출 성운이다.</ref>
|-
|[[W61 3-24]] ([[대마젤란 은하]]에 존재)
|1,393,000
| -10.62
|163,000
|14.03
|43,700
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=w61+3-24 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" | [[VFTS 621]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,380,000
| -10.61
| 164,000
| 15.39
| 54,000
|{{SIMBAD link|VFTS+621|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" | [[WR 131]] ([[백조자리 OB3]]에 존재)
| 1,380,000
| -10.61
| 22,600
| 12.08
| 44,700
|{{SIMBAD link|WR+131|SIMBAD}}
|<ref name="WN" /><ref name=Reed />
|-
| style="background: {{항성-색깔|O}};" |[[Sk -69° 104]] ([[대마젤란 은하]]의 [[NGC 1910]]에 존재)
|1,368,000
| -10.6
|160,000
|12.1
|39,900
|{{SIMBAD link|Sk+-69+104|SIMBAD}}
|<ref name=":42" /><ref name=Bonanos2009 />
|-
| style="background: {{항성-색깔|WN}};" | [[Var A-1]] ([[안드로메다 은하]]에 존재)
| 1,368,000
| -10.6
| 2,500,000
| 17.143
| 21,700
|{{SIMBAD link|RB73+A-1|SIMBAD}}
|<ref name="m31-5">{{저널 인용|last1=Humphreys |first1=Roberta M. |last2=Davidson |first2=Kris |last3=Hahn |first3=David |last4=Martin |first4=John C. |last5=Weis |first5=Kerstin |date=2017-07-01 |title=Luminous and Variable Stars in M31 and M33. V. The Upper HR Diagram |journal=The Astrophysical Journal |volume=844 |issue=1 |pages=40 |doi=10.3847/1538-4357/aa7cef |issn=0004-637X|arxiv=1707.01916 |bibcode=2017ApJ...844...40H |s2cid=119357524 |doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[머서 30]]-6a A ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재하는 WR 46-4 A)
|1,349,000
| -10.585
|40,000
|10.39 (J 대역)
|29,900
|{{SIMBAD link|DNB2016+Mc30-6a|SIMBAD}}
|<ref name=":17" /><ref group=lower-alpha name=Mc30/>
|-
| style="background: {{항성-색깔|WC}};" | [[VFTS 427]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,349,000
| -10.585
| 164,000
| 13.76
|39,800
|{{SIMBAD link|VFTS+427|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[웨스터하우트 51]]-3 ([[웨스터하우트 51]]에 존재)
|1,349,000
| -10.585
|20,000
|16.998 (J 대역)
|39,800
|{{SIMBAD link|2MASS+J19234283%2B1430277|SIMBAD}}
|<ref name=":22" /><ref name=2MASS/>
|-
| style="background: {{항성-색깔|B}};" |[[HD 269722]] ([[대마젤란 은하]]에 존재)
|1,343,000
| -10.58
|163,000
|11.52
|28,200
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+269722 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" |[[CXOGC J174502.8-290859]] ([[은하중심]]에 존재)
|1,318,000
| -10.56
|26,000
|13.93 (J 대역)
|33,000
|{{SIMBAD link|CXOGC+J174502.8-290859|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|O}};" | [[HSH95-49]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,318,000
| -10.56
| 163,000
| 14.75
| 58,000
|{{SIMBAD link|HSH95+49|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" /><ref group="lower-alpha" name="Optical">이 매개변수는 이러한 별에 대한 광학적 적합만을 기반으로 한다.</ref>
|-
|style="background: {{항성-색깔|O}};" |[[HD 269810]] ([[대마젤란 은하]]의[[NGC 2032]]에 존재)
|1,318,000
| -10.56
|163,000
|12.28
|44,700
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+269810 SIMBAD]
|<ref name=":2" />
|-
|[[HD 270145]] ([[대마젤란 은하]]에 존재)
|1,306,000
| -10.55
|163,000
|12.17
|43,700
|
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" |[[웨스터하우트 49]]-15 ([[웨스터하우트 49]]에 존재)
|1,288,000
| -10.535
|36,200
|18.307 (J 대역)
|43,700
|{{SIMBAD link|WBB2016+15|SIMBAD}}
|<ref name="Wu2016" /><ref name=2MASS/>
|-
| style="background: {{항성-색깔|O}};" |[[웨스터하우트 51]]<nowiki/>d ([[웨스터하우트 51]]에 존재)
|1,288,000
| -10.535
|20,000
|15.11 (J 대역)
|42,700
|{{SIMBAD link|2MASS+J19233978%2B1431074|SIMBAD}}
|<ref name=":22" /><ref name=2MASS/>
|-
| style="background: {{항성-색깔|WC}};" |[[WR 18]] ([[용골자리 성운]]의 [[용골자리 OB1]]에 존재)
|1,288,000
| -10.535
|12,450
|10.83
|112,200
|{{SIMBAD link|WR+18|SIMBAD}}
|<ref name="WN" /><ref name="zacharias" />
|-
| style="background: {{항성-색깔|O}};" |[[BMS2003 578|[BMS2003] 578]] B ([[삼각형자리 은하]]의 [[NGC 604]]에 존재)
|1,285,000
| -10.53
|2,700,000
|15.97 (연성계 전체)
|32,000
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=%5BBMS2003%5D+578B&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id SIMBAD]
|<ref name=":0" />
|-
| style="background: {{항성-색깔|WC}};" |[[AB7]] A ([[소마젤란 은하]]의 [[NGC 371]]에 존재)
| 1,259,000
| -10.51
| 197,000
| 13.016 (연성계 전체)
| 105,000
|{{SIMBAD link|SMC+AB+7|SIMBAD}}
|<ref name="shenar" /><ref name=Bonanos2010 />
|-
| style="background: {{항성-색깔|WC}};" |[[아치스 성단|아치스]]-F3 ([[아치스 성단]]에 존재하는 WR 102bb)
| 1,259,000
| -10.51
| 25,000
|16.06 (J 대역)
| 29,600
|{{SIMBAD link|FNG2002+3|SIMBAD}}
|<ref name="martins" /><ref name=Figer/>
|-
| style="background: {{항성-색깔|WC}};" |[[아치스 성단|아치스]]-F8 ([[아치스 성단]]에 존재하는 WR 102ag)
| 1,259,000
| -10.51
| 25,000
|16.31 (J 대역)
| 32,900
|{{SIMBAD link|FNG2002+8|SIMBAD}}
|<ref name="martins" /><ref name=Figer/>
|-
| style="background: {{항성-색깔|WN}};" | [[HD 50064]] ([[NGC 2301]]에 존재)
| 1,259,000
| -10.51
| 9,500
| 8.21
| 13,500
|{{SIMBAD link|HD+50064|SIMBAD}}
|<ref name="aerts">{{저널 인용| date = April 2010 | journal = Astronomy and Astrophysics | volume = 513 | page = L11 | title = Periodic mass-loss episodes due to an oscillation mode with variable amplitude in the hot supergiant HD 50064 | doi = 10.1051/0004-6361/201014124|arxiv = 1003.5551 |bibcode = 2010A&A...513L..11A | last1 = Aerts | first1 = C. | last2 = Lefever | first2 = K. | last3 = Baglin | first3 = A. | last4 = Degroote | first4 = P. | last5 = Oreiro | first5 = R. | last6 = Vučković | first6 = M. | last7 = Smolders | first7 = K. | last8 = Acke | first8 = B. | last9 = Verhoelst | first9 = T. | last10 = Desmet | first10 = M. | last11 = Godart | first11 = M. | last12 = Noels | first12 = A. | last13 = Dupret | first13 = M.-A. | last14 = Auvergne | first14 = M. | last15 = Baudin | first15 = F. | last16 = Catala | first16 = C. | last17 = Michel | first17 = E. | last18 = Samadi | first18 = R. | s2cid = 41541073}}</ref>
|-
| style="background: {{항성-색깔|O}};" |[[HSH95-16]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,259,000
| -10.51
|163,000
|13.65
|42,000
|{{SIMBAD link|HSH95+16|SIMBAD}}
|<ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[HSH95-20]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,259,000
| -10.51
|164,000
|13.71
|46,000
|{{SIMBAD link|HSH95+20|SIMBAD}}
|<ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" | [[HSH95-46]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,259,000
| -10.51
| 163,000
| 14.56
| 47,500
|{{SIMBAD link|HSH95+46|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" | [[R139]] A ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,259,000
| -10.51
| 163,000
| 11.94 (연성계 전체)
|34,000
|{{SIMBAD link|RMC139|SIMBAD}}
|<ref>{{저널 인용| last1 = Taylor | first1 = W. D. | last2 = Evans | first2 = C. J. | last3 = Sana | first3 = H. | last4 = Walborn | first4 = N. R. | last5 = De Mink | first5 = S. E. |author5-link=Selma de Mink| last6 = Stroud | first6 = V. E. | last7 = Alvarez-Candal | first7 = A. | last8 = Barbá | first8 = R. H. | last9 = Bestenlehner | first9 = J. M. | last10 = Bonanos | first10 = A. Z. | last11 = Brott | first11 = I. | last12 = Crowther | first12 = P. A. | last13 = De Koter | first13 = A. | last14 = Friedrich | first14 = K. | last15 = Gräfener | first15 = G. | last16 = Hénault-Brunet | first16 = V. | last17 = Herrero | first17 = A. | last18 = Kaper | first18 = L. | last19 = Langer | first19 = N. | last20 = Lennon | first20 = D. J. | last21 = Maíz Apellániz | first21 = J. | last22 = Markova | first22 = N. | last23 = Morrell | first23 = N. | last24 = Monaco | first24 = L. | last25 = Vink | first25 = J. S. | title = The VLT-FLAMES Tarantula Survey II: R139 revealed as a massive binary system | doi = 10.1051/0004-6361/201116785 | journal = Astronomy & Astrophysics | volume = 530 | pages = L10 | year = 2011 |arxiv = 1103.5387 |bibcode = 2011A&A...530L..10T | s2cid = 119214376 }}</ref><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" | [[VFTS 259]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,259,000
| -10.51
| 164,000
| 13.65
|37,700
|{{SIMBAD link|VFTS+259|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 1031]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,259,000
| -10.51
|164,000
|13.89
|48,000
|{{SIMBAD link|VFTS+1031|SIMBAD}}
|<ref name="Doran2013" />
|-
|[[NGC 2070 MH 980]] ([[대마젤란 은하]]의 [[NGC 2070]]에 존재)
|1,259,000
| -10.51
|163,000
|13.68
|42,700
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=cl*+ngc+2070+mh+980 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|WC}};" |[[Sk -69° 194]] ([[대마젤란 은하]]의 [[NGC 2033]]에 존재)
|1,247,000
| -10.5
|160,000
|12.131 (연성계 전체)
|45,000
|{{SIMBAD link|Sk+-69+194|SIMBAD}}
|<ref name=":42" /><ref name=Ulaczyk>{{저널 인용|last1=Ulaczyk|first1=K.|last2=Szymański|first2=M. K.|last3=Udalski|first3=A.|last4=Kubiak|first4=M.|last5=Pietrzyński|first5=G.|last6=Soszyński|first6=I.|last7=Wyrzykowski|first7=Ł.|last8=Poleski|first8=R.|last9=Gieren|first9=W.|last10=Walker|first10=A. R.|last11=Garcia-Varela|first11=A.|date=1 June 2013|title=Variable Stars from the OGLE-III Shallow Survey in the Large Magellanic Cloud|journal=Acta Astronomica|volume=63|issue=2|pages=159–179|arxiv=1306.4802|bibcode=2013AcA....63..159U|issn=0001-5237|s2cid=119228254}}</ref>
|-
| style="background: {{항성-색깔|O}};" |[[ST2-22]] ([[대마젤란 은하]] [[NGC 2044]]에 존재)
|1,247,000
| -10.5
|160,000
|14.3
|51,300
|{{SIMBAD link|ST92+2-22|SIMBAD}}
|<ref name=":42" /><ref name=Schild/>
|-
|[[HD 269215]] ([[대마젤란 은하]]에 존재)
|1,247,000
| -10.5
|163,000
|11.94
|36,300
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+269215 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" |[[트럼플러 27]]-27 ([[트럼플러 27]]에 존재)
| 1,247,000
| -10.5
| 8,200
|13.31
|37,000
|{{SIMBAD link|Cl+Trumpler+27+27|SIMBAD}}
|<ref name="Massey et al. 2001" /><ref name="zacharias" />
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 1028]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,230,000
| -10.485
|164,000
|13.84
|47,300
|{{SIMBAD link|VFTS+1028|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[LH 10]]-3601 ([[대마젤란 은하]]의 [[NGC 1763]]에 존재)
|1,202,000
| -10.46
|160,000
|13.491
|55,000
|{{SIMBAD link|L72+LH+10-3061|SIMBAD}}
|<ref name=Walborn/><ref name=Bonanos2009 />
|-
| style="background: {{항성-색깔|WC}};" |[[AB1 (항성)|AB1]] ([[소마젤란 은하]]의 [[DEM S10]]에 존재)
|1,175,000
| -10.435
|197,000
|15.238
|79,000
|{{SIMBAD link|SMC+AB+1|SIMBAD}}
|<ref name=Hainich2015>{{저널 인용|last1=Hainich|first1=R.|last2=Pasemann|first2=D.|last3=Todt|first3=H.|last4=Shenar|first4=T.|last5=Sander|first5=A.|last6=Hamann|first6=W. -R|date=2015|title=Wolf-Rayet stars in the Small Magellanic Cloud. I. Analysis of the single WN stars|journal=Astronomy & Astrophysics|volume=581|issue=21|page=30|arxiv=1507.04000|bibcode=2015A&A...581A..21H|doi=10.1051/0004-6361/201526241|s2cid=56230998}}</ref><ref name=Bonanos2010 /><ref group="lower-alpha">DEM S10은 소마젤란 은하의 H II 영역이다.</ref>
|-
| style="background: {{항성-색깔|O}};" |[[BI 253]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재하는 [[폭주성]])
|1,175,000
| -10.435
|164,000
|13.76
|54,000
|{{SIMBAD link|BI+253|SIMBAD}}
|<ref name="schneider2018" /><ref>{{저널 인용|last1=Rivero González|first1=J. G.|last2=Puls|first2=J.|last3=Najarro|first3=F.|last4=Brott|first4=I.|date=2012|title=Nitrogen line spectroscopy of O-stars. II. Surface nitrogen abundances for O-stars in the Large Magellanic Cloud|journal=Astronomy & Astrophysics|volume=537|page=A79|arxiv=1110.5148|bibcode=2012A&A...537A..79R|doi=10.1051/0004-6361/201117790|s2cid=119110554|issn=0004-6361}}</ref>
|-
| style="background: {{항성-색깔|O}};" | [[LGGS J013248.26+303950.4]] ([[삼각형자리 은하]]에 존재)
| 1,175,000
| -10.435
|3,000,000
|17.25
|23,000
|{{SIMBAD link|LGGS+J013248.26%2B303950.4|SIMBAD}}
|<ref name=Kourniotis/><ref>{{저널 인용|last1=Thompson|first1=Todd A.|last2=Prieto|first2=José L.|last3=Stanek|first3=K. Z.|last4=Kistler|first4=Matthew D.|last5=Beacom|first5=John F.|last6=Kochanek|first6=Christopher S.|title=A New Class of Luminous Transients and a First Census of Their Massive Stellar Progenitors|date=2009-11-10|journal=The Astrophysical Journal|volume=705|issue=2|pages=1364–1384|arxiv=0809.0510|bibcode=2009ApJ...705.1364T|doi=10.1088/0004-637X/705/2/1364|hdl=1811/48176|s2cid=17581579|issn=0004-637X}}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[머서 30]]-8 ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재하는 WR 46–6)
|1,175,000
| -10.435
|40,000
|11.658 (J 대역)
|38,100
|{{SIMBAD link|DNB2016+Mc30-8|SIMBAD}}
|<ref name=":17" /><ref group=lower-alpha name=Mc30/>
|-
| style="background: {{항성-색깔|O}};" |[[NGC 346]]-W3 ([[소마젤란 은하]]의 [[NGC 346]]에 존재)
|1,175,000
| -10.435
|200,000
|12.8
|52,500
|{{SIMBAD link|Cl*+NGC+346+W+3|SIMBAD}}
|<ref name=Walborn/><ref name=Bonanos2010 />
|-
| style="background: {{항성-색깔|WC}};" |[[다섯쌍둥이 성단|WR 102d]] ([[다섯쌍둥이 성단]]에 존재)
| 1,175,000
| -10.435
| 26,000
| 15.18 (J 대역)
| 35,100
|{{SIMBAD link|WR+102d|SIMBAD}}
|<ref name="quintuplet" /><ref name="qc" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 126]] ([[여우자리 OB2]]에 존재)
|1,175,000
| -10.435
|24,680
|13.29
|63,000
|{{SIMBAD link|WR+126|SIMBAD}}
|<ref name="sander2019">{{저널 인용|doi=10.1051/0004-6361/201833712|bibcode=2019A&A...621A..92S|arxiv=1807.04293|title=The Galactic WC and WO stars|journal=Astronomy & Astrophysics|volume=621|page=A92|year=2019|last1=Sander|first1=A. A. C.|last2=Hamann|first2=W.-R.|last3=Todt|first3=H.|last4=Hainich|first4=R.|last5=Shenar|first5=T.|last6=Ramachandran|first6=V.|last7=Oskinova|first7=L. M.|s2cid=67754788}}</ref><ref name="zacharias" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 20a]] A ([[웨스터룬드 2]]에 존재)
|1,150,000
| -10.412
|20,000
|13.28 (연성계  전체)
|43,000
|{{SIMBAD link|WR+20a|SIMBAD}}
|<ref name="Rauw2005">{{저널 인용|author=Rauw |display-authors=etal |title=The spectrum of the very massive binary system WR 20a (WN6ha + WN6ha): Fundamental parameters and wind interactions |journal=Astronomy & Astrophysics |volume=432 |issue=3 |pages=985–998 |date=4 March 2005 |doi=10.1051/0004-6361:20042136 |bibcode=2005A&A...432..985R |doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[WR 20a]] B ([[웨스터룬드 2]]에 존재)
|1,150,000
| -10.412
|20,000
|13.28 (연성계 전체)
|43,000
|{{SIMBAD link|WR+20a|SIMBAD}}
|<ref name="Rauw2005" />
|-
| style="background: {{항성-색깔|WC}};" |[[GCIRS 16SW]] A ([[은하중심]]에 존재하는 WR 101k A)
|1,149,000
| -10.411
|26,000
|15.5 (J 대역)
|24,400
|{{SIMBAD link|GCIRS+16SW|SIMBAD}}
|<ref name=Peeples>{{저널 인용|last1=Peeples|first1=Molly S.|last2=Bonanos|first2=A. Z.|last3=DePoy|first3=D. L.|last4=Stanek|first4=K. Z.|last5=Pepper|first5=J.|last6=Pogge|first6=Richard W.|last7=Pinsonneault|first7=M. H.|last8=Sellgren|first8=K.|date=2007-01-01|title=The Nature of the Variable Galactic Center Source GCIRS 16SW Revisited: A Massive Eclipsing Binary|journal=The Astrophysical Journal|volume=654|issue=1|pages=L61–L64|arxiv=astro-ph/0610212|bibcode=2007ApJ...654L..61P|doi=10.1086/510720|s2cid=14242573|issn=0004-637X}}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[GCIRS 16SW]] B ([[은하중심]]에 존재하는 WR 101k B)
|1,149,000
| -10.411
|26,000
|15.5 (J 대역)
|23,500
|{{SIMBAD link|GCIRS+16SW|SIMBAD}}
|<ref name=Peeples />
|-
| style="background: {{항성-색깔|WC}};" | [[BAT99-104]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,148,000
| -10.41
| 165,000
| 14.52
| 63,000
|{{SIMBAD link|BAT99+104|SIMBAD}}
|<ref name="Hainich2014" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[CXOGC J174516.7-285824]] ([[은하중심]]에 존재하는 WR 101–3)
|1,148,000
| -10.41
|26,000
|16.67 (J 대역)
|35,000
|{{SIMBAD link|CXOGC+J174516.7-285824|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|WC}};" | [[G0.121-0.099]] ([[은하중심]]에 존재하는 WR 102–16)
| 1,148,000
| -10.41
| 26,000
|14.972 (J 대역)
|40,000
|{{SIMBAD link|MCD2010+G0.121-0.099|SIMBAD}}
|<ref name="mcd2010" />
|-
| style="background: {{항성-색깔|B}};" |[[G359.797+0.037]] ([[은하중심]]에 존재)
|1,148,000
| -10.41
|26,000
|16.1 (J 대역)
|30,000
|{{SIMBAD link|MCD2010+G329.797%2B0.037|SIMBAD}}
|<ref name="mcd2010" />
|-
| style="background: {{항성-색깔|O}};" |[[HD 93205]] A ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
|1,148,000
| -10.41
|7,500
|7.75 (연성계 전체)
|51,300
|{{SIMBAD link|HD+93205|SIMBAD}}
|<ref name="morrell">{{저널 인용|bibcode=2001MNRAS.326...85M|arxiv=astro-ph/0105014|title=Optical spectroscopy of X-Mega targets - II. The massive double-lined O-type binary HD 93205|journal=Monthly Notices of the Royal Astronomical Society|volume=326|pages=85–94|last1=Morrell|first1=N. I. |author-link1=Nidia Morrell |last2=Barbá|first2=R. H.|last3=Niemela|first3=V. S.|last4=Corti|first4=M. A.|last5=Albacete Colombo|first5=J. F.|last6=Rauw|first6=G.|last7=Corcoran|first7=M.|last8=Morel|first8=T.|last9=Bertrand|first9=J.-F.|last10=Moffat|first10=A. F. J.|last11=St-Louis|first11=N.|year=2001|issue=1|doi=10.1046/j.1365-8711.2001.04500.x|s2cid=16221731}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" | [[HSH95-47]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,148,000
| -10.41
| 163,000
| 14.72
| 46,500
|{{SIMBAD link|HSH95+47|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" /><ref group="lower-alpha" name="Optical" />
|-
| style="background: {{항성-색깔|WC}};" | [[WR 158]] ([[카시오페아자리 OB1]]에 존재)
| 1,148,000
| -10.41
| 16,300
| 11.282
| 44,700
|{{SIMBAD link|WR+158|SIMBAD}}
|<ref name="WN" /><ref name=Laur />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 28]] ([[FSR 1555]]에 존재)
|1,148,000
| -10.41
|18,700
|12.98
|50,100
|{{SIMBAD link|WR+28|SIMBAD}}
|<ref name="WN" /><ref name="zacharias" /><ref group="lower-alpha">FSR 1555은 성단이다.</ref>
|-
| style="background: {{항성-색깔|O}};" |[[트럼플러 16|HD 303308]] ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
|1,138,000
| -10.4
|7,500
|8.17
|51,300
|{{SIMBAD link|HD+303308|SIMBAD}}
|<ref name="Massey et al. 2001" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|WC}};" | [[M33C-15235]] ([[삼각형자리 은하]]에 존재)
| 1,138,000
| -10.4
| 3,000,000
|17.73
| 29,200
|{{SIMBAD link|LGGS+J013351.46%2B304057.0|SIMBAD}}
|<ref name="humphreys2017" /><ref name=Neugent>{{저널 인용|last1=Neugent|first1=Kathryn F.|last2=Massey|first2=Philip|title=The Wolf-Rayet Content of M33|date=2011-06-01|journal=The Astrophysical Journal|volume=733|issue=2|page=123|arxiv=1103.5549|bibcode=2011ApJ...733..123N|doi=10.1088/0004-637X/733/2/123|s2cid=118507918|issn=0004-637X}}</ref>
|-
| style="background: {{항성-색깔|WN}};" | [[ZH 364]] ([[머서 81]]에 존재)
| 1,138,000
| -10.4
| 11,842,000
| 19.59
| 15,860
|{{SIMBAD link|%5BZH91%5D%20M%2081%20364|SIMBAD}}
|<ref name="humphreys2019"/>
|-
| style="background: {{항성-색깔|WN}};" |[[HD 269700]] ([[대마젤란 은하]]에 존재)
|1,127,000
| -10.39
|163,000
|10.54
|19,500
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+269700 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|WC}};" |[[AB9 (항성)|AB9]] ([[소마젤란 은하]] [[DEM S80]]에 존재)
|1,122,000
| -10.385
|197,000
|15.431
|100,000
|{{SIMBAD link|SMC+AB+9|SIMBAD}}
|<ref name=Hainich2015/><ref name=Bonanos2010 /><ref group="lower-alpha">DEM S80은 소마젤란 은하의 H II 영역이다.</ref>
|-
| style="background: {{항성-색깔|O}};" |[[아치스 성단|아치스]]-F18 ([[아치스 성단]]에 존재)
| 1,122,000
| -10.385
| 25,000
|16.7 (J 대역)
|36,900
|{{SIMBAD link|FNG2002+18|SIMBAD}}
|<ref name="martins" /><ref name=Figer/>
|-
| style="background: {{항성-색깔|WC}};" |[[BAT99-64]] A ([[대마젤란 은하]]의 [[NGC 2033]]에 존재)
|1,122,000
| -10.385
|165,000
|14.073 (연성계 전체)
|71,000
|{{SIMBAD link|BAT99+64|SIMBAD}}
|<ref name="Hainich2014" /><ref name=Bonanos2009 />
|-
| style="background: {{항성-색깔|WN}};" |[[M33 Var B|Var B]] ([[삼각형자리 은하]]에 존재)
| 1,122,000
| -10.385
| 3,000,000
| 16.208
|9,000
|{{SIMBAD link|VHK+B|SIMBAD}}
|<ref name="Szeifert et al. 1996" /><ref name=Massey2006/>
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 562]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,122,000
| -10.385
|164,000
|13.66
|42,200
|{{SIMBAD link|VFTS+562|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 37]] ([[G291.27-0.71]]의 [[SFC 27]]에 존재)
|1,122,000
| -10.385
|21,900
|16
|100,000
|{{SIMBAD link|WR+37|SIMBAD}}
|<ref name="WN" /><ref name="zacharias" /><ref group="lower-alpha">SFC 27은 분자운 G291.27-0.71의 일부다.</ref>
|-
| style="background: {{항성-색깔|B}};" |[[SK -69 98]] ([[대마젤란 은하]]에 존재)
|1,096,000
| -10.36
|163,000
|12.29
|28,200
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=sk+-69+98 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 512]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,096,000
| -10.36
|164,000
|14.28
|47,700
|{{SIMBAD link|VFTS+512|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[머서 30]]-6b ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재)
|1,072,000
| -10.335
|40,000
|14.25 (J 대역)
|30,500
|{{SIMBAD link|DNB2016+Mc30-6b|SIMBAD}}
|<ref name=":17" /><ref group=lower-alpha name=Mc30/>
|-
| style="background: {{항성-색깔|B}};" |[[VFTS 3]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,072,000
| -10.335
|164,000
|11.56
|21,000
|{{SIMBAD link|VFTS+3|SIMBAD}}
|<ref name="schneider2018" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 151]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,072,000
| -10.335
|164,000
|14.13
|42,200
|{{SIMBAD link|VFTS+151|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 603]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,060,000
| -10.323
|164,000
|13.99
|43,400
|{{SIMBAD link|VFTS+603|SIMBAD}}
|<ref>{{저널 인용|last1=Walborn|first1=N. R.|last2=Sana|first2=H.|last3=Simón-Díaz|first3=S.|last4=Maíz Apellániz|first4=J.|last5=Taylor|first5=W. D.|last6=Evans|first6=C. J.|last7=Markova|first7=N.|last8=Lennon|first8=D. J.|last9=de Koter|first9=A.|date=2014|title=The VLT-FLAMES Tarantula Survey. XIV. The O-type stellar content of 30 Doradus|journal=Astronomy & Astrophysics|volume=564|issue=40|page=35|arxiv=1402.6969|bibcode=2014A&A...564A..40W|doi=10.1051/0004-6361/201323082|s2cid=119302111}}</ref><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|B}};" |[[HD 268605]] ([[대마젤란 은하]]에 존재)
|1.057,000
| -10.32
|163,000
|11.34
|28,200
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+268605 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" |[[CXOGC J174532.7-285126]] ([[은하중심]]에 존재)
|1,047,000
| -10.31
|26,000
|10.72 (J 대역)
|40,000
|{{SIMBAD link|CXOGC+J174532.7-285126|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|O}};" |[[HD 93403]] A ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
| 1,047,000
| -10.31
| 10,000
| 8.27 (연성계 전체)
| 39,300
|{{SIMBAD link|HD+93403|SIMBAD}}
|<ref name="rauw">{{저널 인용|bibcode=2002A&A...388..552R|title=Phase-resolved X-ray and optical spectroscopy of the massive binary HD 93403|journal=Astronomy and Astrophysics|volume=388|issue=2|page=552|last1=Rauw|first1=G.|last2=Vreux|first2=J.-M.|last3=Stevens|first3=I. R.|last4=Gosset|first4=E.|last5=Sana|first5=H.|last6=Jamar|first6=C.|last7=Mason|first7=K. O.|year=2002|doi=10.1051/0004-6361:20020523|doi-access=free}}</ref><ref name="zacharias" />
|-
| style="background: {{항성-색깔|O}};" |[[머서 30]]-2 ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재)
|1,047,000
| -10.31
|40,000
|12.63 (J 대역)
|21,200
|{{SIMBAD link|DNB2016+Mc30-2|SIMBAD}}
|<ref name=":17" /><ref group=lower-alpha name=Mc30/>
|-
| style="background: {{항성-색깔|O}};" |[[R133]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,047,000
| -10.31
|163,000
|12.49
|37,600
|{{SIMBAD link|RMC133|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|B}};" |[[HD 269786]] ([[대마젤란 은하]]에 존재)
|1,047,000
| -10.31
|163,000
|11.18
|24,000
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+269786 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" |[[HD 97950]] E ([[NGC 3603]]의 [[HD 97950]]에 존재)
|1,038,000
| -10.3
|24,000
|13.081
|46,500
|{{SIMBAD link|HD+97950E|SIMBAD}}
|<ref name="melena2008" /><ref name=":16" />
|-
| style="background: {{항성-색깔|B}};" |[[버클리 87|HD 229059]] ([[버클리 87]]에 존재)
| 1,038,000
| -10.3
| 3,200
| 8.7
| 26,300
|{{SIMBAD link|HD+229059|SIMBAD}}
|<ref name="Massey et al. 2001" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|WC}};" | [[M33C-10788]] ([[삼각형자리 은하]]에 존재)
| 1,038,000
| -10.3
| 3,000,000
|17.95
| 32,000
|{{SIMBAD link|LGGS+J013416.07%2B303642.1|SIMBAD}}
|<ref name="humphreys2017" /><ref name=Neugent />
|-
| style="background: {{항성-색깔|B}};" |[[Sk -69° 200]] ([[대마젤란 은하]]의 [[NGC 2033]]에 존재)
|1,038,000
| -10.3
|160,000
|11.18
|26,300
|{{SIMBAD link|Sk+-69+200|SIMBAD}}
|<ref name=":42" /><ref name="zacharias" />
|-
| style="background: {{항성-색깔|B}};" |[[Sk -69° 259]] ([[대마젤란 은하]]의 [[NGC 2081]]에 존재)
|1,038,000
| -10.3
|160,000
|11.93
|30,000
|{{SIMBAD link|Sk+-69+259|SIMBAD}}
|<ref name=":42" /><ref name="zacharias" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 77k]] ([[웨스터룬드 1]]에 존재)
|1,038,000
| -10.3
|11,000
|18.86
|35,000
|{{SIMBAD link|WR+77k|SIMBAD}}
|<ref>{{저널 인용|last1=Crowther|first1=P. A.|last2=Hadfield|first2=L. J.|last3=Clark|first3=J. S.|last4=Negueruela|first4=I.|last5=Vacca|first5=W. D.|date=2006-11-01|title=A census of the Wolf-Rayet content in Westerlund 1 from near-infrared imaging and spectroscopy|journal=Monthly Notices of the Royal Astronomical Society|volume=372|issue=3|pages=1407–1424|arxiv=astro-ph/0608356|bibcode=2006MNRAS.372.1407C|doi=10.1111/j.1365-2966.2006.10952.x|s2cid=10505573|issn=0035-8711}}</ref><ref>{{저널 인용|last1=Clark|first1=J. S.|last2=Muno|first2=M. P.|last3=Negueruela|first3=I.|last4=Dougherty|first4=S. M.|last5=Crowther|first5=P. A.|last6=Goodwin|first6=S. P.|last7=de Grijs|first7=R.|date=2008|title=Unveiling the X-ray point source population of the Young Massive Cluster Westerlund 1|journal=Astronomy & Astrophysics|volume=477|issue=1|pages=147–163|bibcode=2008A&A...477..147C|doi=10.1051/0004-6361:20077186|issn=0004-6361|doi-access=free}}</ref>
|-
| style="background: {{항성-색깔|A}};" | [[10182-pr-6]] ([[NGC 2403]]에 존재)
| 1,038,000
| -10.3
| 10,314,000
| 18.79
| 8,000
|{{SIMBAD link|%5BHSG2019%5D%2010182-pr-6|SIMBAD}}
|<ref name="humphreys2019"/>
|-
| style="background: {{항성-색깔|B}};" |[[RP2006 542|[RP2006] 542]] ([[대마젤란 은하]]에 존재)
|1,028,000
| -10.29
|163,000
|16.75
|29,500
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=%5Brp2006%5D+542 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|O}};" |[[HD 93250]] A ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
| 1,023,000
| -10.285
| 7,500
| 7.5 (연성계 전체)
| 46,000
|{{SIMBAD link|HD+93250|SIMBAD}}
|<ref name="repolust">{{저널 인용|bibcode=2004A&A...415..349R|title=Stellar and wind parameters of Galactic O-stars. The influence of line-blocking/blanketing|journal=Astronomy and Astrophysics|volume=415|page=349|last1=Repolust|first1=T.|last2=Puls|first2=J.|last3=Herrero|first3=A.|year=2004|doi=10.1051/0004-6361:20034594|doi-access=free}}</ref><ref name="ducati" /><ref group="lower-alpha" name="Binary" />
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 267]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,023,000
| -10.285
|164,000
|13.49
|44,700
|{{SIMBAD link|VFTS+267|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 599]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,023,000
| -10.285
|164,000
|13.8
|47,300
|{{SIMBAD link|VFTS+599|SIMBAD}}
|<ref name="schneider2018" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[VVV CL074]]-9 ([[VVV CL074]]에 존재하는 WR 75–29)
|1,023,000
| -10.285
|20,000
|15.22 (J 대역)
|37,000
|{{SIMBAD link|CBB2013+VVV+CL074+9|SIMBAD}}
|<ref name=Martins2019 /><ref group="lower-alpha" name="VVV" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 156]] ([[세페우스 OB1]]에 존재)
|1,023,000
| -10.285
|13,400
|11.01
|39,800
|{{SIMBAD link|WR+156|SIMBAD}}
|<ref name="WN" /><ref name="tycho2" />
|-
| style="background: {{항성-색깔|WN}};" |[[HD 269050]] ([[대마젤란 은하]]에 존재)
|1,019,000
| -10.28
|163,000
|11.54
|28,200
|[http://simbad.cds.unistra.fr/simbad/sim-id?Ident=hd+269050 SIMBAD]
|<ref name=":2" />
|-
| style="background: {{항성-색깔|WC}};" |[[아치스 성단|아치스]]-F2 ([[아치스 성단]]에 존재하는 WR 102aa)
| 1,000,000
| -10.26
| 25,000
|17.84 (J 대역)
| 33,500
|{{SIMBAD link|FNG2002+2|SIMBAD}}
|<ref name="martins" /><ref name=Figer/>
|-
| style="background: {{항성-색깔|WC}};" |[[아치스 성단|아치스]]-F14 ([[아치스 성단]]에 존재하는 WR 102ba)
| 1,000,000
| -10.26
| 25,000
|16.38 (J 대역)
| 34,500
|{{SIMBAD link|FNG2002+14|SIMBAD}}
|<ref name="martins" /><ref name=Figer/>
|-
| style="background: {{항성-색깔|WC}};" | [[BAT99-68]] ([[대마젤란 은하]]의 [[BSDL 2505]]에 존재)
| 1,000,000
| -10.26
| 163,000
| 14.13
| 45,000
|{{SIMBAD link|BAT99+68|SIMBAD}}
|<ref name="Hainich2014" /><ref>{{저널 인용|last1=Neugent|first1=Kathryn F.|last2=Massey|first2=Philip|last3=Morrell|first3=Nidia|title=The Discovery of a Rare Wo-Type Wolf–Rayet Star in the Large Magellanic Cloud|date=2012-12-01|journal=The Astronomical Journal|volume=144|issue=6|page=162|arxiv=1210.0062|bibcode=2012AJ....144..162N|doi=10.1088/0004-6256/144/6/162|s2cid=118628394|issn=0004-6256}}</ref><ref group="lower-alpha">BSDL 2505은 대마젤란 은하의 성단이다.</ref>
|-
| style="background: {{항성-색깔|O}};" |[[CXOGC J174628.2-283920]] ([[은하중심]]에 존재)
|1,000,000
| -10.26
|26,000
|16.99 (J 대역)
|40,000
|{{SIMBAD link|CXOGC+J174628.2-283920|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|O}};" |[[CXOGC J174703.1-283119]] ([[은하중심]]에 존재)
|1,000,000
| -10.26
|26,000
|16.23 (J 대역)
|40,000
|{{SIMBAD link|CXOGC+J174703.1-283119|SIMBAD}}
|<ref name=":21" />
|-
| style="background: {{항성-색깔|O}};" |[[HSH95-28]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,000,000
| -10.26
|163,000
|14.09
|48,000
|{{SIMBAD link|HSH95+28|SIMBAD}}
|<ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" | [[HSH95-31]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
| 1,000,000
| -10.26
| 163,000
| 14.12
| 48,000
|{{SIMBAD link|HSH95+31|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" /><ref group="lower-alpha" name="Optical" />
|-
| style="background: {{항성-색깔|O}};" |[[HSH95-57]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,000,000
| -10.26
|163,000
|14.8
|47,000
|{{SIMBAD link|HSH95+57|SIMBAD}}
|<ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[R135]] A ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,000,000
| -10.26
|163,000
|13.48 (연성계 전체)
|50,000
|{{SIMBAD link|RMC135|SIMBAD}}
|<ref name="Hainich2014" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[R140a2]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,000,000
| -10.26
|163,000
|12.12 (연성계 전체)
|34,000
|{{SIMBAD link|RMC140a2|SIMBAD}}
|<ref name="Doran2013" />
|-
| style="background: {{항성-색깔|B}};" |[[R142 (star)|R142]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,000,000
| -10.26
|163,000
|11.82 (연성계 전체)
|21,000
|{{SIMBAD link|RMC142|SIMBAD}}
|<ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 64]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,000,000
| -10.26
|164,000
|14.62
|39,800
|{{SIMBAD link|VFTS+64|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|-
| style="background: {{항성-색깔|B}};" |[[VFTS 591]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,000,000
| -10.26
|164,000
|12.55
|27,000
|{{SIMBAD link|VFTS+591|SIMBAD}}
|<ref name="Doran2013" />
|-
| style="background: {{항성-색깔|O}};" |[[VFTS 1034]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|1,000,000
| -10.26
|164,000
|13.36
|34,000
|{{SIMBAD link|VFTS+1034|SIMBAD}}
|<ref name="Doran2013" />
|-
| style="background: {{항성-색깔|WC}};" |[[VVV CL074]]-3 ([[VVV CL074]]에 존재하는 WR 75–28)
|1,000,000
| -10.26
|20,000
|14.72 (J 대역)
|31,500
|{{SIMBAD link|CBB2013+VVV+CL074+3|SIMBAD}}
|<ref name=Martins2019 /><ref group="lower-alpha" name="VVV" />
|-
| colspan="6" style="text-align:center;"| '''다음의 유명한 별들은 비교를 위해 쓰여있다.'''
|-
| style="background: {{항성-색깔|B}};" |[[전갈자리 제타1]] ([[전갈자리 OB1]]의 [[NGC 6231]]에 존재)
| 851,000
| -10.085
| 8,210
| style="background: lightblue;" | 4.705
| 17,200
|{{SIMBAD link|Zeta1+Scorpii|SIMBAD}}
|<ref name=":14">{{저널 인용|last1=Clark|first1=J. S.|last2=Najarro|first2=F.|last3=Negueruela|first3=I.|last4=Ritchie|first4=B. W.|last5=Urbaneja|first5=M. A.|last6=Howarth|first6=I. D.|date=2012|title=On the nature of the galactic early-B hypergiants|journal=Astronomy & Astrophysics|volume=541|page=A145|arxiv=1202.3991|bibcode=2012A&A...541A.145C|doi=10.1051/0004-6361/201117472|s2cid=11978733|issn=0004-6361}}</ref><ref name="aass61_387">{{인용| last1=Kozok | first1=J. R. | title=Photometric observations of emission B-stars in the southern Milky Way | journal=Astronomy and Astrophysics Supplement Series | volume=61 | pages=387–405 |date=September 1985 | bibcode=1985A&AS...61..387K }}</ref>
|-
| style="background: {{항성-색깔|O}};" |[[나오스]] ([[돛자리 분자 능선]]의 [[돛자리 R2]]에 존재)
| 813,000
| -10.035
| 1,080
| style="background: lightblue;" | 2.25
| 40,000
|{{SIMBAD link|Zeta+Puppis|SIMBAD}}
|<ref name="bouret2">{{저널 인용|last1=Bouret|first1=J. -C.|last2=Hillier|first2=D. J.|last3=Lanz|first3=T.|last4=Fullerton|first4=A. W.|year=2012|title=Properties of Galactic early-type O-supergiants: A combined FUV-UV and optical analysis|journal=Astronomy & Astrophysics|volume=544|page=A67|arxiv=1205.3075|bibcode=2012A&A...544A..67B|doi=10.1051/0004-6361/201118594|s2cid=119280104}}</ref><ref name="ducati" /><ref group="lower-alpha">돛자리 R2는 돛자리 분자 능선의 OB 성협이다.</ref>
|-
| style="background: {{항성-색깔|O}};" |[[기린자리 알파]] ([[NGC 1502]]에 존재하는 [[폭주성]])
|676,000
| -9.835
|6,000
| style="background: lightblue;" |4.29
|29,000
|{{SIMBAD link|Alpha+Camelopardalis|SIMBAD}}
|<ref name="repolust" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|WC}};" |[[WR 78]] ([[전갈자리 OB1 성협|전갈자리 OB1]]의 [[NGC 6231]]에 존재)
|631,000
| -9.76
|4,100
| style="background: lightblue;" | 6.48
|50,100
|{{SIMBAD link|WR+78|SIMBAD}}
|<ref name="WN" /><ref name="gcvs" />
|-
| style="background: {{항성-색깔|O}};" |[[세페우스자리 람다]] ([[세페우스자리 OB3]]에 존재하는 [[폭주성]])
|631,000
| -9.76
|3,100
| style="background: lightblue;" |5.05
|36,000
|{{SIMBAD link|Lambda+Cephei|SIMBAD}}
|<ref name="bouret2" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|WN}};" |[[백조자리 P]] ([[백조자리 OB1]]의 [[IC 4996]]에 존재)
| 610,000
| -9.723
| 5,100
| style="background: lightblue;" | 4.82
| 18,700
|{{SIMBAD link|P+Cygni|SIMBAD}}
|<ref name=rivet>{{저널 인용|bibcode=2020MNRAS.494..218R|arxiv=1910.08366|doi=10.1093/mnras/staa588|title=Intensity interferometry of P Cygni in the H α emission line: Towards distance calibration of LBV supergiant stars|year=2020|last1=Rivet|first1=J-P|last2=Siciak|first2=A.|last3=de Almeida|first3=E. S. G.|last4=Vakili|first4=F.|last5=Domiciano de Souza|first5=A.|last6=Fouché|first6=M.|last7=Lai|first7=O.|last8=Vernet|first8=D.|last9=Kaiser|first9=R.|last10=Guerin|first10=W.|journal=Monthly Notices of the Royal Astronomical Society|volume=494|issue=1|pages=218–227|s2cid=204788654}}</ref><ref name="ducati" /><ref group="lower-alpha">IC 4996은 백조자리 OB1의 산개성단이다.</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[WR 79a]] ([[전갈자리 OB1 성협|전갈자리 OB1]]의 [[NGC 6231]]에 존재)
|603,000
| -9.71
|5,600
| style="background: lightblue;" |5.77
|35,000
|{{SIMBAD link|WR+79a|SIMBAD}}
|<ref>{{저널 인용|last1=Skinner|first1=Stephen L.|last2=Zhekov|first2=Svetozar A.|last3=Güdel|first3=Manuel|last4=Schmutz|first4=Werner|last5=Sokal|first5=Kimberly R.|title=New X-Ray Detections of WNL Stars|date=2012-05-01|journal=The Astronomical Journal|volume=143|issue=5|page=116|arxiv=1203.5098|bibcode=2012AJ....143..116S|doi=10.1088/0004-6256/143/5/116|s2cid=119281411|issn=0004-6256}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[알닐람]] ([[오리온자리 분자운 복합체|오리온 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
| 537,000
| -9.585
| 2,000
| style="background: lightblue;" | 1.69
| 27,500
|{{SIMBAD link|Epsilon+Orionis|SIMBAD}}
|<ref name="Searle 20082">{{저널 인용|author=Searle, S. C.|author2=Prinja, R. K.|author3=Massa, D.|author4=Ryans, R.|date=2008|title=Quantitative studies of the optical and UV spectra of Galactic early B supergiants. I. Fundamental parameters|journal=Astronomy and Astrophysics|volume=481|issue=3|pages=777–97|arxiv=0801.4289|bibcode=2008A&A...481..777S|doi=10.1051/0004-6361:20077125|s2cid=1552752}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[용골자리 에타]] B ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
|400,000
| -9.265
|7,500
| style="background: lightblue;" |4.3 (연성계 전체)
|37,200
|{{SIMBAD link|Eta+Carinae|SIMBAD}}
|<ref name="mehner">{{저널 인용|bibcode=2010ApJ...710..729M|title=High-excitation Emission Lines near Eta Carinae, and Its Likely Companion Star|journal=The Astrophysical Journal|volume=710|issue=1|pages=729–742|last1=Mehner|first1=Andrea|last2=Davidson|first2=Kris|last3=Ferland|first3=Gary J.|last4=Humphreys|first4=Roberta M.|author-link4=Roberta M. Humphreys|year=2010|doi=10.1088/0004-637X/710/1/729|arxiv = 0912.1067 |s2cid=5032987}}</ref><ref name="2018-07-02_NAL"/>
|-
| style="background: {{항성-색깔|O}};" |[[작각자자리 뮤]] ([[NGC 6169]]에 존재)
|339,000
| -9.085
|3,260
| style="background: lightblue;" |4.91
|28,000
|{{SIMBAD link|Mu+Normae|SIMBAD}}
|<ref>{{저널 인용|last1=Lefever|first1=K.|last2=Puls|first2=J.|last3=Aerts|first3=C.|date=2007|title=Statistical properties of a sample of periodically variable B-type supergiants: Evidence for opacity-driven gravity-mode oscillations|journal=Astronomy & Astrophysics|volume=463|issue=3|pages=1093–1109|arxiv=astro-ph/0611484|bibcode=2007A&A...463.1093L|doi=10.1051/0004-6361:20066038|s2cid=8783008|issn=0004-6361}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[카시오페아자리 카파]] ([[카시오페아자리 OB14]]에 존재)
|302,000
| -8.96
|4,000
| style="background: lightblue;" |4.16
|23,500
|{{SIMBAD link|Kappa+Cassiopeiae|SIMBAD}}
|<ref name="Searle 20082"/><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[큰개자리 타우]] Aa ([[NGC 2362]]에 존재)
|299,000
| -8.95
|5,120
| style="background: lightblue;" |4.89
|32,000
|{{SIMBAD link|Tau+Canis+Majoris|SIMBAD}}
|<ref name="an331_4_3492">{{인용|last1=Hohle|first1=M. M.|title=Masses and luminosities of O- and B-type stars and red supergiants|date=April 2010|journal=Astronomische Nachrichten|volume=331|issue=4|page=349|arxiv=1003.2335|bibcode=2010AN....331..349H|doi=10.1002/asna.200911355|last2=Neuhäuser|first2=R.|last3=Schutz|first3=B. F.|s2cid=111387483}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[파리자리 세타]] Ab ([[센타우루스자리 OB1]]에 존재)
|295,000
| -8.935
|7,400
| style="background: lightblue;" |5.53 (연성계 전체)
|33,000
|{{SIMBAD link|Theta+Muscae+A|SIMBAD}}
|<ref>{{저널 인용|last1=Sugawara|first1=Y.|last2=Tsuboi|first2=Y.|last3=Maeda|first3=Y.|date=October 2008|title=Redshifted emission lines and radiative recombination continuum from the Wolf-Rayet binary θ Muscae: evidence for a triplet system?|journal=Astronomy & Astrophysics|volume=490|issue=1|pages=259–264|arxiv=0810.1208|bibcode=2008A&A...490..259S|doi=10.1051/0004-6361:20079302|issn=0004-6361|s2cid=118447784}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[돛자리 감마|돛자리 감마2]] B ([[돛자리 OB2]]에 존재)
|280,000
| -8.878
|1,230
| style="background: lightblue;" |1.83 (연성계 전체)
|35,000
|{{SIMBAD link|Gamma2+Velorum|SIMBAD}}
|<ref name=North /><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[멘키브]] ([[페르세우스자리 OB2]]의 [[캘리포니아 성운|NGC 1499]]에 존재)
| 263,000
| -8.81
| 1,200
| style="background: lightblue;" | 4.04
| 35,000
|{{SIMBAD link|Xi+Persei|SIMBAD}}
|<ref name="repolust" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[알니탁]] Aa ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|250,000
| -8.755
|1,260
| style="background: lightblue;" |2.08
|29,500
|{{SIMBAD link|Zeta+Orionis|SIMBAD}}
|<ref>{{저널 인용|last1=Hummel|first1=C. A.|last2=Rivinius|first2=Th.|last3=Nieva|first3=M.-F.|last4=Stahl|first4=O.|last5=van Belle|first5=G.|last6=Zavala|first6=R. T.|date=2013|title=Dynamical mass of the O-type supergiant in ζ Orionis A|journal=Astronomy & Astrophysics|volume=554|page=A52|arxiv=1306.0330|bibcode=2013A&A...554A..52H|doi=10.1051/0004-6361/201321434|s2cid=53645495|issn=0004-6361}}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[파리자리 세타]] Aa ([[센타우루스자리 OB1]]에 존재하는 WR 48)
|234,000
| -8.685
|7,400
| style="background: lightblue;" |5.53 (연성계 전체)
|83,000
|{{SIMBAD link|Theta+Muscae+A|SIMBAD}}
|<ref name="nugis">{{저널 인용|last1=Nugis|first1=T.|last2=Lamers|first2=H. J. G. L. M.|year=2000|title=Mass-loss rates of Wolf-Rayet stars as a function of stellar parameters|journal=Astronomy and Astrophysics|volume=360|page=227|bibcode=2000A&A...360..227N}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[큰개자리 오미크론2]] ([[콜린더 목록|콜린더 121]]에 존재)
|219,000
| -8.61
|2,800
| style="background: lightblue;" |3.043
|15,500
|{{SIMBAD link|Omicron2+Canis+Majoris|SIMBAD}}
|<ref name="aaa446_1_279">{{인용|last1=Crowther|first1=P. A.|title=Physical parameters and wind properties of galactic early B supergiants|date=January 2006|journal=Astronomy and Astrophysics|volume=446|issue=1|pages=279–293|arxiv=astro-ph/0509436|bibcode=2006A&A...446..279C|doi=10.1051/0004-6361:20053685|last2=Lennon|first2=D. J.|last3=Walborn|first3=N. R.|s2cid=18815761}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[오리온자리 세타1 C]]1 ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[사다리꼴성단]]에 존재)
| 204,000
| -8.535
| 1,340
| style="background: lightblue;" | 5.13 (연성계 전체)
| 39,000
|{{SIMBAD link|Theta1+Orionis+C|SIMBAD}}
|<ref>{{저널 인용|last1=Simón-Díaz|first1=S.|last2=Herrero|first2=A.|last3=Esteban|first3=C.|last4=Najarro|first4=F.|date=2006|title=Detailed spectroscopic analysis of the Trapezium cluster stars inside the Orion nebula: Rotational velocities, stellar parameters, and oxygen abundances|journal=Astronomy & Astrophysics|volume=448|issue=1|pages=351–366|arxiv=astro-ph/0510288|bibcode=2006A&A...448..351S|doi=10.1051/0004-6361:20053066|s2cid=16445304|issn=0004-6361}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[민타카]] Aa1 ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|191,000
| -8.46
|1,200
| style="background: lightblue;" |2.5 (연성계 전체)
|29,500
|{{SIMBAD link|Delta+Orionis+A|SIMBAD}}
|<ref name="shenar2015">{{저널 인용|last1=Shenar|first1=T.|last2=Oskinova|first2=L.|last3=Hamann|first3=W.-R.|last4=Corcoran|first4=M. F.|last5=Moffat|first5=A. F. J.|last6=Pablo|first6=H.|last7=Richardson|first7=N. D.|last8=Waldron|first8=W. L.|last9=Huenemoerder|first9=D. P.|last10=Maíz Apellániz|first10=J.|last11=Nichols|first11=J. S.|year=2015|title=A Coordinated X-Ray and Optical Campaign of the Nearest Massive Eclipsing Binary, δ Orionis Aa. IV. A Multiwavelength, Non-LTE Spectroscopic Analysis|journal=Astrophysical Journal|volume=809|issue=2|page=135|arxiv=1503.03476|bibcode=2015ApJ...809..135S|doi=10.1088/0004-637X/809/2/135|last13=Nazé|first13=Y.|last14=Hoffman|first14=J. L.|last15=Pollock|first15=A. M. T.|last16=Negueruela|first16=I.|first12=H.|last12=Todt|hdl=10045/59172|s2cid=14909574}}</ref><ref name=tokovinin1997>{{저널 인용|bibcode=1997A&AS..124...75T|title=MSC - a catalogue of physical multiple stars|journal=Astronomy and Astrophysics Supplement Series|volume=124|pages=75–84|last1=Tokovinin|first1=A. A.|year=1997|doi=10.1051/aas:1997181|doi-access=free}}</ref>
|-
| style="background: {{항성-색깔|WC}};" |[[돛자리 감마|돛자리 감마2]] A ([[돛자리 OB2]]에 존재하는 WR 11)
|170,000
| -8.336
|1,230
| style="background: lightblue;" |1.83 (연성계 전체)
|57,000
|{{SIMBAD link|Gamma2+Velorum|SIMBAD}}
|<ref name=North>{{저널 인용|last1=North|first1=J. R.|last2=Tuthill|first2=P. G.|last3=Tango|first3=W. J.|last4=Davis|first4=J.|date=2007-05-01|title=γ2 Velorum: orbital solution and fundamental parameter determination with SUSI|journal=Monthly Notices of the Royal Astronomical Society|volume=377|issue=1|pages=415–424|arxiv=astro-ph/0702375|bibcode=2007MNRAS.377..415N|doi=10.1111/j.1365-2966.2007.11608.x|s2cid=16425744|issn=0035-8711}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[알루드라]] ([[콜린더 목록|콜린더 121]]에 존재)
|151,000
| -8.21
|2,000
| style="background: lightblue;" |2.45
|15,000
|{{SIMBAD link|Eta+Canis+Majoris|SIMBAD}}
|<ref name="Searle 20082"/><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[남십자자리 카파 (항성)|남십자자리 카파]] ([[센타우루스자리 OB1]]의 [[보석상자 성단]]에 존재)
|151,000
| -8.21
|7,500
| style="background: lightblue;" |5.98
|16,300
|{{SIMBAD link|Kappa+Crucis|SIMBAD}}
|<ref>{{저널 인용|last1=Dufton|first1=P. L.|last2=Smartt|first2=S. J.|last3=Lee|first3=J. K.|last4=Ryans|first4=R. S. I.|last5=Hunter|first5=I.|last6=Evans|first6=C. J.|last7=Herrero|first7=A.|last8=Trundle|first8=C.|last9=Lennon|first9=D. J.|last10=Irwin|first10=M. J.|last11=Kaufer|first11=A.|date=2006|title=The VLT-FLAMES survey of massive stars: stellar parameters and rotational velocities in NGC 3293, NGC 4755 and NGC 6611|journal=Astronomy & Astrophysics|volume=457|issue=1|pages=265–280|arxiv=astro-ph/0606409|bibcode=2006A&A...457..265D|doi=10.1051/0004-6361:20065392|s2cid=15874925|issn=0004-6361}}</ref><ref name="tycho2" />
|-
| style="background: {{항성-색깔|O}};" |[[메이사]] A ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 람다 성단|콜린더 69]]에 존재)
|150,000
| -8.2
|1,100
| style="background: lightblue;" |3.54
|37,700
|{{SIMBAD link|Lambda+Orionis+A|SIMBAD}}
|<ref>{{저널 인용|last1=Murdin|first1=P.|last2=Penston|first2=M. V.|date=1977-12-01|title=The Lambda Orionis association|journal=Monthly Notices of the Royal Astronomical Society|volume=181|issue=4|pages=657–665|bibcode=1977MNRAS.181..657M|doi=10.1093/mnras/181.4.657|issn=0035-8711|doi-access=free}}</ref><ref name="hr">{{서적 인용|last1=Hoffleit|first1=Dorrit|title=The Bright star catalogue|last2=Jaschek|first2=Carlos|publisher=Yale University Observatory|year=1991|edition=5th Revised|location=New Haven, Conn.|bibcode=1991bsc..book.....H}}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[리겔]] A ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|120,000
| -7.96
|860
| style="background: lightblue;" |0.13
|12,100
|{{SIMBAD link|Beta+Orionis+A|SIMBAD}}
|<ref>{{저널 인용|last1=Moravveji|first1=Ehsan|last2=Guinan|first2=Edward F.|last3=Shultz|first3=Matt|last4=Williamson|first4=Michael H.|last5=Moya|first5=Andres|title=Asteroseismology of the Nearby SN-II Progenitor: Rigel. I. Themosthigh-Precision Photometry and Radial Velocity Monitoring|date=2012-03-10|journal=The Astrophysical Journal|volume=747|issue=2|page=108|arxiv=1201.0843|bibcode=2012ApJ...747..108M|doi=10.1088/0004-637X/747/2/108|s2cid=425831|issn=0004-637X}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[오리온자리 세타2]] A ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|107,000
| -7.833
|1,500
| style="background: lightblue;" |5.02
|34,900
|{{SIMBAD link|Theta2+Orionis+A|SIMBAD}}
|<ref name=hillendrand>{{저널 인용|bibcode= 1997AJ....113.1733H|title= On the Stellar Population and Star-Forming History of the Orion Nebula Cluster|journal= Astronomical Journal |volume= 113|page=1733|last1= Hillenbrand|first1= Lynne A.|year= 1997|doi= 10.1086/118389}}</ref><ref>{{저널 인용|bibcode=2015AJ....149...26A|title=The Multiplicity of Massive Stars: A High Angular Resolution Survey with the Guidance Sensor|journal=The Astronomical Journal|volume=149|page=26|last1=Aldoretta|first1=E. J.|last2=Caballero-Nieves|first2=S. M.|last3=Gies|first3=D. R.|last4=Nelan|first4=E. P.|last5=Wallace|first5=D. J.|last6=Hartkopf|first6=W. I.|last7=Henry|first7=T. J.|last8=Jao|first8=W.-C.|last9=Maíz Apellániz|first9=J.|last10=Mason|first10=B. D.|last11=Moffat|first11=A. F. J.|last12=Norris|first12=R. P.|last13=Richardson|first13=N. D.|last14=Williams|first14=S. J.|year=2015|issue=1|doi=10.1088/0004-6256/149/1/26|arxiv = 1410.0021 |s2cid=58911264}}</ref>
|-
| style="background: {{항성-색깔|M}};" |[[베텔게우스]]
|87,100
| -7.61
|550
|style="background: lightblue;" |0.50
|3,600
|[https://simbad.cds.unistra.fr/simbad/sim-id?Ident=HD+39801 SIMBAD]
|<ref>{{저널 인용|last1=Joyce |first1=Meridith |last2=Leung |first2=Shing-Chi |last3=Molnár |first3=László |last4=Ireland |first4=Michael J. |last5=Kobayashi |first5=Chiaki |last6=Nomoto |first6=Ken'ichi |date=2020-10-13 |title=Standing on the shoulders of giants: New mass and distance estimates for Betelgeuse through combined evolutionary, asteroseismic, and hydrodynamical simulations with MESA |journal=The Astrophysical Journal |volume=902 |issue=1 |pages=63 |doi=10.3847/1538-4357/abb8db |arxiv=2006.09837 |bibcode=2020ApJ...902...63J |issn=1538-4357 |doi-access=free }}</ref><ref>{{저널 인용|last=Nicolet |first=B. |date=1978-10-01 |title=Catalogue of homogeneous data in the UBV photoelectric photometric system. |url=https://ui.adsabs.harvard.edu/abs/1978A&AS...34....1N |journal=Astronomy and Astrophysics Supplement Series |volume=34 |pages=1–49 |bibcode=1978A&AS...34....1N |issn=0365-0138}}</ref>
|-
| style="background: {{항성-색깔|O}};" |[[땅꾼자리 제타]] ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[전갈자리-센타우루스자리 성협|상부 전갈자리 성협]]에 존재)
|74,100
| -7.435
|370
| style="background: lightblue;" |2.569
|34,000
|{{SIMBAD link|Zeta+Ophiuchi|SIMBAD}}
|<ref name="repolust" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[하트샤]] Aa1 ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[NGC 1980]]에 존재)
|68,000
| -7.341
|1,340
| style="background: lightblue;" |2.77 (연성계 전체)
|32,500
|{{SIMBAD link|Iota+Orionis|SIMBAD}}
|<ref name=marchenko>{{저널 인용|bibcode=2000MNRAS.317..333M|title=Coordinated monitoring of the eccentric O-star binary Iota Orionis: Optical spectroscopy and photometry|journal=Monthly Notices of the Royal Astronomical Society|volume=317|issue=2|page=333|last1=Marchenko|first1=Sergey V.|last2=Rauw|first2=Gregor|last3=Antokhina|first3=Eleonora A.|last4=Antokhin|first4=Igor I.|last5=Ballereau|first5=Dominique|last6=Chauville|first6=Jacques|last7=Corcoran|first7=Michael F.|last8=Costero|first8=Rafael|last9=Echevarria|first9=Juan|last10=Eversberg|first10=Thomas|last11=Gayley|first11=Ken G.|last12=Koenigsberger|first12=Gloria|author12-link=Gloria Suzanne Koenigsberger Horowitz|last13=Miroshnichenko|first13=Anatoly S.|last14=Moffat|first14=Anthony F. J.|last15=Morrell|first15=Nidia I.|last16=Morrison|first16=Nancy D.|last17=Mulliss|first17=Christopher L.|last18=Pittard|first18=Julian M.|last19=Stevens|first19=Ian R.|last20=Vreux|first20=Jean-Marie|last21=Zorec|first21=Jean|year=2000|doi=10.1046/j.1365-8711.2000.03542.x|doi-access=free}}</ref><ref name=aass34_1/>
|-
| style="background: {{항성-색깔|O}};" |[[오리온자리 웁실론]] ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|60,000
| -7.205
|2,900
| style="background: lightblue;" |4.618
|33,400
|{{SIMBAD link|Upsilon+Orionis|SIMBAD}}
|<ref name="underhill79">{{저널 인용|author=Underhill, A. B.|author2=Divan, L.|author3=Prevot-Burnichon, M.-L.|author4=Doazan, V.|date=1979|title=Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars|journal=[[Monthly Notices of the Royal Astronomical Society]]|volume=189|issue=3|pages=601–05|bibcode = 1979MNRAS.189..601U|doi=10.1093/mnras/189.3.601|doi-access=free}}</ref><ref>{{저널 인용|last=Nieva|first=M.-F.|date=2013|title=Temperature, gravity, and bolometric correction scales for non-supergiant OB stars|journal=Astronomy & Astrophysics|volume=550|page=A26|arxiv=1212.0928|bibcode=2013A&A...550A..26N|doi=10.1051/0004-6361/201219677|s2cid=119275940|issn=0004-6361}}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[사이프|오리온자리 카파]] ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|57,000
| -7.147
|650
| style="background: lightblue;" |2.09
|26,500
|{{SIMBAD link|Kappa+Orionis|SIMBAD}}
|<ref name="an331_4_3492" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[백조자리 시그마]] ([[백조자리 OB4]]에 존재)
|52,000
| -7.06
|3,260
| style="background: lightblue;" |4.233
|10,800
|{{SIMBAD link|Sigma+Cygni|SIMBAD}}
|<ref name="tanriverdi">{{저널 인용|last1=Tanrıverdi|first1=Taner|year=2013|title=Elemental abundances of the supergiant stars σ Cygnus and η Leonis|journal=New Astronomy|volume=25|page=50|arxiv=1512.04557|bibcode=2013NewA...25...50T|doi=10.1016/j.newast.2013.03.013|s2cid=118525375}}</ref><ref name="firnstein">{{저널 인용|last1=Firnstein|first1=M.|last2=Przybilla|first2=N.|year=2012|title=Quantitative spectroscopy of Galactic BA-type supergiants. I. Atmospheric parameters|journal=Astronomy & Astrophysics|volume=543|page=A80|arxiv=1207.0308|bibcode=2012A&A...543A..80F|doi=10.1051/0004-6361/201219034|s2cid=54725386}}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[페르세우스자리 제타]] ([[페르세우스자리 OB2]]에 존재)
|47,000
| -6.941
|750
| style="background: lightblue;" |2.86
|20,800
|{{SIMBAD link|Zeta+Persei|SIMBAD}}
|<ref name="an331_4_3492" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[비둘기자리 뮤]] ([[사다리꼴성단]]에 존재하는 [[폭주성]])
|46,000
| -6.91
|1,300
| style="background: lightblue;" |5.18
|33,000
|{{SIMBAD link|mu+Columbae|SIMBAD}}
|<ref name=":15">{{저널 인용|last1=Martins|first1=F.|last2=Schaerer|first2=D.|last3=Hillier|first3=D. J.|last4=Meynadier|first4=F.|last5=Heydari-Malayeri|first5=M.|last6=Walborn|first6=N. R.|date=2005|title=O stars with weak winds: the Galactic case|journal=Astronomy & Astrophysics|volume=441|issue=2|pages=735–762|arxiv=astro-ph/0507278|bibcode=2005A&A...441..735M|doi=10.1051/0004-6361:20052927|s2cid=11547293|issn=0004-6361}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|O}};" |[[오리온자리 시그마]] Aa ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|41,700
| -6.81
|1,260
| style="background: lightblue;" |4.07 (연성계 전체)
|35,000
|{{SIMBAD link|Sigma+Orionis+A|SIMBAD}}
|<ref name=simondiaz2015>{{저널 인용|bibcode=2015ApJ...799..169S|arxiv=1412.3469|title=Orbital and Physical Properties of the σ Ori Aa, Ab, B Triple System|journal=The Astrophysical Journal|volume=799|issue=2|page=169|last1=Simón-Díaz|first1=S.|last2=Caballero|first2=J. A.|last3=Lorenzo|first3=J.|last4=Maíz Apellániz|first4=J.|last5=Schneider|first5=F. R. N.|last6=Negueruela|first6=I.|last7=Barbá|first7=R. H.|last8=Dorda|first8=R.|last9=Marco|first9=A.|last10=Montes|first10=D.|last11=Pellerin|first11=A.|last12=Sanchez-Bermudez|first12=J.|last13=Sódor|first13=Á.|last14=Sota|first14=A.|year=2015|doi=10.1088/0004-637X/799/2/169|s2cid=118500350}}</ref><ref name=wds>{{저널 인용|bibcode=2001AJ....122.3466M|title=The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog|journal=The Astronomical Journal|volume=122|issue=6|page=3466|last1=Mason|first1=Brian D.|last2=Wycoff|first2=Gary L.|last3=Hartkopf|first3=William I.|last4=Douglass|first4=Geoffrey G.|last5=Worley|first5=Charles E.|year=2001|doi=10.1086/323920|doi-access=free}}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[드슈바]] A ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[전갈자리-센타우루스자리 성협|상부 전갈자리 성협]]에 존재)
|38,000
| -6.71
|440
| style="background: lightblue;" |2.307 (연성계 전체)
|27,400
|{{SIMBAD link|Delta+Scorpii|SIMBAD}}
|<ref name=Pecaut>{{저널 인용|last1=Pecaut|first1=Mark J.|last2=Mamajek|first2=Eric E.|last3=Bubar|first3=Eric J.|title=A Revised Age for Upper Scorpius and the Star Formation History Among the F-Type Members of the Scorpius–Centaurus Ob Association|date=2012-02-20|journal=The Astrophysical Journal|volume=746|issue=2|page=154|arxiv=1112.1695|bibcode=2012ApJ...746..154P|doi=10.1088/0004-637X/746/2/154|s2cid=118461108|issn=0004-637X}}</ref><ref>{{저널 인용|last1=Gutierrez-Moreno|first1=Adelina|last2=Moreno|first2=Hugo|date=1968-06-01|title=A Photometric Investigation of the SCORPlO-CENTAURUS Association|journal=The Astrophysical Journal Supplement Series|volume=15|page=459|bibcode=1968ApJS...15..459G|doi=10.1086/190168|issn=0067-0049|doi-access=free}}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[페르세우스자리 엡실론]] A ([[페르세우스자리 알파 성단]]에 존재)
|28,300
| -6.391
|640
| style="background: lightblue;" |2.88 (연성계 전체)
|26,500
|{{SIMBAD link|Epsilon+Persei|SIMBAD}}
|<ref name="an331_4_3492" /><ref name=aj82_431>{{인용| last1=Lutz | first1=T. E. | last2=Lutz | first2=J. H.	|author2-link= Julie Lutz | title=Spectral classification and UBV photometry of bright visual double stars | journal=Astronomical Journal | volume=82 | pages=431–434 |date=June 1977 | doi=10.1086/112066 | bibcode=1977AJ.....82..431L | doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[용골자리 세타]] A ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[IC 2602]]에 존재)
|25,700
| -6.284
|460
| style="background: lightblue;" |2.76 (연성계 전체)
|31,000
|{{SIMBAD link|Theta+Carinae|SIMBAD}}
|<ref name="an331_4_3492" /><ref name="clpl4" />
|-
| style="background: {{항성-색깔|B}};" |[[미르잠]] ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[국부 거품]]에 존재)
|25,000
| -6.26
|490
| style="background: lightblue;" |1.985
|23,200
|{{SIMBAD link|Beta+Canis+Majoris|SIMBAD}}
|<ref name=mnras369_1_L61>{{인용| display-authors=1 | last1=Hubrig | first1=S. | last2=Briquet | first2=M. | last3=Schöller | first3=M. | last4=De Cat | first4=P. | last5=Mathys | first5=G. | last6=Aerts | first6=C. | title=Discovery of magnetic fields in the βCephei star ξ1 CMa and in several slowly pulsating B stars* | journal=[[Monthly Notices of the Royal Astronomical Society: Letters]] | volume=369 | issue=1 | pages=L61–L65 |date=June 2006 | doi=10.1111/j.1745-3933.2006.00175.x | bibcode=2006MNRAS.369L..61H |arxiv = astro-ph/0604283 | s2cid=18201908 }}</ref><ref name=mnassa31_69>{{인용| title=UBV Photometry of Some Very Bright Stars | last1=Cousins | first1=A. W. J. | journal=Monthly Notes of the Astronomical Society of Southern Africa | volume=31 | page=69 | date=1972 | bibcode=1972MNSSA..31...69C }}</ref>
|-
| style="background: {{항성-색깔|O}};" |[[오리온자리 시그마]] Ab ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|18,600
| -5.934
|1,260
| style="background: lightblue;" |4.07 (연성계 전체)
|29,000
|{{SIMBAD link|Sigma+Orionis+A|SIMBAD}}
|<ref name=simondiaz2015/><ref name=wds/>
|-
| style="background: {{항성-색깔|B}};" |[[오리온자리 시그마]] B ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|15,800
| -5.757
|1,260
| style="background: lightblue;" |4.07 (연성계 전체)
|31,000
|{{SIMBAD link|Sigma+Orionis+B|SIMBAD}}
|<ref name=simondiaz2015/><ref name=wds/>
|-
| style="background: {{항성-색깔|B}};" |[[오리온자리 세타2]] B ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|12,300
| -5.485
|1,500
| style="background: lightblue;" |6.38
|29,300
|{{SIMBAD link|Theta2+Orionis+B|SIMBAD}}
|<ref name=nieva>{{저널 인용|bibcode=2014A&A...566A...7N|arxiv=1412.1418|title=Fundamental properties of nearby single early B-type stars|journal=Astronomy & Astrophysics|volume=566|page=A7|last1=Nieva|first1=María-Fernanda|last2=Przybilla|first2=Norbert|year=2014|doi=10.1051/0004-6361/201423373|s2cid=119227033}}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[벨라트릭스]] ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[벨라트릭스|벨라트릭스 성단]]에 존재)
|9,210
| -5.17
|250
| style="background: lightblue;" |1.64
|21,800
|{{SIMBAD link|Gamma+Orionis|SIMBAD}}
|<ref name="challouf2">{{저널 인용|last1=Challouf|first1=M.|last2=Nardetto|first2=N.|last3=Mourard|first3=D.|last4=Graczyk|first4=D.|last5=Aroui|first5=H.|last6=Chesneau|first6=O.|last7=Delaa|first7=O.|last8=Pietrzyński|first8=G.|last9=Gieren|first9=W.|last10=Ligi|first10=R.|last11=Meilland|first11=A.|year=2014|title=Improving the surface brightness-color relation for early-type stars using optical interferometry⋆|journal=Astronomy & Astrophysics|volume=570|page=A104|arxiv=1409.1351|bibcode=2014A&A...570A.104C|doi=10.1051/0004-6361/201423772|first12=K.|first18=N.|last12=Perraut|first21=N.|last21=Scott|first20=N.|last20=Vargas|first19=C.|last19=Farrington|last18=Turner|last13=Tallon-Bosc|first17=L.|last17=Sturmann|first16=J.|last16=Sturmann|first15=T.|last15=Ten Brummelaar|first14=H.|last14=McAlister|first13=I.|s2cid=14624307}}</ref><ref name="ducati2">{{저널 인용|last1=Ducati|first1=J. R.|date=2002|title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system.|journal=CDS/ADC Collection of Electronic Catalogues|volume=2237|bibcode=2002yCat.2237....0D|s2cid=118191108}}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[하트샤]] Aa2 ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[NGC 1980]]에 존재)
|8,630
| -5.1
|1,340
| style="background: lightblue;" |2.77 (연성계 전체)
|27,000
|{{SIMBAD link|Iota+Orionis|SIMBAD}}
|<ref name="marchenko" /><ref name="aass34_1" />
|-
| style="background: {{항성-색깔|B}};" |[[황소자리 람다]] A ([[물고기자리-에리다누스자리 성류]]에 존재)
|5,800
| -4.669
|480
| style="background: lightblue;" |3.47 (연성계 전체)
|18,700
|{{SIMBAD link|Lambda+Tauri|SIMBAD}}
|<ref name="an331_4_3492" /><ref name=aaass34_1>{{저널 인용| last1=Nicolet | first1=B. | title=Catalogue of homogeneous data in the UBV photoelectric photometric system | journal=Astronomy and Astrophysics Supplement Series | volume=34 | pages=1–49 |date=October 1978 | bibcode=1978A&AS...34....1N }}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[땅꾼자리 로]] A ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[땅군자리 로 분자운 복합체]]에 존재)
|4,000
| -4.285
|360
| style="background: lightblue;" |4.63 (연성계 전체)
|22,000
|{{SIMBAD link|Rho+Ophiuchi+A|SIMBAD}}
|<ref>{{저널 인용|last1=Pillitteri|first1=I.|last2=Fossati|first2=L.|last3=Castro Rodriguez|first3=N.|last4=Oskinova|first4=L.|last5=Wolk|first5=S. J.|date=2018|title=Detection of magnetic field in the B2 star ρ Ophiuchi A with ESO FORS2|journal=Astronomy & Astrophysics|volume=610|page=L3|arxiv=1712.00728|bibcode=2018A&A...610L...3P|doi=10.1051/0004-6361/201732078|s2cid=119395824|issn=0004-6361}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[페르세우스자리 델타]] ([[페르세우스자리 알파 성단]]에 존재)
|2,860
| -3.901
|520
| style="background: lightblue;" |3.01
|14,900
|{{SIMBAD link|Delta+Persei|SIMBAD}}
|<ref name="XHIP" /><ref name=clpl4/>
|-
| style="background: {{항성-색깔|B}};" |[[안타레스]] B ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[루프 I 거품]]에 존재)
|2,820
| -3.885
|550
| style="background: lightblue;" |5.5
|18,500
|{{SIMBAD link|Alpha+Scorpii+B|SIMBAD}}
|<ref name=antaresb>{{저널 인용|bibcode=1978A&A....70..227K|title=On the absolute scale of mass-loss in red giants. II. Circumstellar absorption lines in the spectrum of alpha Sco B and mass-loss of alpha Sco A|journal=Astronomy and Astrophysics|volume=70|page=227|last1=Kudritzki|first1=R. P.|last2=Reimers|first2=D.|date=1978}}</ref><ref name=hr/>
|-
| style="background: {{항성-색깔|B}};" |[[피콕 (항성)]] Aa ([[큰부리새자리-시계자리 성협]]에 존재)
|2,150
| -3.593
|180
| style="background: lightblue;" |1.94
|17,700
|{{SIMBAD link|Alpha+Pavonis|SIMBAD}}
|<ref name=aa50_369>{{인용| last1=Jerzykiewicz | first1=M. | last2=Molenda-Zakowicz | first2=J. | title=Empirical Luminosities and Radii of Early-Type Stars after Hipparcos | journal=Acta Astronomica | volume=50 | pages=369–380 |date=September 2000 | bibcode=2000AcA....50..369J }}</ref><ref name=aass34_1>{{인용| last1=Nicolet | first1=B. | year=1978 | title=Photoelectric photometric Catalogue of homogeneous measurements in the UBV System | journal=Astronomy and Astrophysics Supplement Series | volume=34 | pages=1–49 | bibcode=1978A&AS...34....1N }}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[알키오네 (항성)]] A ([[플레이아데스 성단]]에 존재)
|1,820
| -3.409
|440
| style="background: lightblue;" |2.87 (연성계 전체)
|12,300
|{{SIMBAD link|Eta+Tauri|SIMBAD}}
|<ref name=harmanec>{{저널 인용|bibcode=2000ASPC..214...13H|title=Physical Properties and Evolutionary Stage of Be Stars|journal=The be Phenomenon in Early-Type Stars|volume=214|page=13|last1=Harmanec|first1=P.|year=2000}}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[돛자리 오미크론]] ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[IC 2391]]에 존재)
|1,000
| -2.76
|490
| style="background: lightblue;" |3.6
|16,200
|{{SIMBAD link|Omicron+Velorum|SIMBAD}}
|<ref>{{저널 인용|last1=Hubrig|first1=S.|last2=Briquet|first2=M.|last3=De Cat|first3=P.|last4=Schöller|first4=M.|last5=Morel|first5=T.|last6=Ilyin|first6=I.|date=2009|title=New magnetic field measurements of β Cephei stars and slowly pulsating B stars|journal=Astronomische Nachrichten|volume=330|issue=4|pages=317–329|arxiv=0902.1314|bibcode=2009AN....330..317H|doi=10.1002/asna.200811187|s2cid=17497112}}</ref><ref name=clpl4>{{인용| display-authors=1 | last1=Johnson | first1=H. L. | last2=Iriarte | first2=B. | last3=Mitchell | first3=R. I. | last4=Wisniewskj | first4=W. Z. | title=UBVRIJKL photometry of the bright stars | journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | page=99 | year=1966 | bibcode=1966CoLPL...4...99J }}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[페르세우스자리 프시]] ([[페르세우스자리 알파 성단]]에 존재)
|775
| -2.483
|580
| style="background: lightblue;" |4.31
|16,000
|{{SIMBAD link|Psi+Persei|SIMBAD}}
|<ref name="XHIP" /><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[뮬리파인]] ([[콜린더 목록|콜린더 121]]에 존재)
|715
| -2.397
|440
| style="background: lightblue;" |4.1
|13,600
|{{SIMBAD link|Gamma+Canis+Majoris|SIMBAD}}
|<ref name="XHIP" /><ref name=apjss52_7>{{인용| last1=Fernie | first1=J. D. | title=New UBVRI photometry for 900 supergiants | journal=Astrophysical Journal Supplement Series | volume=52 | pages=7–22 | date=May 1983 | doi=10.1086/190856 | bibcode=1983ApJS...52....7F | postscript=. | doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[물병자리 오미크론]] ([[물고기자리-에리다누스자리 성류]]에 존재)
|340
| -1.589
|440
| style="background: lightblue;" |4.71
|13,500
|{{SIMBAD link|Omicron+Aquarii|SIMBAD}}
|<ref name=XHIP/><ref name=aj84_1713>{{인용| last1=Feinstein | first1=A. | last2=Marraco | first2=H. G. | title=The photometric behavior of Be Stars | journal=Astronomical Journal | volume=84 | pages=1713–1725 |date=November 1979 | doi=10.1086/112600 | bibcode=1979AJ.....84.1713F | postscript=. | doi-access=free }}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[에리다누스자리 피]] ([[큰부리새자리-시계자리 성협]]에 존재)
| 255
| -1.276
|150
| style="background: lightblue;" |3.55
|13,700
|{{SIMBAD link|Phi+Eridani|SIMBAD}}
|<ref name=Mcdonald2012>{{인용| display-authors=1 | last1=McDonald | first1=I. | last2=Zijlstra | first2=A. A. | last3=Boyer | first3=M. L. | title=Fundamental Parameters and Infrared Excesses of Hipparcos Stars | journal=Monthly Notices of the Royal Astronomical Society | volume=427 | issue=1 | pages=343–57 | date=2012 | bibcode=2012MNRAS.427..343M | arxiv=1208.2037 | doi = 10.1111/j.1365-2966.2012.21873.x | s2cid=118665352 | postscript=. }}</ref><ref name=Mermilliod1986>{{인용| last1=Mermilliod | first1=J.-C. | title=Compilation of Eggen's UBV data, transformed to UBV (unpublished) | journal=Catalogue of Eggen's UBV Data | publisher=[[SIMBAD]] | date=1986 | bibcode=1986EgUBV........0M | postscript=. }}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[화로자리 누]] ([[물고기자리-에리다누스자리 성류]]에 존재)
|245
| -1.233
|370
| style="background: lightblue;" |4.69
|13,400
|{{SIMBAD link|nu+Fornacis|SIMBAD}}
|<ref name=aaa334_181>{{저널 인용| last1=North | first1=P. | title=Do SI stars undergo any rotational braking? | journal=Astronomy and Astrophysics | volume=334 | pages=181–87 | date=1998 | bibcode=1998A&A...334..181N | arxiv=astro-ph/9802286 }}</ref><ref name="ducati" />
|-
| style="background: {{항성-색깔|B}};" |[[카멜레온자리 엡실론]] ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[카멜레온자리 엡실론 운동성단]]에 존재)
|100
| -0.26
|360
| style="background: lightblue;" |4.91
|10,900
|{{SIMBAD link|Epsilon+Chamaeleontis|SIMBAD}}
|<ref name=Fang2013>{{인용| title=Young stars in ɛ Chamaleontis and their disks: disk evolution in sparse associations | last1=Fang | first1=M. | last2=van Boekel | first2=R. | last3=Bouwman | first3=J. | last4=Henning | first4=Th. | last5=Lawson | first5=W. A. | last6=Sicilia-Aguilar | first6=A. | journal=Astronomy & Astrophysics | display-authors=1 | volume=549 | id=A15 | page=17 | date=January 2013 | doi=10.1051/0004-6361/201118528 | bibcode=2013A&A...549A..15F | arxiv=1209.5832 | s2cid=118332644 | postscript=.}}</ref><ref name=clpl4/>
|-
| style="background: {{항성-색깔|B}};" |[[카멜레온자리 에타]] ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[카멜레온자리 에타 운동성단]]에 존재)
|95
| -0.204
|310
| style="background: lightblue;" |5.453
|12,500
|{{SIMBAD link|Eta+Chamaeleontis|SIMBAD}}
|<ref name="XHIP" /><ref name="tycho2" />
|-
| style="background: {{항성-색깔|B}};" |[[물뱀자리 엡실론]] ([[큰부리새자리-시계자리 성협]]에 존재)
|60
|0.295
|150
| style="background: lightblue;" |4.12
|11,000
|{{SIMBAD link|Epsilon+Hydri|SIMBAD}}
|<ref name=Zorec2012>{{저널 인용| arxiv=1201.2052 | bibcode=2012A&A...537A.120Z | doi=10.1051/0004-6361/201117691 | title=Rotational velocities of A-type stars | journal=Astronomy & Astrophysics | volume=537 | page=A120 | year=2012 | last1=Zorec | first1=J. | last2=Royer | first2=F. | s2cid=55586789 }} [http://vizier.u-strasbg.fr/viz-bin/VizieR-4?-source=J/A%2bA/537/A120/table1&HD=16978 Vizier catalog entry]</ref><ref name=XHIP>{{저널 인용| bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015 | arxiv=1108.4971 | title=XHIP: An extended hipparcos compilation | journal=Astronomy Letters | volume=38 | issue=5 | page=331 | year=2012 | last1=Anderson | first1=E. | last2=Francis | first2=Ch. | s2cid=119257644 }} [http://vizier.u-strasbg.fr/viz-bin/VizieR-4?-source=V/137D/XHIP&HIP=12394 Vizier catalog entry]</ref>
|-
| style="background: {{항성-색깔|B}};" |[[물병자리 타우1]] ([[물고기자리-에리다누스자리 성류]]에 존재)
|50
|0.429
|320
| style="background: lightblue;" |5.66
|10,600
|{{SIMBAD link|Tau1+Aquarii|SIMBAD}}
|<ref name=XHIP/><ref name=mnrassa27_11>{{인용| last1=Corben | first1=P. M. | last2=Stoy | first2=R. H. | title=Photoelectric Magnitudes and Colours for Bright Southern Stars | journal=Monthly Notes of the Astronomical Society of Southern Africa | volume=27 | page=11 | year=1968 | bibcode=1968MNSSA..27...11C | postscript=. }}</ref>
|-
| style="background: {{항성-색깔|B}};" |[[큰부리새자리 베타]] ([[큰부리새자리-시계자리 성협]]에 존재)
|40
|0.735
|140
| style="background: lightblue;" |4.37
|10,600
|{{SIMBAD link|Beta1+Tucanae|SIMBAD}}
|<ref>{{인용| title=The Hα Profiles of Be Shell Stars  | last1=Silaj | first1=J. | last2=Jones | first2=C. E.  | last3=Sigut | first3=T. A. A. | last4=Tycner | first4=C.  | display-authors=1 | journal=The Astrophysical Journal  | volume=795 | issue=1 | id=82 | page=12 | date=November 2014  | doi=10.1088/0004-637X/795/1/82 | bibcode=2014ApJ...795...82S  | s2cid=120167606 | postscript=. }}</ref><ref name=hr/>
|-
| style="background:lightyellow;" | [[태양]] ([[태양계]]에 존재)
| 1
| 4.739996
| 0.0000158
| style="background: lightyellow;" | -26.744
| 5,772
|{{URL | 1=https://www.iau.org/static/resolutions/IAU2015_English.pdf| 2=IAU}}
|<ref>{{저널 인용|bibcode = 2016AJ....152...41P|title = Nominal Values for Selected Solar and Planetary Quantities: IAU 2015 Resolution B3|last1 = Prša|first1 = Andrej|last2 = Harmanec|first2 = Petr|last3 = Torres|first3 = Guillermo|last4 = Mamajek|first4 = Eric|last5 = Asplund|first5 = Martin|last6 = Capitaine|first6 = Nicole|last7 = Christensen-Dalsgaard|first7 = Jørgen|last8 = Depagne|first8 = Éric|last9 = Haberreiter|first9 = Margit|last10 = Hekker|first10 = Saskia|last11 = Hilton|first11 = James|last12 = Kopp|first12 = Greg|last13 = Kostov|first13 = Veselin|last14 = Kurtz|first14 = Donald W.|last15 = Laskar|first15 = Jacques|last16 = Mason|first16 = Brian D.|last17 = Milone|first17 = Eugene F.|last18 = Montgomery|first18 = Michele|last19 = Richards|first19 = Mercedes|last20 = Schmutz|first20 = Werner|last21 = Schou|first21 = Jesper|last22 = Stewart|first22 = Susan G.|journal = The Astronomical Journal|year = 2016|volume = 152|issue = 2|page = 41|doi = 10.3847/0004-6256/152/2/41|arxiv = 1605.09788|hdl = 1885/108637|s2cid = 55319250 | doi-access=free }}</ref><ref>{{저널 인용|last1=Luzum|first1=Brian|last2=Capitaine|first2=Nicole|last3=Fienga|first3=Agnès|last4=Folkner|first4=William|last5=Fukushima|first5=Toshio|last6=Hilton|first6=James|last7=Hohenkerk|first7=Catherine|last8=Krasinsky|first8=George|last9=Petit|first9=Gérard|last10=Pitjeva|first10=Elena|last11=Soffel|first11=Michael|date=August 2011|title=The IAU 2009 system of astronomical constants: the report of the IAU working group on numerical standards for Fundamental Astronomy|journal=Celestial Mechanics and Dynamical Astronomy|volume=110|issue=4|pages=293–304|bibcode=2011CeMDA.110..293L|doi=10.1007/s10569-011-9352-4|issn=0923-2958|doi-access=free}}</ref><ref>{{저널 인용|last1=Bessell|first1=M.S.|last2=Castelli|first2=F.|last3=Plez|first3=B.|date=1998|title=Model atmospheres broad-band colors, bolometric corrections and temperature calibrations for O–M stars|journal=[[Astronomy and Astrophysics]]|volume=333|pages=231–250|bibcode=1998A&A...333..231B}}</ref>
|}
{{각주|group=lower-alpha}}

== 같이 보기 ==
* [[반지름 순 별 목록]]
* [[질량이 큰 별 목록]]
* [[유효온도가 낮은 항성 목록]]
* [[유효온도가 높은 항성 목록]]
* [[겉보기등급 순 항성 목록]]
* [[가까운 별 목록]]
* [[퀘이사]]
* [[감마선 폭발]]
* [[거리지수]]

[[분류:항성 목록]]
[[분류:항성 목록]]
[[분류:우리은하]]