WOH G64 (IRAS 04553-6825) is an unusual[3]red supergiant (RSG) star in the Large Magellanic Cloud (LMC) satellite galaxy in the southern constellation of Dorado. It is one of the largest known stars, being described as possibly being the largest star known.[3][12] It is also one of the most luminous and massive red supergiants, with a radius calculated to be around 1,540 times that of the Sun (R☉) and a luminosity around 282,000 times the solar luminosity (L☉).
WOH G64
Location of WOH G64 (circled) in the Large Magellanic Cloud Credit: NASA/JPL-Caltech/M. Meixner (STScI) & the SAGE Legacy Team
WOH G64 is surrounded by an optically thick dust envelope of roughly a light year in diameter containing 3 to 9 times the Sun's mass of expelled material that was created by the strong stellar wind.[13] If placed at the center of the Solar System, the star's photosphere would engulf the orbit of Jupiter.
WOH G64 was discovered in the 1970s by Bengt Westerlund, Olander and Hedin. Like NML Cygni, the "WOH" in the star's name comes from the names of its three discoverers, but in this case refers to a whole catalogue of giant and supergiant stars in the LMC.[14] Westerlund also discovered another notable red supergiant star, Westerlund 1-26, found in the massive super star clusterWesterlund 1 in the constellation Ara.[15] In 1986, infrared observations showed that it was a highly luminous supergiant surrounded by gas and dust which absorbed around three quarters of its radiation.[5]
In 2007, observers using the Very Large Telescope (VLT) showed that WOH G64 is surrounded by a torus-shaped cloud.[13]
Distance
The distance of WOH G64 is assumed to be around 50,000 parsecs (160,000 ly) away from Earth, since it appears to be in the LMC.[3] The Gaia Data Release 2 parallax for WOH G64 is −0.2280±0.0625 mas and the negative parallax does not provide a reliable distance.[1]
Variability
WOH G64 varies regularly in brightness by over a magnitude at visual wavelengths with a primary period of around 800 days.[7] The star suffers from over six magnitudes of extinction at visual wavelengths, and the variation at infra-red wavelengths is much smaller.[3] It has been described as a carbon-rich Mira or long-period variable, which would necessarily be an asymptotic-giant-branch star (AGB star) rather than a supergiant.[8] Brightness variability has been confirmed by other researchers in some spectral bands, but it is unclear what the actual variable type is. No significant spectral variation has been found.[3]
The spectral type of WOH G64 is given as M5,[3] but it is usually found to have a much cooler spectral type of M7.5, highly unusual for a supergiant star.[10][4][5]
WOH G64 is classified as an extremely luminous M class supergiant and is likely to be the largest star and the most luminous and coolest red supergiant in the LMC.[3] The combination of the star's temperature and luminosity places it toward the upper right corner of the Hertzsprung–Russell diagram. The star's evolved state means that it can no longer hold on to its atmosphere due to low density, high radiation pressure, and the relatively opaque products of thermonuclear fusion.[citation needed] It has an average mass loss rate of 3.1 to 5.8×10−4M☉ per year, among the highest known and unusually high even for a red supergiant.[9]
The parameters of WOH G64 are uncertain. The star was originally calculated to be around between 490,000 and 600,000 L☉ based on spectroscopic measurements assuming spherical shells, suggesting initial masses at least 40 M☉ and consequently larger values for the radius between 2,575 and 3,000 R☉.[16][4][17] 2007 measurements using the Very Large Telescope (VLT) gave the star a bolometric luminosity of 282,000+40,000 −30,000L☉, suggesting an initial mass of 25±5 M☉, and a radius around 1,730 R☉ based on the assumption of an effective temperature of 3,200 K and radiative transfer modelling of the surrounding torus.[13] In 2009, Levesque calculated an effective temperature of 3,400±25 K by spectral fitting of the optical and near-UV SED. Adopting the Ohnaka luminosity with this new temperature gives a radius of 1,540 R☉ but with a margin of error of 5% or 77 R☉.[3] Ignoring the effect of the dusty torus in redirecting infrared radiation, estimates of 1,970 - 1,990 R☉ based on a luminosity of 450,000+150,000 −120,000L☉ and an effective temperature of 3,372 - 3,400 K have also been derived.[3]
A 2018 paper gives a luminosity of 432,000 L☉ and a higher effective temperature of 3,500 K, based on optical and infrared photometry and assuming spherically-symmetric radiation from the surrounding dust. This suggests a radius of 1,788 R☉.[11][a]
Spectral features
WOH G64 was discovered to be a prominent source of OH, H 2O, and SiOmasers emission, which is typical of an OH/IR supergiant star.[3] It shows an unusual spectrum of nebular emission; the hot gas is rich in nitrogen and has a radial velocity considerably more positive than that of the star.[3] The stellar atmosphere is producing a strong silicate absorption band in mid-infrared wavelengths, accompanied a line emission due to highly excited carbon monoxide.[18]
Possible companion
WOH G64 has a possible late O-type dwarf companion of a bolometric magnitude of −7.5 or a luminosity of 100,000 L☉, which would make WOH G64 a binary star although there has been no confirmation of this observation and the intervening dust clouds makes the study of the star very difficult.[3]
^ abcdefgBrown, 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:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
^Bhardwaj, Anupam; Kanbur, Shashi; He, Shiyuan; Rejkuba, Marina; Matsunaga, Noriyuki; De Grijs, Richard; Sharma, Kaushal; Singh, Harinder P.; Baug, Tapas; Ngeow, Chow-Choong; Ou, Jia-Yu (2019). "Multiwavelength Period-Luminosity and Period-Luminosity-Color Relations at Maximum Light for Mira Variables in the Magellanic Clouds". The Astrophysical Journal. 884 (1): 20. arXiv:1908.01795. Bibcode:2019ApJ...884...20B. doi:10.3847/1538-4357/ab38c2. S2CID 199452754.
^ abcdefghijklmnopqrLevesque, E. M.; Massey, P.; Plez, B.; Olsen, K. A. G. (2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". The Astronomical Journal. 137 (6): 4744. arXiv:0903.2260. Bibcode:2009AJ....137.4744L. doi:10.1088/0004-6256/137/6/4744. S2CID 18074349.
^ abcdVan Loon, J. Th.; Cioni, M.-R. L.; Zijlstra, A. A.; Loup, C. (2005). "An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars". Astronomy and Astrophysics. 438 (1): 273–289. arXiv:astro-ph/0504379. Bibcode:2005A&A...438..273V. doi:10.1051/0004-6361:20042555. S2CID 16724272.
^ abcElias, J.H. (March 1986). "Two Supergiants in the Large Magellanic Cloud with Thick Dust Shells". Astrophysical Journal. 302: 675. Bibcode:1986ApJ...302..675E. doi:10.1086/164028. hdl:1887/6514.
^ abcCutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
^ abFraser, Oliver J.; Hawley, Suzanne L.; Cook, Kem H. (2008). "The Properties of Long-Period Variables in the Large Magellanic Cloud from MACHO". The Astronomical Journal. 136 (3): 1242–1258. arXiv:0808.1737. Bibcode:2008AJ....136.1242F. doi:10.1088/0004-6256/136/3/1242. S2CID 2754884.
^ abcSoszyñski, I.; Udalski, A.; Szymañski, M. K.; Kubiak, M.; Pietrzyñski, G.; Wyrzykowski, Ł.; Szewczyk, O.; Ulaczyk, K.; Poleski, R. (2009). "The Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. IV. Long-Period Variables in the Large Magellanic Cloud". Acta Astronomica. 59 (3): 239. arXiv:0910.1354. Bibcode:2009AcA....59..239S.
^ abcdSteven R. Goldman; Jacco Th. van Loon (2016). "The wind speeds, dust content, and mass-loss rates of evolved AGB and RSG stars at varying metallicity". Monthly Notices of the Royal Astronomical Society. 465 (1): 403–433. arXiv:1610.05761. Bibcode:2017MNRAS.465..403G. doi:10.1093/mnras/stw2708. S2CID 11352637.
^ abcDavies, Ben; Crowther, Paul A.; Beasor, Emma R. (2018). "The luminosities of cool supergiants in the Magellanic Clouds, and the Humphreys–Davidson limit revisited". Monthly Notices of the Royal Astronomical Society. 478 (3): 3138–3148. arXiv:1804.06417. Bibcode:2018MNRAS.478.3138D. doi:10.1093/mnras/sty1302. S2CID 59459492.
^ abGroenewegen, Martin A. T.; Sloan, Greg C. (2018). "Luminosities and mass-loss rates of Local Group AGB stars and Red Supergiants". Astronomy & Astrophysics. 609: A114. arXiv:1711.07803. Bibcode:2018A&A...609A.114G. doi:10.1051/0004-6361/201731089. ISSN 0004-6361. S2CID 59327105.
^Jones, Olivia; Woods, Paul; Kemper, Franziska; Kraemer, Elena; Sloan, G.; Srinivasan, Sivakrishnan; Oliveira, Joana; van Loon, Jacco; Boyer, Martha; Sargent, Benjamin; Mc Donald, I.; Meixner, Margaret; Zijlstra, A.; Ruffel, Paul; Lagadec, Eric; Pauly, Tyler (May 7, 2017). "The SAGE-Spec Spitzer Legacy program: the life-cycle of dust and gas in the Large Magellanic Cloud. Point source classification – III". Monthly Notices of the Royal Astronomical Society. 470 (3): 3250–3282. doi:10.1093/mnras/stx1101. Retrieved 23 June 2022.
^ abcdOhnaka, K.; Driebe, T.; Hofmann, K. H.; Weigelt, G.; Wittkowski, M. (2009). "Resolving the dusty torus and the mystery surrounding LMC red supergiant WOH G64". Proceedings of the International Astronomical Union. 4: 454–458. Bibcode:2009IAUS..256..454O. doi:10.1017/S1743921308028858.
^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.
^Westerlund, B. E. (1987). "Photometry and spectroscopy of stars in the region of a highly reddened cluster in ARA". Astronomy and Astrophysics. Supplement. 70 (3): 311–324. Bibcode:1987A&AS...70..311W. ISSN 0365-0138.
^Elias, J. H; Frogel, J. A; Schwering, P. B. W (1986). "Two Supergiants in the Large Magellanic Cloud with Thick Dust Shells". The Astrophysical Journal. 302: 675. Bibcode:1986ApJ...302..675E. doi:10.1086/164028. hdl:1887/6514.
^Monnier, J. D; Millan-Gabet, R; Tuthill, P. G; Traub, W. A; Carleton, N. P; Coudé Du Foresto, V; Danchi, W. C; Lacasse, M. G; Morel, S; Perrin, G; Porro, I. L; Schloerb, F. P; Townes, C. H (2004). "High-Resolution Imaging of Dust Shells by Using Keck Aperture Masking and the IOTA Interferometer". The Astrophysical Journal. 605 (1): 436–461. arXiv:astro-ph/0401363. Bibcode:2004ApJ...605..436M. doi:10.1086/382218. S2CID 7851916.
^The mass-loss rates of red supergiants at low metallicity: Detectionof rotational CO emission from two red supergiants in the LargeMagellanic Cloud
May 06, 2023
iras, 04553, 6825, unusual, supergiant, star, large, magellanic, cloud, satellite, galaxy, southern, constellation, dorado, largest, known, stars, being, described, possibly, being, largest, star, known, also, most, luminous, massive, supergiants, with, radius. WOH G64 IRAS 04553 6825 is an unusual 3 red supergiant RSG star in the Large Magellanic Cloud LMC satellite galaxy in the southern constellation of Dorado It is one of the largest known stars being described as possibly being the largest star known 3 12 It is also one of the most luminous and massive red supergiants with a radius calculated to be around 1 540 times that of the Sun R and a luminosity around 282 000 times the solar luminosity L WOH G64Location of WOH G64 circled in the Large Magellanic CloudCredit NASA JPL Caltech M Meixner STScI amp the SAGE Legacy TeamObservation dataEpoch J2000 0 Equinox J2000 0Constellation Dorado LMC Right ascension 04h 55m 10 5252s 1 Declination 68 20 29 998 1 Apparent magnitude V 17 7 18 8 2 CharacteristicsEvolutionary stage OH IR red supergiantSpectral type M5 I 3 M7 5e 4 5 Apparent magnitude K 6 849 6 Apparent magnitude R 15 69 7 Apparent magnitude G 15 0971 1 Apparent magnitude I 12 795 8 Apparent magnitude J 9 252 6 Apparent magnitude H 7 745 6 Variable type Carbon rich LPV Mira 8 AstrometryRadial velocity Rv 294 2 3 km sProper motion m RA 1 108 1 mas yr Dec 1 348 1 mas yrParallax p 0 2280 0 0625 mas 1 Distance160 000 ly 50 000 3 pc Absolute magnitude MV 6 00 3 DetailsRadius1 540 9 R Luminosity340 000 454 000 9 589 000 57 000 52 000 10 L Surface gravity log g 0 0 11 0 5 3 cgsTemperature3 008 3 300 9 KAge 5 10 MyrOther designationsWOH G064 2MASS J04551048 6820298 IRAS 04553 6825 MSX LMC 1182Database referencesSIMBADdataWOH G64 is surrounded by an optically thick dust envelope of roughly a light year in diameter containing 3 to 9 times the Sun s mass of expelled material that was created by the strong stellar wind 13 If placed at the center of the Solar System the star s photosphere would engulf the orbit of Jupiter Contents 1 Discovery 2 Distance 3 Variability 4 Physical properties 4 1 Spectral features 5 Possible companion 6 See also 7 Notes 8 ReferencesDiscovery EditWOH G64 was discovered in the 1970s by Bengt Westerlund Olander and Hedin Like NML Cygni the WOH in the star s name comes from the names of its three discoverers but in this case refers to a whole catalogue of giant and supergiant stars in the LMC 14 Westerlund also discovered another notable red supergiant star Westerlund 1 26 found in the massive super star cluster Westerlund 1 in the constellation Ara 15 In 1986 infrared observations showed that it was a highly luminous supergiant surrounded by gas and dust which absorbed around three quarters of its radiation 5 In 2007 observers using the Very Large Telescope VLT showed that WOH G64 is surrounded by a torus shaped cloud 13 Distance EditThe distance of WOH G64 is assumed to be around 50 000 parsecs 160 000 ly away from Earth since it appears to be in the LMC 3 The Gaia Data Release 2 parallax for WOH G64 is 0 2280 0 0625 mas and the negative parallax does not provide a reliable distance 1 Variability EditWOH G64 varies regularly in brightness by over a magnitude at visual wavelengths with a primary period of around 800 days 7 The star suffers from over six magnitudes of extinction at visual wavelengths and the variation at infra red wavelengths is much smaller 3 It has been described as a carbon rich Mira or long period variable which would necessarily be an asymptotic giant branch star AGB star rather than a supergiant 8 Brightness variability has been confirmed by other researchers in some spectral bands but it is unclear what the actual variable type is No significant spectral variation has been found 3 Physical properties Edit Artist s impression of the dusty torus around WOH G64 European Southern Observatory The spectral type of WOH G64 is given as M5 3 but it is usually found to have a much cooler spectral type of M7 5 highly unusual for a supergiant star 10 4 5 WOH G64 is classified as an extremely luminous M class supergiant and is likely to be the largest star and the most luminous and coolest red supergiant in the LMC 3 The combination of the star s temperature and luminosity places it toward the upper right corner of the Hertzsprung Russell diagram The star s evolved state means that it can no longer hold on to its atmosphere due to low density high radiation pressure and the relatively opaque products of thermonuclear fusion citation needed It has an average mass loss rate of 3 1 to 5 8 10 4 M per year among the highest known and unusually high even for a red supergiant 9 The parameters of WOH G64 are uncertain The star was originally calculated to be around between 490 000 and 600 000 L based on spectroscopic measurements assuming spherical shells suggesting initial masses at least 40 M and consequently larger values for the radius between 2 575 and 3 000 R 16 4 17 2007 measurements using the Very Large Telescope VLT gave the star a bolometric luminosity of 282 000 40 000 30 000 L suggesting an initial mass of 25 5 M and a radius around 1 730 R based on the assumption of an effective temperature of 3 200 K and radiative transfer modelling of the surrounding torus 13 In 2009 Levesque calculated an effective temperature of 3 400 25 K by spectral fitting of the optical and near UV SED Adopting the Ohnaka luminosity with this new temperature gives a radius of 1 540 R but with a margin of error of 5 or 77 R 3 Ignoring the effect of the dusty torus in redirecting infrared radiation estimates of 1 970 1 990 R based on a luminosity of 450 000 150 000 120 000 L and an effective temperature of 3 372 3 400 K have also been derived 3 Those physical parameters are consistent with the largest galactic red supergiants and hypergiants found elsewhere such as Westerlund 1 26 VY Canis Majoris and NML Cygni and with theoretical models of the coolest most luminous and largest possible cool supergiants e g the Hayashi limit or the Humphreys Davidson limit 3 13 4 A 2018 paper gives a luminosity of 432 000 L and a higher effective temperature of 3 500 K based on optical and infrared photometry and assuming spherically symmetric radiation from the surrounding dust This suggests a radius of 1 788 R 11 a Spectral features Edit WOH G64 was discovered to be a prominent source of OH H2 O and SiO masers emission which is typical of an OH IR supergiant star 3 It shows an unusual spectrum of nebular emission the hot gas is rich in nitrogen and has a radial velocity considerably more positive than that of the star 3 The stellar atmosphere is producing a strong silicate absorption band in mid infrared wavelengths accompanied a line emission due to highly excited carbon monoxide 18 Possible companion EditWOH G64 has a possible late O type dwarf companion of a bolometric magnitude of 7 5 or a luminosity of 100 000 L which would make WOH G64 a binary star although there has been no confirmation of this observation and the intervening dust clouds makes the study of the star very difficult 3 See also EditWOH S281 WOH G17 HV 888Notes Edit Applying the Stefan Boltzmann Law with a nominal solar effective temperature of 5 772 K 5772 3500 4 432 190 1787 94 R displaystyle sqrt 5772 3500 4 432 190 1787 94 R odot References Edit a b c d e f g Brown A G A et al Gaia collaboration August 2018 Gaia Data Release 2 Summary of the contents and survey properties Astronomy amp Astrophysics 616 A1 arXiv 1804 09365 Bibcode 2018A amp A 616A 1G doi 10 1051 0004 6361 201833051 Gaia DR2 record for this source at VizieR Bhardwaj Anupam Kanbur Shashi He Shiyuan Rejkuba Marina Matsunaga Noriyuki De Grijs Richard Sharma Kaushal Singh Harinder P Baug Tapas Ngeow Chow Choong Ou Jia Yu 2019 Multiwavelength Period Luminosity and Period Luminosity Color Relations at Maximum Light for Mira Variables in the Magellanic Clouds The Astrophysical Journal 884 1 20 arXiv 1908 01795 Bibcode 2019ApJ 884 20B doi 10 3847 1538 4357 ab38c2 S2CID 199452754 a b c d e f g h i j k l m n o p q r Levesque E M Massey P Plez B Olsen K A G 2009 The Physical Properties of the Red Supergiant WOH G64 The Largest Star Known The Astronomical Journal 137 6 4744 arXiv 0903 2260 Bibcode 2009AJ 137 4744L doi 10 1088 0004 6256 137 6 4744 S2CID 18074349 a b c d Van Loon J Th Cioni M R L Zijlstra A A Loup C 2005 An empirical formula for the mass loss rates of dust enshrouded red supergiants and oxygen rich Asymptotic Giant Branch stars Astronomy and Astrophysics 438 1 273 289 arXiv astro ph 0504379 Bibcode 2005A amp A 438 273V doi 10 1051 0004 6361 20042555 S2CID 16724272 a b c Elias J H March 1986 Two Supergiants in the Large Magellanic Cloud with Thick Dust Shells Astrophysical Journal 302 675 Bibcode 1986ApJ 302 675E doi 10 1086 164028 hdl 1887 6514 a b c Cutri Roc M Skrutskie Michael F Van Dyk Schuyler D Beichman Charles A Carpenter John M Chester Thomas Cambresy Laurent Evans Tracey E Fowler John W Gizis John E Howard Elizabeth V Huchra John P Jarrett Thomas H Kopan Eugene L Kirkpatrick J Davy Light Robert M Marsh Kenneth A McCallon Howard L Schneider Stephen E Stiening Rae Sykes Matthew J Weinberg Martin D Wheaton William A Wheelock Sherry L Zacarias N 2003 VizieR Online Data Catalog 2MASS All Sky Catalog of Point Sources Cutri 2003 CDS ADC Collection of Electronic Catalogues 2246 II 246 Bibcode 2003yCat 2246 0C a b Fraser Oliver J Hawley Suzanne L Cook Kem H 2008 The Properties of Long Period Variables in the Large Magellanic Cloud from MACHO The Astronomical Journal 136 3 1242 1258 arXiv 0808 1737 Bibcode 2008AJ 136 1242F doi 10 1088 0004 6256 136 3 1242 S2CID 2754884 a b c Soszynski I Udalski A Szymanski M K Kubiak M Pietrzynski G Wyrzykowski L Szewczyk O Ulaczyk K Poleski R 2009 The Optical Gravitational Lensing Experiment The OGLE III Catalog of Variable Stars IV Long Period Variables in the Large Magellanic Cloud Acta Astronomica 59 3 239 arXiv 0910 1354 Bibcode 2009AcA 59 239S a b c d Steven R Goldman Jacco Th van Loon 2016 The wind speeds dust content and mass loss rates of evolved AGB and RSG stars at varying metallicity Monthly Notices of the Royal Astronomical Society 465 1 403 433 arXiv 1610 05761 Bibcode 2017MNRAS 465 403G doi 10 1093 mnras stw2708 S2CID 11352637 a b c Davies Ben Crowther Paul A Beasor Emma R 2018 The luminosities of cool supergiants in the Magellanic Clouds and the Humphreys Davidson limit revisited Monthly Notices of the Royal Astronomical Society 478 3 3138 3148 arXiv 1804 06417 Bibcode 2018MNRAS 478 3138D doi 10 1093 mnras sty1302 S2CID 59459492 a b Groenewegen Martin A T Sloan Greg C 2018 Luminosities and mass loss rates of Local Group AGB stars and Red Supergiants Astronomy amp Astrophysics 609 A114 arXiv 1711 07803 Bibcode 2018A amp A 609A 114G doi 10 1051 0004 6361 201731089 ISSN 0004 6361 S2CID 59327105 Jones Olivia Woods Paul Kemper Franziska Kraemer Elena Sloan G Srinivasan Sivakrishnan Oliveira Joana van Loon Jacco Boyer Martha Sargent Benjamin Mc Donald I Meixner Margaret Zijlstra A Ruffel Paul Lagadec Eric Pauly Tyler May 7 2017 The SAGE Spec Spitzer Legacy program the life cycle of dust and gas in the Large Magellanic Cloud Point source classification III Monthly Notices of the Royal Astronomical Society 470 3 3250 3282 doi 10 1093 mnras stx1101 Retrieved 23 June 2022 a b c d Ohnaka K Driebe T Hofmann K H Weigelt G Wittkowski M 2009 Resolving the dusty torus and the mystery surrounding LMC red supergiant WOH G64 Proceedings of the International Astronomical Union 4 454 458 Bibcode 2009IAUS 256 454O doi 10 1017 S1743921308028858 Westerlund B E Olander N Hedin B 1981 Supergiant and giant M type stars in the Large Magellanic Cloud Astronomy amp Astrophysics Supplement Series 43 267 295 Bibcode 1981A amp AS 43 267W Westerlund B E 1987 Photometry and spectroscopy of stars in the region of a highly reddened cluster in ARA Astronomy and Astrophysics Supplement 70 3 311 324 Bibcode 1987A amp AS 70 311W ISSN 0365 0138 Elias J H Frogel J A Schwering P B W 1986 Two Supergiants in the Large Magellanic Cloud with Thick Dust Shells The Astrophysical Journal 302 675 Bibcode 1986ApJ 302 675E doi 10 1086 164028 hdl 1887 6514 Monnier J D Millan Gabet R Tuthill P G Traub W A Carleton N P Coude Du Foresto V Danchi W C Lacasse M G Morel S Perrin G Porro I L Schloerb F P Townes C H 2004 High Resolution Imaging of Dust Shells by Using Keck Aperture Masking and the IOTA Interferometer The Astrophysical Journal 605 1 436 461 arXiv astro ph 0401363 Bibcode 2004ApJ 605 436M doi 10 1086 382218 S2CID 7851916 The mass loss rates of red supergiants at low metallicity Detectionof rotational CO emission from two red supergiants in the LargeMagellanic Cloud Retrieved from https en wikipedia org w index php title WOH G64 amp oldid 1141289296, wikipedia, wiki, book, books, library,
