Westerlund 1 W26

Image:Westerlund 1.jpg in infrared from 2MASS]]

Westerlund 1 was discovered by Bengt Westerlund in 1961 during an infrared survey in the Zone of Avoidance of the sky, and described as "a heavily reddened cluster in Ara". The spectral types of the component stars could not be determined at the time except for the brightest star which was tentatively considered type M.{{cite journal|doi=10.1086/127618|title=A Heavily Reddened Cluster in ARA|journal=Publications of the Astronomical Society of the Pacific|volume=73|issue=430|pages=51|year=1961|last1=Westerlund|first1=Bengt|bibcode=1961PASP...73...51W|s2cid=119636689 }}{{cite journal|bibcode=1987A&AS...70..311W|title=Photometry and spectroscopy of stars in the region of a highly reddened cluster in ARA|journal=Astronomy and Astrophysics Supplement Series |issn=0365-0138|volume=70|pages=311|last1=Westerlund|first1=B. E.|year=1987}}

In 1969, Borgman, Kornneef, and Slingerland conducted a photometric survey of the cluster and assigned letters to the stars they measured. This star, identified as a strong radio source, was given the letter "A".{{cite journal|bibcode=1970A&A.....4..248B|title=Infra-red photometry of a heavily reddened cluster in Ara|journal=Astronomy and Astrophysics|volume=4|pages=248|last1=Borgman|first1=J.|author-link1=Jan Borgman|last2=Koornneef|first2=J.|last3=Slingerland|first3=J.|year=1970}} This leads to the designation Westerlund-1 BKS A as used by Simbad, although the cluster was not known as Westerlund 1 at that time. At the time it was referred to as Ara A, with another strong radio source in the cluster called Ara C. Its brightness in the radio spectrum makes it one of the rare "radio stars". Westerlund made spectroscopic observations of the cluster, still not known as Westerlund 1, published in 1987 and numbered the stars, giving the number 26 and the spectral type M2I. Westerlund also discovered another notable red supergiant, WOH G64, found in the Large Magellanic Cloud in the constellation Dorado.

Modern terminology stems from 1998 when the cluster was referred to as Westerlund 1 (Wd1), with a paper describing Ara A as star 26 and Ara C as star 9.{{cite journal|doi=10.1046/j.1365-8711.1998.02038.x|title=Discovery of extended radio emission in the young cluster Wd1|journal=Monthly Notices of the Royal Astronomical Society|volume=299|issue=4|pages=L43|year=1998|last1=Clark|first1=J. S.|last2=Fender|first2=R. P.|last3=Waters|first3=L. B. F. M.|last4=Dougherty|first4=S. M.|last5=Korrnneef|first5=J.|last6=Steele|first6=I. A.|last7=Van Blokland|first7=A.|doi-access=free |bibcode=1998MNRAS.299L..43C|arxiv = astro-ph/9807303 |s2cid=16663149}}

Image:Comparison of Radii of RSGs located in the Westerlund 1 star cluster.png star cluster.]]

W26 is classified as a luminous cool supergiant. It occupies the upper right corner of the Hertzsprung–Russell diagram. The cool temperature means it emits a significant part of its energy in the infrared spectrum. It also shows huge mass loss of atmospheric material, suggesting that it may further evolve into a hotter supergiant. W26 has been observed to change its spectral class (and thus its temperature) during several periods, but it has not been seen to change its luminosity.

The star is almost obscured at visible wavelengths by extinction of around 13 magnitudes due to interstellar dust, hence it has been studied extensively in the longer infrared to radio wavelengths, which made it easier to study. Its spectral type identifies it a red star with a high luminosity. The bolometric luminosity of W26 has been calculated from its K-band infrared brightness to be 380,000 or 320,000 times higher than the sun's ({{solar luminosity|link=y}}), depending on the spectral type between M2 and M5. These luminosities imply a radius 1,530 or 1,580 times the Sun's radius ({{solar radius|link=y}}) based on assumed effective temperatures of 3,660 or 3,450 K for spectral types M2 and M5 respectively. These parameters make W26 one of the most luminous red supergiants and are similar to those estimated for another notable red supergiant star, VY Canis Majoris.

An earlier calculation of the luminosity and the temperature by fitting the spectral energy distribution and based on the spectrum by using DUSTY model gave a far higher luminosity near {{solar luminosity|1,100,000}}, considerably more luminous than expected for a red supergiant. The model also gave a photospheric temperature of {{val|3,700|fmt=commas|u=K}}, corresponding to a radius of {{solar radius|2,519}}, leading to a volume 16 billion times bigger than the Sun.{{cite journal|bibcode=2012ApJ...760...65F|arxiv=1209.6427|title=Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters|journal=The Astrophysical Journal|volume=760|issue=1|pages=65|last1=Fok|first1=Thomas K. T.|last2=Nakashima|first2=Jun-Ichi|last3=Yung|first3=Bosco H. K.|last4=Hsia|first4=Chih-Hao|last5=Deguchi|first5=Shuji|year=2012|doi=10.1088/0004-637X/760/1/65|s2cid=53393926}}{{efn | name=radius2 | Applying the Stefan-Boltzmann Law with a nominal solar effective temperature of 5,772 K: $\backslash sqrt\{(5,772/3,700)^4\; *\; 10^\{6.03\}\}\; =\; 2,519.12\backslash \; R\backslash odot$}}

In October 2013, astronomers using the European Southern Observatory's Very Large Survey Telescope (VST) discovered that W26 is surrounded by a glowing cloud of ionized hydrogen. This is the first ionized nebula to have been discovered around a red supergiant star through its optical emission lines, and follows the discovery of an ionized nebula around NML Cyg in 1982.{{cite journal|bibcode=1983ApJ...267..179M|title=The nature of NML Cygnus|journal=Astrophysical Journal|volume=267|pages=179|last1=Morris|first1=M.|last2=Jura|first2=M.|year=1983|doi=10.1086/160856|doi-access=free}}{{cite journal|bibcode=1982A&A...108..412H|title=An H II region near NML Cygnus|journal=Astronomy and Astrophysics|volume=108|pages=412|last1=Habing|first1=H. J.|last2=Goss|first2=W. M.|last3=Winnberg|first3=A.|year=1982}} The nebula extends 1.30 parsecs from the star.{{citation needed|date=October 2018}} The nebulae of both Westerlund 1 W20 and W26 are extended outward from the cluster core and most bright at inward direction, indicating the outward cluster wind.{{citation|arxiv=1803.07008|year=2018|title=Asymmetric ejecta of cool supergiants and hypergiants in the massive cluster Westerlund 1|doi=10.1093/mnrasl/sly046|last1=Andrews|first1=H.|last2=Fenech|first2=D.|last3=Prinja|first3=R. K.|last4=Clark|first4=J. S.|last5=Hindson|first5=L.|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=477|issue=1 |pages=L55–L59|doi-access=free |bibcode=2018MNRAS.477L..55A }} A later study analyzed the ejecta surrounding some of Westerlund 1's stars; the study determined the mass of W26's ejecta to be {{solar mass|{{val|403|e=-3}}}}, with an uncertainty of ± {{solar mass|{{val|94|e=-3}}}}.{{cite journal |last1=Andrews |first1=H |title=Asymmetric ejecta of cool supergiants and hypergiants in the massive cluster Westerlund 1 |journal=Monthly Notices of the Royal Astronomical Society |date=June 2018 |volume=477 |issue=1 |pages=L55–L59 |doi=10.1093/mnrasl/sly046 |doi-access=free |arxiv=1803.07008 |bibcode=2018MNRAS.477L..55A }}

• Westerlund 1 W237
• Westerlund 1 W75

{{notelist}}

{{reflist|25em|refs=

{{cite journal|last1=Wright|first1=N. J.|last2=Wesson|first2=R.|last3=Drew|first3=J. E.|last4=Barentsen|first4=G.|last5=Barlow|first5=M. J.|last6=Walsh|first6=J. R.|last7=Zijlstra|first7=A.|last8=Drake|first8=J. J.|last9=Eisloffel|first9=J.|last10=Farnhill|first10=H. J.|title=The ionized nebula surrounding the red supergiant W26 in Westerlund 1|journal=Monthly Notices of the Royal Astronomical Society: Letters|date=16 October 2013|volume=437|issue=1|pages=L1–L5|doi=10.1093/mnrasl/slt127|doi-access=free |arxiv = 1309.4086 |bibcode = 2014MNRAS.437L...1W |s2cid=14889377}}

{{Cite journal

|last1=Levesque |first1=Emily M.

|last2=Massey |first2=Philip

|last3=Olsen |first3=K.A.G.

|last4=Plez |first4=Bertrand

|last5=Josselin |first5=Eric

|last6=Maeder |first6=Andre

|last7=Meynet |first7=Georges

|year=2005

|title=The effective temperature scale of galactic red supergiants: Cool, but not as cool as we thought

|journal=The Astrophysical Journal

|volume=628 |issue=2 |pages=973–985

|arxiv=astro-ph/0504337 |bibcode=2005ApJ...628..973L

|doi=10.1086/430901 |s2cid=15109583

}}

}}

• {{cite journal|arxiv=1508.07003|doi=10.1051/0004-6361/201526159|title=Cold gas in hot star clusters: The wind from the red supergiant W26 in Westerlund 1|journal=Astronomy & Astrophysics|volume=582|pages=A24|year=2015|last1=MacKey|first1=Jonathan|last2=Castro|first2=Norberto|last3=Fossati|first3=Luca|last4=Langer|first4=Norbert|bibcode=2015A&A...582A..24M|s2cid=54683876}}

{{Stars of Ara}}

{{DEFAULTSORT:Westerlund 1 W26}}

Category:Ara (constellation)

Category:Astronomical objects discovered in 1961

J16470540-4550367

Category:M-type supergiants