View source for R136

{{Short description|Super star cluster in the constellation Dorado, in the Large Magellanic Cloud}}
{{about|the star cluster|the road in Dublin|R136 road|routes 136|route 136}}

{{Infobox open cluster
| name= '''R136'''
| image= [[File:Grand star-forming region R136 in NGC 2070 (captured by the Hubble Space Telescope).jpg|280px]]
| caption = In ultraviolet, visible, and red light by [[Hubble Space Telescope]] Wide Field Camera 3
| credit= NASA, ESA
| epoch = J2000.0
| constellation = [[Dorado]]
| ra = {{RA|05|38|42.396}}<ref name=tycho2>{{cite journal |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. |title=The Tycho-2 catalogue of the 2.5 million brightest stars – Letter to the Editor |journal=Astronomy and Astrophysics |volume=355 |pages=L27–L30 |date=January 2000 |bibcode=2000A&A...355L..27H}}</ref>
| dec = {{DEC|-69|06|03.36}}<ref name=tycho2/>
| dist_ly = [[1 E21 m|157]] [[light-year|kly]]
| dist_pc = 48.5 [[parsec|kpc]]
| appmag_v = 9.50
| age = {{val|1.5|0.3|0.7}} million years<ref name=crowther2016/>
| mass_msol = 90,000<ref name=crowther2016/>
| names = UCAC2 1803442, SAO 249329, HD 38268, TYC 9163-1014-1, CD-69 324, GC 7114<ref name="simbadq">{{cite simbad|title=RMC 136}}</ref>
}}
'''R136''' (formerly known as '''RMC 136''' from the [[Radcliffe Observatory]] [[Magellanic Clouds]] catalogue<ref name=rmc>{{cite journal|bibcode=1960MNRAS.121..337F|title=The brightest stars in the Magellanic Clouds|journal=Monthly Notices of the Royal Astronomical Society|volume=121|issue=4|pages=337|last1=Feast|first1=M. W.|last2=Thackeray|first2=A. D.|last3=Wesselink|first3=A. J.|date=1960|doi=10.1093/mnras/121.4.337|doi-access=free}}</ref>) is the central concentration of stars in the [[NGC 2070]] star cluster, which lies at the centre of the [[Tarantula Nebula]] in the [[Large Magellanic Cloud]].  When originally named it was an unresolved stellar object (catalogued as HD 38268 and Wolf-Rayet star Brey 82) but is now known to include 72 class O and [[Wolf–Rayet star]]s within 5 [[parsec]]s (20 arc seconds) of the centre of the cluster.<ref name=census>{{Cite journal|arxiv=1308.3412 |last1= Doran |first1= E. I. |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 |pages= A134 |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=  Grafener |first9= G. |last10=  Herrero |first10= A. |last11=  Kohler |first11= K. |last12=  Maiz Apellaniz |first12= J. |last13=  Najarro |first13= F. |last14=  Puls |first14= J. |last15=  Sana |first15= H. |last16=  Schneider |first16= F. R. N. |last17=  Taylor |first17= W. D. |last18=  van Loon |first18= J. Th. |last19=  Vink |first19= J. S. |date= 2013 |doi= 10.1051/0004-6361/201321824 |bibcode = 2013A&A...558A.134D |s2cid= 118510909 }}</ref>  The extreme number and concentration of young massive stars in this part of the LMC qualifies it as a [[starburst region]].<ref name=brandl>{{Cite journal | doi = 10.1086/177507| title = Adaptive Optics Near-Infrared Imaging of R136 in 30 Doradus: The Stellar Population of a Nearby Starburst| journal = The Astrophysical Journal| volume = 466| pages = 254| year = 1996| last1 = Brandl | first1 = B.| last2 = Sams | first2 = B. J.| last3 = Bertoldi | first3 = F.| last4 = Eckart | first4 = A.| last5 = Genzel | first5 = R.| last6 = Drapatz | first6 = S.| last7 = Hofmann | first7 = R.| last8 = Loewe | first8 = M.| last9 = Quirrenbach | first9 = A.
| bibcode = 1996ApJ...466..254B}}</ref>

==Properties==
R136 produces most of the energy that makes the Tarantula Nebula visible. The estimated mass of the cluster is 450,000 solar masses, suggesting it may become a [[globular cluster]] in the future.<ref>{{cite journal | last=Bosch | first=Guillermo |author2=Terlevich, Elena|author2-link=Elena Terlevich |author3=Terlevich, Roberto | title=Gemini/GMOS Search for Massive Binaries in the Ionizing Cluster of 30 Dor | journal=Astronomical Journal | volume=137 |issue=2 | pages=3437–3441 | date=2009 | bibcode=2009AJ....137.3437B | doi=10.1088/0004-6256/137/2/3437|arxiv = 0811.4748 | s2cid=17976455 }}</ref>  R136 has around 200 times the stellar density of a typical OB association such as [[Cygnus OB2]].<ref name=massey/>  The central R136 concentration of the cluster is about 2 parsecs across, although the whole NGC 2070 cluster is much larger.<ref name=massey>{{Cite journal | doi = 10.1086/305126| title = Star Formation in R136: A Cluster of O3 Stars Revealed by ''Hubble'' Space Telescope ''Spectroscopy''| journal = The Astrophysical Journal| volume = 493| issue = 1| pages = 180| year = 1998| last1 = Massey | first1 = P. | last2 = Hunter | first2 = D. A. | bibcode = 1998ApJ...493..180M| doi-access = free}}</ref>

R136 is thought to be less than 2 million years old.<ref name=massey/><ref name=crowther>{{Cite journal |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 |arxiv=1007.3284 |bibcode=2010MNRAS.408..731C |doi=10.1111/j.1365-2966.2010.17167.x  |doi-access=free |s2cid=53001712 }}</ref>  None of the member stars are significantly evolved, and none are thought to have exploded as supernova. Because of this, the cluster contains no red supergiants, blue hypergiants, or luminous blue variables. The brightest stars are WNh, O supergiants, and OIf/WN [[slash star]]s, all extremely massive fully convective stars. A small number of B-type main sequence stars have been detected in the outskirts of the cluster, but less massive and less luminous stars cannot be resolved from the dense cluster core at the large distance of the LMC.<ref name=census/>

===R136a===
R136a is the bright knot at the centre of R136.  It consists of eight extremely massive stars, three of them [[Wolf-Rayet stars]] and the rest early O-class stars.<ref name=crowther2016>{{cite journal|bibcode=2016MNRAS.458..624C|arxiv=1603.04994|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|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.|author11-link=Selma de Mink|last12=Evans|first12=C. J.|last13=Gräfener|first13=G.|last14=Herrero|first14=A.|last15=Howarth|first15=I. D.|last16=Langer|first16=N.|last17=Lennon|first17=D. J.|last18=Puls|first18=J.|last19=Sana|first19=H.|last20=Vink|first20=J. S.|year=2016|doi=10.1093/mnras/stw273|doi-access=free }}</ref>

==Components==
The cluster contains many of the most massive and luminous stars known, including [[R136a1]]. Within the central 5 parsecs there are 32 of the hottest type&nbsp;O stars (O2.0–3.5), 40&nbsp;other O&nbsp;stars, and 12&nbsp;Wolf-Rayet stars, mostly of the extremely luminous WNh&nbsp;type. Within 150&nbsp;parsecs there are a further {{nobr|325 O stars}} and 19 Wolf-Rayet stars.<ref name=census/> Several [[runaway star]]s have been associated with R136, including [[VFTS 682]].<ref name=banerjee>{{cite journal |last1 = Banerjee |first1 = S. |last2 = Kroupa |first2 = P. |last3 = Oh |first3 = S. |year = 2012 |title = Runaway massive stars from R136: Vfts 682 is very likely a "slow runaway" |journal = [[The Astrophysical Journal]] |volume = 746 |issue = 1 |page = 15 |doi = 10.1088/0004-637X/746/1/15 |bibcode = 2012ApJ...746...15B |arxiv = 1111.0291 |s2cid = 117959362}}</ref>
R136 was first resolved into three components R136a, [[R136b]], and [[R136c]]. R136a was resolved using [[speckle interferometry]] and eventually space-based observations into as many as 24&nbsp;components,<ref name=campbell>{{cite journal | last1 = Campbell | first1 = B. | last2 = Hunter | first2 = D.A. | last3 = Holtzman | first3 = J.A. | last4 = Lauer | first4 = T.R. | last5 = Shayer | first5 = E.J. | last6 = Code | first6 = A. | last7 = Faber | first7 = S.M. | last8 = Groth | first8 = E.J. | last9 = Light | first9 = R.M. | last10 = Lynds | first10 = R. | last11 = O'Neil | first11 = ((E.J., Jr.)) | last12 = Westphal | first12 = J.A. | display-authors = 6 | date = November 1992 | title = Hubble Space Telescope Planetary Camera images of R136 | journal = The Astronomical Journal | volume = 104 | number=5 | pages = 1721–1742 | bibcode = 1992AJ....104.1721C | doi=10.1086/116355 | doi-access=free | url = https://authors.library.caltech.edu/52364/1/1992AJ____104_1721C.pdf }}</ref> dominated by R136a1, R136a2, and R136a3, all three being extremely massive WNh stars several million times more luminous than the sun.<ref name=Brands2022>{{Cite journal |last1=Brands |first1=S. |last2=de Koter |first2=A. |last3=Bestenlehner |first3=J. |last4=Crowther |first4=P. O|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. |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. |date=7 April 2022 |title=The R136 star cluster dissected with Hubble Space Telescope/STIS. III. The most massive stars and their clumped winds |url=https://www.aanda.org/10.1051/0004-6361/202142742 |journal=Astronomy & Astrophysics |volume=663 |pages=A36 |arxiv=2202.11080 |bibcode=2022A&A...663A..36B |doi=10.1051/0004-6361/202142742 |issn=0004-6361|s2cid=247025548}}</ref>

{| class="wikitable sortable"
|+Basic data for the original RMC 136 a, b, and c stars
! Name
! [[Right ascension]]<ref name=census/>
! [[Declination]]<ref name=census/>
! [[Apparent magnitude|V]]<ref name=crowther2016/> (F555W)
! [[Spectral type]]<ref name=Brands2022/>
! M<sub>V</sub><ref name=bestenlehner2020>{{cite journal |bibcode=2020MNRAS.499.1918B |title=The R136 star cluster dissected with Hubble Space Telescope/STIS. II. Physical properties of the most massive stars in R136 |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. |last12=Maíz Apellániz |first12=Jesus |last13=Puls |first13=Joachim |last14=Vink |first14=Jorick S. |journal=Monthly Notices of the Royal Astronomical Society |year=2020 |volume=499 |issue=2 |page=1918 |doi=10.1093/mnras/staa2801 |doi-access=free |arxiv=2009.05136 }}</ref> (F555W)
! Temperature ([[Kelvin|K]])<ref name=Brands2022/><ref name="Kalari 2022-07-26">{{cite journal |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 |date=26 July 2022 |title=Resolving the core of R136 in the optical |journal=The Astrophysical Journal |volume=935 |issue=2 |page=162 |doi=10.3847/1538-4357/ac8424 |arxiv=2207.13078 |bibcode=2022ApJ...935..162K |s2cid=251067072 |doi-access=free }}</ref>
! Luminosity ({{Solar luminosity}}){{r|Brands2022|Kalari 2022-07-26}}
! Mass ({{Solar mass}}){{r|Brands2022|Kalari 2022-07-26}}
|-
| [[R136a1]] || {{nowrap|{{RA|05|38|42.39}}}} || {{nowrap|{{DEC|−69|06|02.91}}}} || style="text-align:right"|12.28 || WN5h || style="text-align:right"|−8.18 || style="text-align:right"|46,000 || style="text-align:right"|4,677,000 || style="text-align:right" |196
|-
| [[R136a2]] || {{nowrap|{{RA|05|38|42.40}}}} || {{nowrap|{{DEC|−69|06|02.88}}}} || style="text-align:right"|12.80 || WN5h || style="text-align:right"|−7.80 || style="text-align:right"|50,000 || style="text-align:right" |3,548,000 || style="text-align:right" |151
|-
| [[R136a3]] || {{nowrap|{{RA|05|38|42.33}}}} || {{nowrap|{{DEC|−69|06|03.27}}}} || style="text-align:right"|12.97 || WN5h || style="text-align:right"|−7.52 || style="text-align:right"|50,000 || style="text-align:right"|3,631,000 || style="text-align:right" |155
|-
| R136a4 || {{nowrap|{{RA|05|38|42.34}}}} || {{nowrap|{{DEC|−69|06|02.60}}}} || style="text-align:right"|13.96 || O3 V((f*))(n) || style="text-align:right"|−6.68 || style="text-align:right"|50,000 || style="text-align:right" |1,905,000 || style="text-align:right" |108
|-
| R136a5 || {{nowrap|{{RA|05|38|42.43}}}} || {{nowrap|{{DEC|−69|06|02.73}}}} || style="text-align:right"|13.71 || O2I(n)f<sup>*</sup> || style="text-align:right"|−6.86 || style="text-align:right"|48,000 || style="text-align:right" |2,089,000 || style="text-align:right" |116
|-
| R136a6 || {{nowrap|{{RA|05|38|42.29}}}} || {{nowrap|{{DEC|−69|06|03.37}}}} || style="text-align:right"|13.35 || O2I(n)f<sup>*</sup>p || style="text-align:right"|−6.46 || style="text-align:right"|52,000 || style="text-align:right" |1,738,000 || style="text-align:right" |105
|-
| R136a7 || {{nowrap|{{RA|05|38|42.41}}}} || {{nowrap|{{DEC|−69|06|02.57}}}} || style="text-align:right"|13.97 || O3III(f<sup>*</sup>) || style="text-align:right"|−6.59 || style="text-align:right"|54,000 || style="text-align:right" |2,291,000 || style="text-align:right" |127
|-
| R136a8 || {{nowrap|{{RA|05|38|42.37}}}} || {{nowrap|{{DEC|−69|06|01.9}}?}} || style="text-align:right"|14.42 || O2–3V<ref name=crowther2016/> || style="text-align:right"|−6.05<ref name=crowther2016/> || style="text-align:right"|49,500 || style="text-align:right" |1,479,000 || style="text-align:right" |96
|-
| [[R136b]] || {{nowrap|{{RA|05|38|42.74}}}} || {{nowrap|{{DEC|−69|06|03.78}}}} || style="text-align:right"|13.24 || O4If || style="text-align:right"|−7.70 || style="text-align:right"|35,500 || style="text-align:right" |2,239,000 || style="text-align:right" |92
|-
| [[R136c]] || {{nowrap|{{RA|05|38|42.90}}}} || {{nowrap|{{DEC|−69|06|04.83}}}} || style="text-align:right"|12.86 || WN5h<ref name="schneider2018" />|| style="text-align:right" |−7.9<ref name=census/> || style="text-align:right"|42,170<ref name="schneider2018" />|| style="text-align:right" |3,802,000<ref name="schneider2018" />|| style="text-align:right" |142<ref name=schneider2018>{{cite journal |title=An excess of massive stars in the local 30 Doradus starburst |year=2018 |bibcode=2018Sci...359...69S |arxiv=1801.03107 |doi=10.1126/science.aan0106 |journal=Science |volume=359 |issue=6371 |pages=69–71 |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. |last12=Tramper |first12=F. |last13=Crowther |first13=P. A. |last14=de Koter |first14=A. |last15=de Mink |first15=S. E. |last16=Dufton |first16=P. L. |last17=Garcia |first17=M. |last18=Gieles |first18=M. |last19=Hénault-Brunet |first19=V. |last20=Herrero |first20=A. |last21=Izzard |first21= R. G. |last22=Kalari |first22= V. |last23=Lennon |first23= D. J. |last24=Maíz Apellániz |first24= J. |last25=Markova |first25= N. |last26=Najarro |first26= F. |last27=Podsiadlowski |first27= Ph. |last28=Puls |first28= J. |last29=Taylor |first29= W. D. |last30=van Loon |first30= J. Th. |last31=Vink |first31= J. S. |last32=Norman |first32= C. |pmid=29302009 |s2cid=206658504 }}</ref>
|-
|}

==Gallery==
<gallery>
R136 observed with WFC3.jpg|R136 observed with Hubble's WFC3<ref>{{cite web|title=R136 observed with WFC3 |url=https://esahubble.org/images/heic1605a/ |last1=NASA |last2=ESA |last3=Crowther |first3=P. |website=ESA/Hubble |date=17 March 2016 |access-date=23 March 2016}}</ref>
Runaway star speeding from 30 Doradus.jpg|Runaway star speeding from 30 Doradus in an image taken by the Hubble Space Telescope
Grand star-forming region R136 in NGC 2070 (infrared, captured by the Hubble Space Telescope).jpg|R136 in infrared (Hubble Space Telescope)
</gallery>

==See also==
{{wikinews|Astronomers discover largest star on record}}
* [[Hodge 301]], an older massive star cluster in Tarantula Nebula
* [[NGC 2060]], a smaller open cluster near R136
* [[LMC N79]], containing another super star cluster in the Large Magellanic Cloud
* [[List of most massive stars]]
{{clear}}

==References==
{{reflist}}

==Further reading==
* ESA Hubble, [http://www.spacetelescope.org/news/html/heic0416.html Symphony of colours in the Tarantula], 15 December 2004
* {{Cite journal
 | bibcode = 1997A&A...320..500C
 | title = Fundamental parameters of Wolf-Rayet stars / VI. Large Magellanic Cloud WNL stars
 | date = 1997
 | journal = Astronomy and Astrophysics
 | volume = 320
 | pages = 500–524
 | first = P.A.
 | last = Crowther
 |author2=L.J. Smith
 }}
* [http://aladin.u-strasbg.fr/AladinPreview?-c=SNR+B0538-69.1&ident=SNR+B0538-69.1&submit=Aladin+previewer R 136 in the Aladin previewer]

==External links==
* SIMBAD [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=RMC%20136 RMC 136]
* NED [http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=RMC+136&extend=no&hconst=73&omegam=0.27&omegav=0.73&corr_z=1&out_csys=Equatorial&out_equinox=J2000.0&obj_sort=RA+or+Longitude&of=pre_text&zv_breaker=30000.0&list_limit=5&img_stamp=YES RMC 136]

{{Dorado}}

{{DEFAULTSORT:R136}}
[[Category:Super star clusters]]
[[Category:Open clusters]]
[[Category:Tarantula Nebula]]
[[Category:Henry Draper Catalogue objects|038268]]
[[Category:Astronomical objects discovered in 1920|?]]
[[Category:Large Magellanic Cloud]]
[[Category:Star-forming regions]]
[[Category:Durchmusterung objects]]
[[Category:Dorado]]