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==Characteristics==
==Characteristics==
The star is located 11,500 light-years from Earth and is almost obscured at visible wavelengths by [[Extinction (astronomy)|extinction]] of around 13 magnitudes due to [[interstellar dust]],<ref name=lim/> hence it has been studied extensively in the longer infrared to radio wavelengths. The star has a radius between {{solar radius|1,530 and 1,580|link=y}}.<!-- An earlier calculation of the radius gave a value of {{solar radius|2,000}}. This estimate is most likely of a guess than a measurement--><ref name=clark2011/> Its spectral type identifies it a red star with a high luminosity.<!-- At radio wavelengths it is 310,000 times brighter than the Sun,<ref name=dougherty>{{cite journal|bibcode=2010A&A...511A..58D|title=Radio emission from the massive stars in the galactic super star cluster Westerlund 1|journal=Astronomy and Astrophysics|volume=511|pages=A58|author1=Dougherty|first1=S. M.|last2=Clark|first2=J. S.|last3=Negueruela|first3=I.|last4=Johnson|first4=T.|last5=Chapman|first5=J. M.|year=2010|doi=10.1051/0004-6361/200913505|arxiv = 0912.4165 }}</ref> value not in the paper, presumably calculated in some way? --> Its [[bolometric luminosity]] has been calculated from its [[K band (infrared)|K-band infrared]] brightness to be between 320,000 and 380,000 times higher than the sun's.<ref name=wright/> An earlier calculation of the luminosity by fitting the [[spectral energy distribution]] gave a luminosity of just over {{solar luminosity|a million}}.<ref name=fok>{{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|pages=65|author1=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}}</ref>
The star is located 11,500 light-years from Earth and is almost obscured at visible wavelengths by [[Extinction (astronomy)|extinction]] of around 13 magnitudes due to [[interstellar dust]],<ref name=lim/> hence it has been studied extensively in the longer infrared to radio wavelengths. The star has a radius between {{solar radius|1,530 and 1,580|link=y}}.<!-- An earlier calculation of the radius gave a value of {{solar radius|2,000}}. This estimate is most likely of a guess than a measurement--><ref name=clark2011/> Another recent estimate gives the star a significantly higher radius of {{solar radius|2,550}}.<ref name=fok/> Its spectral type identifies it a red star with a high luminosity.<!-- At radio wavelengths it is 310,000 times brighter than the Sun,<ref name=dougherty>{{cite journal|bibcode=2010A&A...511A..58D|title=Radio emission from the massive stars in the galactic super star cluster Westerlund 1|journal=Astronomy and Astrophysics|volume=511|pages=A58|author1=Dougherty|first1=S. M.|last2=Clark|first2=J. S.|last3=Negueruela|first3=I.|last4=Johnson|first4=T.|last5=Chapman|first5=J. M.|year=2010|doi=10.1051/0004-6361/200913505|arxiv = 0912.4165 }}</ref> value not in the paper, presumably calculated in some way? --> Its [[bolometric luminosity]] has been calculated from its [[K band (infrared)|K-band infrared]] brightness to be between 320,000 and 380,000 times higher than the sun's.<ref name=wright/> An earlier calculation of the luminosity by fitting the [[spectral energy distribution]] gave a luminosity of just over {{solar luminosity|a million}}.<ref name=fok>{{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|pages=65|author1=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}}</ref>


Westerlund 1-26 is classified as a luminous supergiant. With its surface temperature of about 3,600 [[Kelvin|K]], it occupies the upper right corner of the [[Hertzsprung–Russell diagram]]. The cool temperature means it emits most 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. Westerlund 1-26 has been observed to change its [[spectral class]] during several periods, but it has not been seen to change its luminosity.<ref name=wright/>
Westerlund 1-26 is classified as a luminous supergiant. With its surface temperature of about 3,600 [[Kelvin|K]], it occupies the upper right corner of the [[Hertzsprung–Russell diagram]]. The cool temperature means it emits most 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. Westerlund 1-26 has been observed to change its [[spectral class]] during several periods, but it has not been seen to change its luminosity.<ref name=wright/>
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==See also==
==See also==
⚫
*[[VY Canis Majoris]]
*[[NML Cygni]]
*[[NML Cygni]]
*[[UY Scuti]]
*[[UY Scuti]]
⚫
*[[VY Canis Majoris]]
*[[WOH G64]]
*[[WOH G64]]


Revision as of 08:03, 9 September 2018

Westerlund 1-26

Westerlund 1 with the inset showing W1-26 and the associated ionised hydrogen cloud
Credit: ESO
Observation data
Epoch J2000      Equinox J2000
Constellation Ara
Right ascension 16h 47m 05.403s[1]
Declination −45° 50′ 36.76″[1]
Apparent magnitude (V) 17.194[2]
Characteristics
Spectral type M2-M6Ia[3]
Apparent magnitude (B) 22.1[4]
Apparent magnitude (J) 4.31[1]
Apparent magnitude (H) 1.35[1]
Apparent magnitude (K) 1.9[5]
U−B color index −7.445[2]
B−V color index +5.000[2]
Astrometry
Distance11,500 ly
(3,550[6] pc)
Details
Radius1,530 - 1,580[6], ~2,550[7][a]  R☉
Luminosity320,000 - 380,000[6], 1,100,000[7] L☉
Temperature3,600[8]–3,700[7] K
Age3.5-5.0[4] Myr
Other designations
Westerlund 1 W26, 2MASS J16470540-4550367, Westerlund 1 BKS AS, Westerlund 1 BKS A
Database references
SIMBADdata

Westerlund 1-26 or Wd 1-26 is a red supergiant or hypergiant within the outskirts of the Westerlund 1 super star cluster. It is one of the largest known stars discovered so far, with a radius between 1,530–2,550 solar radii (1.06×109–1.77×109 km; 7.1–11.9 au), corresponding to a volume between 3.6–16.6 billion times bigger than the Sun. Assuming the upper estimate is correct, if placed at the center of the Solar System, its photosphere would engulf the orbit of Saturn.

Discovery

Westerlund 1 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.[9][10]

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".[11] This leads to the designation Westerlund-1 BKS A used at 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.[10]

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.[12]

Characteristics

The star is located 11,500 light-years from Earth and is almost obscured at visible wavelengths by extinction of around 13 magnitudes due to interstellar dust,[2] hence it has been studied extensively in the longer infrared to radio wavelengths. The star has a radius between 1,530 and 1,580 R☉.[3] Another recent estimate gives the star a significantly higher radius of 2,550 R☉.[7] Its spectral type identifies it a red star with a high luminosity. Its bolometric luminosity has been calculated from its K-band infrared brightness to be between 320,000 and 380,000 times higher than the sun's.[6] An earlier calculation of the luminosity by fitting the spectral energy distribution gave a luminosity of just over a million L☉.[7]

Westerlund 1-26 is classified as a luminous supergiant. With its surface temperature of about 3,600 K, it occupies the upper right corner of the Hertzsprung–Russell diagram. The cool temperature means it emits most 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. Westerlund 1-26 has been observed to change its spectral class during several periods, but it has not been seen to change its luminosity.[6]

In October 2013, astronomers using the European Southern Observatory's Very Large Survey Telescope (VST) discovered that Westerlund 1-26 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.[13][14] The nebula extends 1.30 parsecs from the star.

See also

References

  1. ^ a b c d Cutri, R. M.; Skrutskie, M. F.; Van Dyk, S.; Beichman, C. A.; Carpenter, J. M.; Chester, T.; Cambresy, L.; Evans, T.; Fowler, J.; Gizis, J.; Howard, E.; Huchra, J.; Jarrett, T.; Kopan, E. L.; Kirkpatrick, J. D.; Light, R. M.; Marsh, K. A.; McCallon, H.; Schneider, S.; Stiening, R.; Sykes, M.; Weinberg, M.; Wheaton, W. A.; Wheelock, S.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". VizieR On-line Data Catalog: II/246. Originally published in: 2003yCat.2246....0C. 2246: 0. Bibcode:2003yCat.2246....0C.
  2. ^ a b c d Lim, Beomdu; Chun, Moo-Young; Sung, Hwankyung; Park, Byeong-Gon; Lee, Jae-Joon; Sohn, Sangmo T.; Hur, Hyeonoh; Bessell, Michael S. (2013). "The Starburst Cluster Westerlund 1: The Initial Mass Function and Mass Segregation". The Astronomical Journal. 145 (2): 46. arXiv:1211.5832. Bibcode:2013AJ....145...46L. doi:10.1088/0004-6256/145/2/46.
  3. ^ a b Clark, J. S.; Ritchie, B. W.; Negueruela, I.; Crowther, P. A.; Damineli, A.; Jablonski, F. J.; Langer, N. (2011). "A VLT/FLAMES survey for massive binaries in Westerlund 1". Astronomy & Astrophysics. 531: A28. arXiv:1105.0776. Bibcode:2011A&A...531A..28C. doi:10.1051/0004-6361/201116990.
  4. ^ a b Clark, J. S.; Negueruela, I.; Crowther, P. A.; Goodwin, S. P. (2005). "On the massive stellar population of the super star cluster Westerlund 1". Astronomy and Astrophysics. 434 (3): 949. arXiv:astro-ph/0504342. Bibcode:2005A&A...434..949C. doi:10.1051/0004-6361:20042413.
  5. ^ Piatti, A. E.; Bica, E.; Claria, J. J. (1998). "Fundamental parameters of the highly reddened young open clusters Westerlund 1 and 2". Astronomy and Astrophysics Supplement. 127 (3): 423. Bibcode:1998A&AS..127..423P. doi:10.1051/aas:1998111.
  6. ^ a b c d e Wright, N. J.; Wesson, R.; Drew, J. E.; Barentsen, G.; Barlow, M. J.; Walsh, J. R.; Zijlstra, A.; Drake, J. J.; Eisloffel, J.; Farnhill, H. J. (16 October 2013). "The ionized nebula surrounding the red supergiant W26 in Westerlund 1". Monthly Notices of the Royal Astronomical Society: Letters. 437 (1): L1 – L5. arXiv:1309.4086. Bibcode:2014MNRAS.437L...1W. doi:10.1093/mnrasl/slt127.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  7. ^ a b c d e Fok, Thomas K. T.; Nakashima, Jun-Ichi; Yung, Bosco H. K.; Hsia, Chih-Hao; Deguchi, Shuji (2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". The Astrophysical Journal. 760: 65. arXiv:1209.6427. Bibcode:2012ApJ...760...65F. doi:10.1088/0004-637X/760/1/65.
  8. ^ MacKey, Jonathan; Castro, Norberto; Fossati, Luca; Langer, Norbert (2015). "Cold gas in hot star clusters: The wind from the red supergiant W26 in Westerlund 1". Astronomy & Astrophysics. 582: A24. arXiv:1508.07003. Bibcode:2015A&A...582A..24M. doi:10.1051/0004-6361/201526159.
  9. ^ Westerlund, Bengt (1961). "A Heavily Reddened Cluster in ARA". Publications of the Astronomical Society of the Pacific. 73: 51. Bibcode:1961PASP...73...51W. doi:10.1086/127618.
  10. ^ a b Westerlund, B. E. (1987). "Photometry and spectroscopy of stars in the region of a highly reddened cluster in ARA". Astronomy and Astrophysics Supplement Series. 70: 311. Bibcode:1987A&AS...70..311W. ISSN 0365-0138.
  11. ^ Borgman, J.; Koornneef, J.; Slingerland, J. (1970). "Infra-red photometry of a heavily reddened cluster in Ara". Astronomy and Astrophysics. 4: 248. Bibcode:1970A&A.....4..248B.
  12. ^ Clark, J. S.; Fender, R. P.; Waters, L. B. F. M.; Dougherty, S. M.; Korrnneef, J.; Steele, I. A.; Van Blokland, A. (1998). "Discovery of extended radio emission in the young cluster Wd1". Monthly Notices of the Royal Astronomical Society. 299 (4): L43. arXiv:astro-ph/9807303. Bibcode:1998MNRAS.299L..43C. doi:10.1046/j.1365-8711.1998.02038.x.
  13. ^ Morris, M.; Jura, M. (1983). "The nature of NML Cygnus". Astrophysical Journal. 267: 179. Bibcode:1983ApJ...267..179M. doi:10.1086/160856.
  14. ^ Habing, H. J.; Goss, W. M.; Winnberg, A. (1982). "An H II region near NML Cygnus". Astronomy and Astrophysics. 108: 412. Bibcode:1982A&A...108..412H.

Notes

  1. ^ Applying the Stefan-Boltzmann Law with a nominal solar effective temperature of 5,772 K:

Template:Top 10 largest stars

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