Westerlund 1-26

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Westerlund 1-26
Surprise Cloud Around Vast Star-inset.png
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]
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]
Proper motion (μ) RA: −0.910±0.608[6] mas/yr
Dec.: −4.481±0.582[6] mas/yr
Parallax (π)0.6798 ± 0.2455[6] mas
Distance11,500 ly
(3,550[7] pc)
Radius1,530 - 1,580[7], ~2,550[8][a]  R
Luminosity320,000 - 380,000[7], 1,100,000[8] L
Temperature3,600[9]–3,700[8] 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

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.


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.[10][11]

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".[12] 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.[11]

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.[13]


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. 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, giving a radius between 1,530 and 1,580 R.[7] This makes Westerlund 1-26 one of most luminous red supergiants. An earlier calculation of the luminosity by fitting the spectral energy distribution gave a luminosity of just over a million L, which corresponds to a very large radius of 2,550 R and is considerably more luminous than expected for any red supergiant and extreme.[8]

Westerlund 1-26 is classified as a luminous cool supergiant. With its surface temperature of below 4,000 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 (and thus its temperature) during several periods, but it has not been seen to change its luminosity.[7]

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.[14][15] The nebula extends 1.30 parsecs from the star.

See also[edit]


  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:1211.5832Freely accessible. Bibcode:2013AJ....145...46L. doi:10.1088/0004-6256/145/2/46. 
  3. ^ 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:1105.0776Freely accessible. 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/0504342Freely accessible. 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 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365Freely accessible. Bibcode:2018A&A...616A...1GFreely accessible. doi:10.1051/0004-6361/201833051Freely accessible.  Gaia DR2 record for this source at VizieR.
  7. ^ 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:1309.4086Freely accessible. Bibcode:2014MNRAS.437L...1W. doi:10.1093/mnrasl/slt127. 
  8. ^ a b c d 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:1209.6427Freely accessible. Bibcode:2012ApJ...760...65F. doi:10.1088/0004-637X/760/1/65. 
  9. ^ 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:1508.07003Freely accessible. Bibcode:2015A&A...582A..24M. doi:10.1051/0004-6361/201526159. 
  10. ^ 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. 
  11. ^ 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. 
  12. ^ 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. 
  13. ^ 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/9807303Freely accessible. Bibcode:1998MNRAS.299L..43C. doi:10.1046/j.1365-8711.1998.02038.x. 
  14. ^ Morris, M.; Jura, M. (1983). "The nature of NML Cygnus". Astrophysical Journal. 267: 179. Bibcode:1983ApJ...267..179M. doi:10.1086/160856. 
  15. ^ 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. 


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