Astronomy:Mensa (constellation)

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Short description: Constellation in the southern celestial hemisphere


Mensa
Constellation
Mensa
AbbreviationMen
GenitiveMensae
Pronunciation/ˈmɛnsə/
genitive: /ˈmɛnsiː/
Symbolismthe Table Mountain
Right ascension 03h 12m 55.9008s -  07h 36m 51.5289s
Declination−71° - −85.5°
QuadrantSQ1
Area153 sq. deg. (75th)
Main stars4
Bayer/Flamsteed
stars		16
Stars with planets3
Stars brighter than 3.00m0
Stars within 10.00 pc (32.62 ly)0
Brightest starα Men (5.09m)
Messier objects0
Meteor showers0
Bordering
constellations		Chamaeleon
Dorado
Hydrus
Octans
Volans
Visible at latitudes between +4° and −90°.
Best visible at 21:00 (9 p.m.) during the month of January.
The constellation Mensa as seen by the naked eye

Mensa is a constellation in the Southern Celestial Hemisphere near the south celestial pole, one of fourteen constellations drawn up in the 18th century by French astronomer Nicolas-Louis de Lacaille. Its name is Latin for table, though it originally commemorated Table Mountain and was known as "Mons Mensae". One of the eighty-eight constellations designated by the International Astronomical Union (IAU), it covers a keystone-shaped wedge of sky 153.5 square degrees in area. Other than the south polar constellation of Octans, it is the most southerly of constellations and is observable only south of the 5th parallel of the Northern Hemisphere.

One of the faintest constellations in the night sky, Mensa contains no apparently bright stars—the brightest, Alpha Mensae, is barely visible in suburban skies. Part of the Large Magellanic Cloud, several star clusters and a quasar lie in the area covered by the constellation, and at least three of its star systems have been found to have exoplanets.

History

Originally named "Montagne de la Table" or "Mons Mensae",[1] Mensa was created by Nicolas-Louis de Lacaille out of dim Southern Hemisphere stars in honor of Table Mountain, a South African mountain overlooking Cape Town, near the location of Lacaille's observatory. He recalled that the Magellanic Clouds were sometimes known as Cape clouds, and that Table Mountain was often covered in clouds when a southeasterly stormy wind blew. Hence he made a "table" in the sky under the clouds.[2] Lacaille had observed and catalogued 10,000 southern stars during a two-year stay at the Cape of Good Hope. He devised 14 new constellations in uncharted regions of the Southern Celestial Hemisphere not visible from Europe. Mensa was the only constellation that did not honor an instrument symbolic of the Age of Enlightenment.[3] Sir John Herschel proposed shrinking the name to one word in 1844, noting that Lacaille himself had abbreviated some of his constellations thus.[4]

Although the stars of Mensa do not feature in any ancient mythology, the mountain it is named after has a rich mythology. Called "Tafelberg" in Dutch and German, it has two neighboring mountains called "Devil's Peak" and "Lion's Head". Table Mountain features in the mythology of the Cape of Good Hope, notorious for its storms. Explorer Bartolomeu Dias saw the mountain as a mythical anvil for storms.

Characteristics

Mensa is bordered by Dorado to the north, Hydrus to the northwest and west, Octans to the south, Chamaeleon to the east and Volans to the northeast. Covering 153.5 square degrees and 0.372% of the night sky, it ranks 75th of the 88 constellations in size.[5] The three-letter abbreviation for the constellation, as adopted by the IAU in 1922, is "Men".[6] The official constellation boundaries, as set by Belgian astronomer Eugène Delporte in 1930, are defined by a polygon of eight segments. In the equatorial coordinate system, the right ascension coordinates of these borders lie between  03h 12m 55.9008s and  07h 36m 51.5289s, while the declination coordinates are between −69.75° and −85.26°.[7] The whole constellation is visible to observers south of latitude 5°N.[5][lower-alpha 1]

Features

Stars

Bright stars

Lacaille gave eleven stars in the constellation Bayer designations, using the Greek alphabet to label them Alpha through to Lambda Mensae (excluding Kappa). Gould later added Kappa, Mu, Nu, Xi and Pi Mensae. Stars as dim as these were not generally given designations; however, Gould felt their closeness to the South Celestial Pole warranted their naming.[2] Alpha Mensae is the brightest star with a barely visible apparent magnitude of 5.09,[8] making it the only constellation with no star above magnitude 5.0.[9] Overall, there are 22 stars within the constellation's borders brighter than or equal to apparent magnitude 6.5.[lower-alpha 2][5]

  • Alpha Mensae is a solar-type star (class G7V) 33.32 ± 0.02 light-years from Earth.[11] It came to within 11 light-years from Earth around 250,000 years ago and would have been considerably brighter back then—nearly of second magnitude.[12] An infrared excess has been detected around this star, indicating the presence of a circumstellar disk at a radius of over 147 astronomical units (AU). The estimated temperature of this dust is below 22 K.[13] However, data from Herschel Space Observatory failed to confirm this excess, leaving the finding in doubt.[14] No planetary companions have yet been discovered around it. It has a red dwarf companion star at an angular separation of 3.05 arcseconds; equivalent to a projected separation of roughly 30 AU.[8][15][16]
  • Gamma Mensae is the second-brightest star in the constellation, at magnitude 5.19.[17] Located 104.9 ± 0.5 light-years from Earth,[11] it is an ageing (10.6 billion year-old) star around 1.04 times as massive as the Sun. It has swollen to around 5 times the solar radius,[18] becoming an orange giant of spectral type K2III.[19]
  • Beta Mensae is slightly fainter at magnitude 5.31.[17] Located 660 ± 10 light-years from Earth,[11] it is a yellow giant of spectral type G8III, around 3.6 times as massive and 513 times as luminous as the Sun. It is 270 million years old,[20] and lies in front of the Large Magellanic Cloud.[17]
  • Zeta and Eta Mensae have infrared excesses suggesting they too have circumstellar disks of dust.[21][22] Zeta Mensae is an ageing white giant of spectral type A5 III around 394 ± 4 light-years from Earth,[23][11] and Eta Mensae is an orange giant of spectral type K4 III,[22] lying 650 ± 10 light-years away from Earth.[11]
  • Pi Mensae is a solar-type (G1) star 59.62 ± 0.07 light-years distant.[11] In 2001, a substellar companion was discovered in an eccentric orbit.[24] Incorporating more accurate Hipparcos data yields a mass range for the companion to be anywhere from 10.27 to 29.9 times that of Jupiter. This confirms its substellar nature with the upper limit of mass putting it in the brown dwarf range.[25] The discovery of a second substellar companion—a super-Earth—was announced on 16 September 2018. It takes 6.27 days to complete its orbit and is the first exoplanet detected by the Transiting Exoplanet Survey Satellite (TESS) submitted for publication.[26]

Planet-hosting stars

Variable stars

  • TZ Mensae is an eclipsing binary that varies between magnitude 6.2 and 6.9 every 8.57 days.[9] It is composed of two white main sequence stars in close orbit. One of these is of spectral type A0V, has a radius twice as that of the Sun and is 2.5 times as massive. The other, an A8V spectral type, has a radius 1.4 times that of the Sun and is 1.5 times as massive.[30][31]
  • UX Mensae is another eclipsing binary system composed of two young stars around 1.2 times as massive as the Sun and 2.2 ± 0.5 billion years of age,[32] orbiting each other every 4.19 days.[33] The system is 338.2 ± 0.9 light-years distant.[11]
  • TY Mensae is another eclipsing binary system classified as a W Ursae Majoris variable; the two components are so close that they share a common envelope of stellar material. The larger star has been calculated to be 1.86 times as massive, have 1.85 times the diameter and is 13.6 times as luminous, while the smaller is 0.4 times as massive, 0.84 times the diameter, and 1.7 times as luminous as the Sun. Their surface temperatures have been calculated at 8164 and 7183 K respectively.[34]
  • YY Mensae is an orange giant of spectral type K1III around 2.2 times as massive as the Sun, with 12.7 times its diameter and 70 times its luminosity. A rapidly rotating star with a period of 9.5 days, it is a strong emitter of X-rays and belongs to a class of star known as FK Comae Berenices variables.[35] These stars are thought to have formed with the merger of two stars in a contact binary system.[36] With an apparent magnitude of 8.05, it is 707 ± 6 light-years distant.[11]
  • AH Mensae is a cataclysmic variable star system composed of a white dwarf and a red dwarf that orbit each other every 2 hours 57 minutes. The stars are close enough that the white dwarf strips material off the red dwarf, creating an accretion disc that periodically ignites with a resulting brightening of the system.[37]
NGC 1987 imaged by the Hubble Space Telescope
  • TU Mensae is another cataclysmic variable composed of a red dwarf and white dwarf. The orbital period of 2 hours 49 minutes is one of the longest for cataclysmic variable systems exhibiting brighter outbursts, known as superhumps. The normal outbursts result in an increase in brightness lasting around a day every 37 days, while the superhumps last 5–20 days and take place every 194 days.[38]
  • AO Mensae is a faint star of magnitude 9.8. An orange dwarf that has 80% the size and mass of the Sun,[39] it is also a BY Draconis variable.[40] These are a class of stars with starspots prominent enough that the star changes brightness as it rotates.[41] It is a member of the Beta Pictoris moving group, a loose association of young stars moving across the galaxy.[39]

Other stars

  • WISE 0535−7500 is a binary system composed of two sub-brown dwarfs of spectral class cooler than Y1 located 47 ± 3 light-years away. Unable to be separated by observations to date, they are presumed to be of similar mass—8 to 20 times that of Jupiter—and are less than one AU apart.[42]

Deep-sky objects

File:Discs and Bulges IC 2051.tif

The Large Magellanic Cloud lies partially within Mensa's boundaries,[44] although most of it lies in neighbouring Dorado.[9] It is a satellite galaxy of the Milky Way, located at a distance of 163,000 light-years.[45] Among its stars within Mensa are W Mensae, an unusual yellow-white supergiant that belongs to a rare class of star known as a R Coronae Borealis variable,[46] HD 268835, a blue hypergiant that is girded by a vast circumstellar disk of dust,[47] and R71, a luminous blue variable star that brightened in 2012 to over a million times as luminous as the Sun.[48] Also within the galaxy is NGC 1987, a globular cluster estimated to be around 600 million years old that has a significant number of red ageing stars,[49] and NGC 1848, a 27 million year old open cluster.[50] Mensa contains several described open clusters, most of which can be only be clearly observed from large telescopes.[51]

PKS 0637-752 is a distant quasar with a calculated redshift of z = 0.651. It was chosen as the first target of the then newly-operational Chandra X-Ray Observatory in 1999. The resulting images revealed a gas jet approximately 330,000 light-years long. It is visible at radio, optical and x-ray wavelengths.[52]

Notes

  1. ↑ While parts of the constellation technically rise above the horizon to observers between 5°N and 20°N, stars within a few degrees of the horizon are practically unobservable.[5]
  2. ↑ Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban–rural transition night skies.[10]

References

  1. ↑ Ridpath, Ian. "Mensa: the Table Mountain". http://www.ianridpath.com/startales/mensa.html. 
  2. ↑ 2.0 2.1 Wagman 2003, pp. 207–08.
  3. ↑ Wagman 2003, pp. 6–7.
  4. ↑ Herschel, John (1844). "Farther Remarks on the Division of Southern Constellations". Monthly Notices of the Royal Astronomical Society 6 (5): 60–62. doi:10.1093/mnras/6.5.60a. https://books.google.com/books?id=s-tBAQAAMAAJ&pg=RA1-PA62. 
  5. ↑ 5.0 5.1 5.2 5.3 Ridpath, Ian. "Constellations: Lacerta–Vulpecula". Star Tales. Self-published. http://www.ianridpath.com/constellations2.html. 
  6. ↑ Russell, Henry Norris (1922). "The New International Symbols for the Constellations". Popular Astronomy 30: 469. Bibcode: 1922PA.....30..469R. 
  7. ↑ "Mensa, Constellation Boundary". The Constellations (International Astronomical Union). https://www.iau.org/public/themes/constellations/#men. Retrieved 4 March 2016. 
  8. ↑ 8.0 8.1 "LTT 2490 – High proper-motion star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=alpha+mensae&submit=SIMBAD+search. 
  9. ↑ 9.0 9.1 9.2 Arnold, H.J.P; Doherty, Paul; Moore, Patrick (1999). The Photographic Atlas of the Stars. Boca Raton, Florida: CRC Press. p. 57. ISBN 978-0750306546. https://books.google.com/books?id=YjcvJUfnWBAC&pg=PA57. 
  10. ↑ Bortle, John E. (February 2001). "The Bortle Dark-Sky Scale". Sky & Telescope. Sky Publishing Corporation. http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y. 
  11. ↑ 11.0 11.1 11.2 11.3 11.4 11.5 11.6 11.7 11.8 11.9 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Enter the star name in the identifier box here, take reciprocal of parallax (in mas) and multiply by 3260 to get distance in light-years
  12. ↑ Kaler, Jim. "Alpha Mensae". Stars. University of Illinois. http://stars.astro.illinois.edu/sow/alphamen.html. 
  13. ↑ Eiroa, C.; Marshall, J.P.; Mora, A.; Montesinos, B.; Absil, O.; Augereau, J.Ch.; Bayo, A.; Bryden, G. et al. (2013). "DUst around NEarby Stars. The survey observational results". Astronomy & Astrophysics 555: A11. doi:10.1051/0004-6361/201321050. Bibcode: 2013A&A...555A..11E.  Search for HIPPARCOS no. of the star: 29271
  14. ↑ Sibthorpe, B.; Kennedy, G.M.; Wyatt, M.C.; Lestrade, J.-F.; Greaves, J.S.; Matthews, B.C.; Duchêne, G. (2018). "Analysis of the Herschel DEBRIS Sun-like star sample". Monthly Notices of the Royal Astronomical Society 475 (3): 3046–64. doi:10.1093/mnras/stx3188. Bibcode: 2018MNRAS.475.3046S. 
  15. ↑ Eggenberger, A. et al. (2007). "The impact of stellar duplicity on planet occurrence and properties. I. Observational results of a VLT/NACO search for stellar companions to 130 nearby stars with and without planets". Astronomy and Astrophysics 474 (1): 273–91. doi:10.1051/0004-6361:20077447. Bibcode: 2007A&A...474..273E. 
  16. ↑ "HD 43834B – Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD%2043834B.  (details on the stellar properties of the companion star)
  17. ↑ 17.0 17.1 17.2 Bagnall, Philip M. (2012). The Star Atlas Companion: What You Need to Know about the Constellations. New York: Springer. p. 290. ISBN 978-1461408307. https://books.google.com/books?id=KcIg02TKW6QC&pg=PA290. 
  18. ↑ Wittenmyer, Robert A.; Liu, Fan; Wang, Liang et al. (2016). "The Pan-Pacific Planet Search. V. Fundamental Parameters for 164 Evolved Stars". The Astronomical Journal 152 (1): 15. doi:10.3847/0004-6256/152/1/19. 19. Bibcode: 2016AJ....152...19W. 
  19. ↑ Gray, R.O.; Corbally, C.J.; Garrison, R.F. et al. (2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal 132 (1): 161–70. doi:10.1086/504637. Bibcode: 2006AJ....132..161G. 
  20. ↑ Luck, R. Earle (2015). "Abundances in the Local Region. I. G and K Giants". The Astronomical Journal 150 (3): 23. doi:10.1088/0004-6256/150/3/88. 88. Bibcode: 2015AJ....150...88L. 
  21. ↑ Ishihara, Daisuke; Takeuchi, Nami; Kobayashi, Hiroshi et al. (2017). "Faint warm debris disks around nearby bright stars explored by AKARI and IRSF". Astronomy & Astrophysics 601: 18. doi:10.1051/0004-6361/201526215. A72. Bibcode: 2017A&A...601A..72I. 
  22. ↑ 22.0 22.1 Kim, Sungsoo S.; Zuckerman, B.; Silverstone, Murray (2001). "Extent of Excess Far-Infrared Emission around Luminosity Class III Stars". The Astrophysical Journal 550 (2): 1000–06. doi:10.1086/319803. Bibcode: 2001ApJ...550.1000K. 
  23. ↑ Belle, Gerard T. (2012). "Interferometric observations of rapidly rotating stars". The Astronomy and Astrophysics Review 20 (1): 51. doi:10.1007/s00159-012-0051-2. Bibcode: 2012A&ARv..20...51V. 
  24. ↑ Jones, H.R.A.; Paul Butler, R.; Tinney, C.G. et al. (2002). "A probable planetary companion to HD 39091 from Anglo-Australian Planet Search". Monthly Notices of the Royal Astronomical Society 333 (4): 871–75. doi:10.1046/j.1365-8711.2002.05459.x. Bibcode: 2002MNRAS.333..871J.  (web Preprint)
  25. ↑ Reffert, S.; Quirrenbach, A. (2011). "Mass constraints on substellar companion candidates from the re-reduced Hipparcos intermediate astrometric data: nine confirmed planets and two confirmed brown dwarfs". Astronomy & Astrophysics 527: id.A140. doi:10.1051/0004-6361/201015861. Bibcode: 2011A&A...527A.140R. 
  26. ↑ Huang, Chelsea Xu; Burt, Jennifer; Vanderburg, Andrew; Günther, Maximilian N.; Shporer, Avi; Dittmann, Jason A.; Winn, Joshua N.; Wittenmyer, Rob et al. (2018). "TESS Discovery of a Transiting Super-Earth in the Π Mensae System". The Astrophysical Journal Letters 868 (2): L39. doi:10.3847/2041-8213/aaef91. PMID 31360431. Bibcode: 2018ApJ...868L..39H. 
  27. ↑ "Australia" (in en). http://www.nameexoworlds.iau.org/australia. 
  28. ↑ 28.0 28.1 Tinney, C.G.; Wittenmyer, Robert A.; Butler, R. Paul; Jones, Hugh R.A.; O'Toole, Simon J.; Bailey, Jeremy A.; Carter, Brad D.; Horner, J. (2011). "The Anglo-Australian Planet Search. XXI. A Gas-giant Planet in a One Year Orbit and the Habitability of Gas-giant Satellites". The Astrophysical Journal 732 (1): 31. doi:10.1088/0004-637x/732/1/31. Bibcode: 2011ApJ...732...31T. http://eprints.usq.edu.au/20482/3/Tinney_Wittenmyer_Butler_etal_AJ_2011_PV.pdf. 
  29. ↑ Brandão, I.M.; Dogan, G.; Christensen-Dalsgaard, J.; Cunha, M.S.; Bedding, T.R.; Metcalfe, T.S.; Kjeldsen, H.; Bruntt, H. et al. (2011). "The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets". Astronomy and Astrophysics. Bibcode: 2011arXiv1109.2497M. 
  30. ↑ Graczyk, Dariusz; Konorski, Piotr; Pietrzyński, Grzegorz et al. (2017). "The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions". The Astrophysical Journal 837 (1): 19. doi:10.3847/1538-4357/aa5d56. 7. Bibcode: 2017ApJ...837....7G. 
  31. ↑ Andersen, J.; Clausen, J.V.; Nordstrom, B. (1987). "Absolute dimensions of eclipsing binaries. XII – TZ Mensae". Astronomy and Astrophysics 175 (1–2): 60–70. Bibcode: 1987A&A...175...60A. 
  32. ↑ Higl, J.; Weiss, A. (2017). "Testing stellar evolution models with detached eclipsing binaries". Astronomy and Astrophysics 608: A62. doi:10.1051/0004-6361/201731008. Bibcode: 2017A&A...608A..62H. 
  33. ↑ Andersen, J.; Clausen, J.V.; Magain, P. (1989). "Absolute dimensions of eclipsing binaries. XIV – UX Mensae". Astronomy and Astrophysics 211 (2): 346–52. Bibcode: 1989A&A...211..346A. 
  34. ↑ Maceroni, C.; van't Veer, F. (1996). "The properties of W Ursae Majoris contact binaries: new results and old problems.". Astronomy and Astrophysics 311: 523–31. Bibcode: 1996A&A...311..523M. 
  35. ↑ Audard, Marc; Telleschi, Alessandra; Güdel, Manuel; Skinner, Stephen L.; Pallavicini, Roberto; Mitra-Kraev, Urmila (2004). "Some like it hot: the X-ray emission of the giant star YY Mensae". Astrophys. J. 617 (1): 531–50. doi:10.1086/424590. Bibcode: 2004ApJ...617..531A. 
  36. ↑ Howell, Steve B.; Mason, Elena; Boyd, Patricia; Smith, Krista Lynne; Gelino, Dawn M. (2016). "Rapidly Rotating, X-Ray Bright Stars in the Kepler Field". The Astrophysical Journal 831 (1): 27. doi:10.3847/0004-637X/831/1/27. Bibcode: 2016ApJ...831...27H. 
  37. ↑ Gänsicke, B.T.; Koester, D. (1999). "SW Ursae Majoris, CU Velorum and AH Mensae: three more accreting white dwarfs unveiled?". Astronomy and Astrophysics 346: 151–57. Bibcode: 1999A&A...346..151G. 
  38. ↑ Sion, Edward M.; Gänsicke, Boris T.; Long, Knox S.; Szkody, Paula; Knigge, Christian; Hubeny, Ivan; deMartino, Domitilla; Godon, Patrick (2008). "Hubble Space Telescope STIS Spectroscopy of Long-Period Dwarf Novae in Quiescence". The Astrophysical Journal 681 (1): 543–53. doi:10.1086/586699. Bibcode: 2008ApJ...681..543S. 
  39. ↑ 39.0 39.1 Messina, S; Desidera, S-; Turatto, M.; Lanzafame, A.C.; Guinan, E.F. (2010). "RACE-OC project: Rotation and variability of young stellar associations within 100 pc". Astronomy and Astrophysics 520: A15. doi:10.1051/0004-6361/200913644. Bibcode: 2010A&A...520A..15M. 
  40. ↑ Samus, N.N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1. Bibcode: 2009yCat....102025S. 
  41. ↑ AFOEV (2011). "BY Draconis variables". Observatoire de Strasbourg. http://cdsarc.u-strasbg.fr/afoev/var/eby.htx. 
  42. ↑ Leggett, S.K.; Tremblin, P.; Esplin, T.L.; Luhman, K.L.; Morley, Caroline V. (2017). "The Y-type Brown Dwarfs: Estimates of Mass and Age from New Astrometry, Homogenized Photometry, and Near-infrared Spectroscopy". The Astrophysical Journal 842 (2): 118. doi:10.3847/1538-4357/aa6fb5. Bibcode: 2017ApJ...842..118L. 
  43. ↑ "Discs and Bulges" (in en). https://www.spacetelescope.org/images/potw1950a/. 
  44. ↑ Tirion, Wil; Rappaport, Barry; Remaklus, Will (2012). Uranometria 2000.0 (All Sky ed.). Willmann-Bell. p. Chart 212. ISBN 978-0943396972. 
  45. ↑ Pietrzyński, G; Graczyk, D.; Gieren, W. et al. (2013). "An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent". Nature 495 (7439): 76–79. doi:10.1038/nature11878. PMID 23467166. Bibcode: 2013Natur.495...76P. 
  46. ↑ Milone, Luis A. (1990). "Identification charts for southern R Coronae Borealis-stars". Astrophysics and Space Science 172 (2): 263–271. doi:10.1007/BF00643318. Bibcode: 1990Ap&SS.172..263M. 
  47. ↑ Kastner, J.H.; Buchanan, C.L.; Sargent, B.; Forrest, W.J. (2006). "SpitzerSpectroscopy of Dusty Disks around B\e] Hypergiants in the Large Magellanic Cloud". The Astrophysical Journal 638 (1): L29. doi:10.1086/500804. Bibcode: 2006ApJ...638L..29K. 
  48. ↑ Mehner, A.; Baade, D.; Groh, J.H.; Rivinius, T.; Hambsch, F.-J.; Bartlett, E.S.; Asmus, D.; Agliozzo, C. et al. (2017). "Spectroscopic and photometric oscillatory envelope variability during the S Doradus outburst of the luminous blue variable R71". Astronomy and Astrophysics 608: A124. doi:10.1051/0004-6361/201731829. Bibcode: 2017A&A...608A.124M. 
  49. ↑ Zinnecker, H.; Ferraro, F.; Fusi Pecci, F.; Renzini, Alvio; Buonanno, R.; Corsi, C.E.; Turndrup, D.M. (1991-02-28). "Infrared Imaging of Intermediate Age LMC/SMC Clusters". in Haynes, Raymond. The Magellanic Clouds: Proceedings of the 148th Symposium of the International Astronomical Union, held in Sydney, Australia, July 9–13, 1990. New York: Springer Science & Business Media. pp. 228–30. ISBN 978-0792311102. https://books.google.com/books?id=F4lsaf2TTh4C&pg=PA229. 
  50. ↑ Ahumada, Andrea V.; Vega, Luis R.; Clariá, Juan J. et al. (2016). "Determination of Reddening and Age for Ten Large Magellanic Cloud Star Clusters from Integrated Spectroscopy". Publications of the Astronomical Society of the Pacific 128 (967): 094101. doi:10.1088/1538-3873/128/967/094101. Bibcode: 2016PASP..128i4101A. 
  51. ↑ Inglis, Mike (2013). Observer's Guide to Star Clusters. New York: Springer Science & Business Media. p. 148. ISBN 978-1461475675. https://books.google.com/books?id=ewHABAAAQBAJ&pg=PA148. 
  52. ↑ Schwartz, D.A.; Marshall, H.L.; Lovell, J.E.J. et al. (2000). "Chandra Discovery of a 100 kiloparsec X-Ray Jet in PKS 0637-752". The Astrophysical Journal 540 (2): 69–72. doi:10.1086/312875. Bibcode: 2000ApJ...540L..69S. 

Citations

  • Wagman, Morton (2003). Lost Stars: Lost, Missing and Troublesome Stars from the Catalogues of Johannes Bayer, Nicholas Louis de Lacaille, John Flamsteed, and Sundry Others. Blacksburg, VA: The McDonald & Woodward Publishing Company. ISBN 978-0939923786. 

External links

Coordinates: Sky map 05h 00m 00s, −80° 00′ 00″



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