WOH S264

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WOH S264
W60 B90.png
DSS2 image of WOH S264, the star can be seen in the centre.
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Dorado (LMC)
Right ascension 05h 24m 19.3095s [1]
Declination −69° 38′ 49.374″ [1]
Apparent magnitude  (V)14.271 [2]
Characteristics
Evolutionary stage Red supergiant
Spectral type M3 I [3]
Apparent magnitude  (U)19.519 [4]
Apparent magnitude  (B)16.688 [4]
Apparent magnitude  (R)11 [4]
Apparent magnitude  (G)12.135779 [5]
Apparent magnitude  (I)10.804 [4]
Apparent magnitude  (J)8.36 [4]
Apparent magnitude  (H)7.375 [4]
Apparent magnitude  (K)6.809 [4]
Astrometry
Radial velocity (Rv)263.49±1.02 [6]  km/s
Parallax (π)0.0457 ± 0.027  mas [5]
Distance 45,590 [7]   pc
Details
Mass 24.9 [8]   M☉
Radius 1,390+130
−110 [3]   R☉
Luminosity 282,000+49,300
−42,000 [3]   L☉
Surface gravity (log g)+0.5±0.1 [3]   cgs
Temperature 3,570+59
−46 [3]   K
Other designations
WOH S264, LI-LMC 976, MSX LMC 461, RM 1-339, SP77 47-10 [1]
Database references
SIMBAD data

WOH S264 ([W60] B90) is a large, highly luminous [3] red supergiant star in the Large Magellanic Cloud.

Contents

Discovery

WOH S264 was discovered in 1956 by Karl Gordon Henize in a catalogue of H-alpha emission stars and nebulae in the Large Magellanic Cloud. He designated it LHA 120-N 132E, indicating emission line nebula 132E on plate 120. The LHA is originally LHα, standing for H-alpha emission objects identified at the Lamont-Hussey Observatory. [9]

The designation WOH S264 indicates that it is supergiant 264 in a 1981 survey by Westerlund, Olander, and Hedin. [10]

Properties

WOH S264 is believed to be one of the largest, most luminous red supergiants in the Large Magellanic Cloud with a luminosity of more than 280,000 solar luminosities and a radius of around 1,390 solar radii. [3] It needs further investigation to constrain the luminosity and radius with higher certainty. [3]

See also

Related Research Articles

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References

  1. 1 2 3 "[W60] B90". Université de Strasbourg.
  2. ↑ Ulaczyk, K.; Szymański, M. K.; Udalski, A.; Kubiak, M.; Pietrzyński, G.; Soszyński, I.; Wyrzykowski, Ł.; Poleski, R.; Gieren, W.; Walker, A. R.; Garcia-Varela, A. (20 June 2013). "Variable Stars from the OGLE-III Shallow Survey in the Large Magellanic Cloud". Acta Astronomica. 63 (2): 159–179. arXiv: 1306.4802 . Bibcode:2013AcA....63..159U.
  3. 1 2 3 4 5 6 7 8 de Wit, S.; Bonanos, A.Z.; Tramper, F.; Yang, M.; Maravelias, G.; Boutsia, K.; Britavskiy, N.; Zapartas, E. (2023). "Properties of luminous red supergiant stars in the Magellanic Clouds". Astronomy and Astrophysics. 669: 17. arXiv: 2209.11239 . Bibcode:2023A&A...669A..86D. doi:10.1051/0004-6361/202243394. S2CID   252519285.
  4. 1 2 3 4 5 6 7 Kamath, D.; Wood, P. R.; Van Winckel, H. (4 August 2015). "Optically visible post-AGB stars, post-RGB stars and young stellar objects in the Large Magellanic Cloud". The Royal Astronomical Society. 454 (2): 1468–1502. arXiv: 1508.00670 . Bibcode:2015MNRAS.454.1468K. doi:10.1093/mnras/stv1202.
  5. 1 2 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  6. ↑ Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  7. ↑ Pietrzyński, G.; Graczyk, D.; Gallenne, A.; Gieren, W.; Thompson, I. B.; Pilecki, B.; Karczmarek, P.; Górski, M.; Suchomska, K.; Taormina, M.; Zgirski, B.; Wielgórski, P.; Kołaczkowski, Z.; Konorski, P.; Villanova, S.; Nardetto, N.; Kervella, P.; Bresolin, F.; Kudritzki, R. P.; Storm, J.; Smolec, R.; Narloch, W. (2019). "A distance to the Large Magellanic Cloud that is precise to one per cent". Nature. 567 (7747): 200–203. arXiv: 1903.08096 . Bibcode:2019Natur.567..200P. doi:10.1038/s41586-019-0999-4. PMID   30867610. S2CID   76660316.
  8. ↑ Ren, Yi; Jiang, Bi-Wei (2020-07-20). "On the Granulation and Irregular Variation of Red Supergiants". The Astrophysical Journal. 898 (1): 24. arXiv: 2006.06605 . Bibcode:2020ApJ...898...24R. doi: 10.3847/1538-4357/ab9c17 . ISSN   1538-4357.
  9. ↑ Henize, Karl G. (1956-05-05). "Catalogues of Hα-emission Stars and Nebulae in the Magellanic Clouds". Astrophysical Journal. 2: 315. Bibcode:1956ApJS....2..315H. doi:10.1086/190025.
  10. ↑ Westerlund, B. E.; Olander, N.; Hedin, B. (1981). "Supergiant and giant M type stars in the Large Magellanic Cloud". Astronomy & Astrophysics Supplement Series. 43: 267–295. Bibcode:1981A&AS...43..267W.
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