Microscopium

Microscopium
Constellation

Abbreviation Mic
Genitive Microscopii
Pronunciation /ˌmaɪkrəˈskɒpiəm/, genitive /ˌmaɪkrəˈskɒpiaɪ/
Symbolism the Microscope
Right ascension 21
Declination −36
Quadrant SQ4
Area 210 sq. deg. (66th)
Main stars 5
Bayer/Flamsteed
stars		 13
Stars with planets 2
Stars brighter than 3.00m 0
Stars within 10.00 pc (32.62 ly) 2
Brightest star γ Mic (4.67m)
Messier objects none
Meteor showers Microscopids
Bordering
constellations
Visible at latitudes between +45° and −90°.
Best visible at 21:00 (9 p.m.) during the month of September.

Microscopium /ˌmaɪkrəˈskɒpiəm/ is a minor constellation in the Southern Celestial Hemisphere, one of twelve created in the 18th century by French astronomer Nicolas Louis de Lacaille and one of several depicting scientific instruments. Its name is a Latinised form of the Greek word for microscope. Its stars are faint and hardly visible from most of the non-tropical Northern Hemisphere.

The constellation's brightest star is Gamma Microscopii of apparent magnitude 4.68, a yellow giant 2.5 times the Sun's mass located around 381 light-years distant. It passed within 1.14 and 3.45 light-years of the Sun some 3.9 million years ago, possibly disturbing the outer Solar System. Two star systems—WASP-7 and HD 205739—have planets, while two others—the young red dwarf star AU Microscopii and the sunlike HD 202628—have debris disks. AU Microscopii and the binary red dwarf system AT Microscopii are probably a wide triple system and members of the Beta Pictoris moving group. Nicknamed "Speedy Mic", BO Microscopii is a star with an extremely fast rotation period of 9 hours 7 minutes.

Characteristics

Microscopium is a small constellation bordered by Capricornus to the north, Piscis Austrinus and Grus to the west, Sagittarius to the east, and Indus to the south, touching on Telescopium to the southeast. The recommended three-letter abbreviation for the constellation, as adopted by the International Astronomical Union in 1922, is 'Mic'.[1] The official constellation boundaries, as set by Eugène Delporte in 1930, are defined by a polygon of four segments (illustrated in infobox). In the equatorial coordinate system, the right ascension coordinates of these borders lie between 20h 27.3m and 21h 28.4m, while the declination coordinates are between −27.45° and −45.09°.[2] The whole constellation is visible to observers south of latitude 45°N.[3][lower-alpha 1] Given that its brightest stars are of fifth magnitude, the constellation is invisible to the naked eye in areas with polluted skies.[4][lower-alpha 2]

Features

The constellation Microscopium as it can be seen by the naked eye.

Stars

French astronomer Nicolas Louis de Lacaille charted and designated ten stars with the Bayer designations Alpha through to Iota in 1756. A star in neighbouring Indus that Lacaille had labelled Nu Indi turned out to be in Microscopium, so Gould renamed it Nu Microscopii. Francis Baily considered Gamma and Epsilon Microscopii to belong to the neighbouring constellation Piscis Austrinus, but subsequent cartographers did not follow this.[6] In his 1725 Catalogus Britannicus, John Flamsteed labelled the stars 1, 2, 3 and 4 Piscis Austrini, which became Gamma Microscopii, HR 8076, HR 8110 and Epsilon Microscopii respectively.[7] Within the constellation's borders, there are 43 stars brighter than or equal to apparent magnitude 6.5.[lower-alpha 3][3]

Depicting the eyepiece of the microscope is Gamma Microscopii,[8] which—at magnitude of 4.68—is the brightest star in the constellation. Having spent much of its 620-million-year lifespan as a blue-white main sequence star, it has swollen and cooled to become a yellow giant of spectral type G6III, with a diameter ten times that of the Sun.[9] Measurement of its parallax yields a distance of 229±4 light years from Earth.[10] At around 2.5 times the mass of the Sun, it likely passed within 1.14 and 3.45 light-years of the Sun some 3.9 million years ago, possibly massive enough and close enough to disturb the Oort cloud.[11] Alpha Microscopii is also an ageing yellow giant star of spectral type G7III with an apparent magnitude of 4.90.[12] Located 380±30 light-years away from Earth,[10] it has swollen to 17.5 times the diameter of the Sun.[13] Alpha has a 10th magnitude companion, visible in 7.5 cm telescopes,[14][15] though this is a coincidental closeness rather than a true binary system.[13] Epsilon Microscopii lies 182±2 light years away,[10] and is a white star of apparent magnitude 4.7,[15] and spectral type A1V.[16] Theta1 and Theta2 Microscopii make up a wide double whose components are splittable to the naked eye. Both are white A-class magnetic spectrum variable stars with strong metallic lines, similar to Cor Caroli. They mark the constellation's specimen slide.[8]

Many notable objects are too faint to be seen with the naked eye. AX Microscopii, better known as Lacaille 8760, is a red dwarf which lies only 12.9 light-years from the Solar System. At magnitude 6.68, it is the brightest red dwarf in the sky.[17] BO Microscopii is a rapidly rotating star that has 80% the diameter of the Sun. Nicknamed "Speedy Mic", it has a rotation period of 9 hours 7 minutes.[18] An active star, it has prominent stellar flares that average 100 times stronger than those of the Sun, and are emitting energy mainly in the X-ray and ultraviolet bands of the spectrum.[19] AT Microscopii is a binary star system, both members of which are flare star red dwarfs. The system lies close to and may form a very wide triple system with AU Microscopii,[20] a young star which appears to be a planetary system in the making with a debris disk. The three stars are candidate members of the Beta Pictoris moving group, one of the nearest associations of stars that share a common motion through space.[21]

The Astronomical Society of Southern Africa in 2003 reported that observations of four of the Mira variables in Microscopium were very urgently needed as data on their light curves was incomplete.[22] Two of them—R and S Microscopii—are challenging stars for novice amateur astronomers,[23] and the other two U and RY Microscopii are more difficult still.[22] Another red giant, T Microscopii, is a semiregular variable that ranges between magnitudes 7.7 and 9.6 over 344 days.[24] Of apparent magnitude 11, DD Microscopii is a symbiotic star system composed of an orange giant of spectral type K2III and white dwarf in close orbit, with the smaller star ionizing the stellar wind of the larger star. The system has a low metallicity. Combined with its high galactic latitude, this indicates that the star system has its origin in the galactic halo of the Milky Way.[25]

HD 205739 is a yellow-white main sequence star of spectral type F7V that is around 1.22 times as massive and 2.3 times as luminous as the Sun. It has a Jupiter-sized planet with an orbital period of 280 days that was discovered by the radial velocity method.[26] WASP-7 is a star of spectral type F5V with an apparent magnitude of 9.54, about 1.28 times as massive as the Sun. Its hot Jupiter planet—WASP-7b—was discovered by transit method and found to orbit the star every 4.95 days.[27] HD 202628 is a sunlike star of spectral type G2V with a debris disk that ranges from 158 to 220 AU distant. Its inner edge is sharply defined, indicating a probable planet orbiting between 86 and 158 AU from the star.[28]

Deep sky objects

Describing Microscopium as "totally unremarkable", astronomer Patrick Moore concluded there was nothing of interest for amateur observers.[29] NGC 6925 is a barred spiral galaxy of apparent magnitude 11.3 which is lens-shaped, as it lies almost edge-on to observers on Earth, 3.7 degrees west-northwest of Alpha Microscopii.[30] SN 2011ei, a Type II Supernova in NGC 6925, was discovered by Stu Parker in New Zealand in July 2011.[31] NGC 6923 lies nearby and is a magnitude fainter still.[32] The Microscopium Void is a roughly rectangular region of relatively empty space, bounded by incomplete sheets of galaxies from other voids.[33] The Microscopium Supercluster is an overdensity of galaxy clusters that was first noticed in the early 1990s. The component Abell clusters 3695 and 3696 are likely to be gravitationally bound, while the relations of Abell clusters 3693 and 3705 in the same field are unclear.[34]

Meteor showers

Seen in the 1824 star chart set Urania's Mirror (in the lower left)

The Microscopids are a minor meteor shower that appear from June to mid-July.[35]

History

The stars that comprise Microscopium are in a region previously considered the hind feet of Sagittarius, a neighbouring constellation.[36] John Ellard Gore wrote that al-Sufi seems to have reported that Ptolemy had seen the stars but he (Al Sufi) did not pinpoint their positions.[37] Microscopium itself was introduced in 1751–52 by Lacaille with the French name le Microscope,[38][39] after he had observed and catalogued 10,000 southern stars during a two-year stay at the Cape of Good Hope. He devised fourteen new constellations in uncharted regions of the Southern Celestial Hemisphere not visible from Europe. All but one honoured instruments that symbolised the Age of Enlightenment.[40] Commemorating the compound microscope,[41] the Microscope's name had been Latinised by Lacaille to Microscopium by 1763.[38]

Notes

  1. ↑ While parts of the constellation technically rise above the horizon to observers between 45°N and 62°N, stars within a few degrees of the horizon are to all intents and purposes unobservable.[3]
  2. ↑ Objects of magnitude 5.0 are barely visible to the unaided eye in the night skies of city-suburban transition areas.[5]
  3. ↑ Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban-rural transition night skies.[5]

References

Citations

  1. ↑ Russell, Henry Norris (1922). "The new international symbols for the constellations". Popular Astronomy. Vol. 30. p. 469. Bibcode:1922PA.....30..469R.
  2. ↑ "Microscopium, constellation boundary". The Constellations. International Astronomical Union. Retrieved 13 July 2012.
  3. 1 2 3 Ian Ridpath. "Constellations: Lacerta–Vulpecula". Star Tales. Self-published. Retrieved 29 November 2014.
  4. ↑ Kambič, Bojan (2009). Viewing the Constellations with Binoculars. Springer. p. 341. ISBN 0-387-85354-5.
  5. 1 2 Bortle, John E. (February 2001). "The Bortle Dark-Sky Scale". Sky & Telescope. Sky Publishing Corporation. Retrieved 29 November 2014.
  6. ↑ Wagman 2003, pp. 181, 210.
  7. ↑ Wagman 2003, p. 458.
  8. 1 2 Motz, Lloyd; Nathanson, Carol (1991). The Constellations: An Enthusiast's Guide to the Night Sky. London, United Kingdom: Aurum Press. pp. 369–370. ISBN 1-85410-088-2.
  9. ↑ Kaler, James B. (Jim). "Gamma Mic". Stars. Retrieved 13 July 2012.
  10. 1 2 3 van Leeuwen, F. (2007). "Validation of the New Hipparcos Reduction". Astronomy and Astrophysics. 474 (2): 653–664. Bibcode:2007A&A...474..653V. arXiv:0708.1752 Freely accessible. doi:10.1051/0004-6361:20078357.
  11. ↑ Bailer-Jones, C. A. L. (2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. Bibcode:2015A&A...575A..35B. arXiv:1412.3648 Freely accessible. doi:10.1051/0004-6361/201425221. A35.
  12. ↑ "Alpha MicroscopiI". SIMBAD. Retrieved 15 July 2012.
  13. 1 2 Kaler, James B. (Jim). "Alpha Mic". Stars. Retrieved 19 March 2015.
  14. ↑ Malin, David; Frew , David J. (1995). Hartung's Astronomical Objects for Southern Telescopes, with an Addendum for Northern Observatories: A Handbook for Amateur Observers. Cambridge, United Kingdom: Cambridge University Press. p. 287. ISBN 978-0-521-55491-6.
  15. 1 2 Ridpath, Ian; Tirion, Wil (2007). Stars and Planets Guide. Princeton, New Jersey: Princeton University Press. pp. 184–185. ISBN 978-0-691-13556-4.
  16. ↑ "Epsilon Microscopii". SIMBAD. Retrieved 15 July 2012.
  17. ↑ Croswell, Ken (July 2002). "The Brightest Red Dwarf". Sky & Telescope. p. 32. Retrieved 15 July 2012.
  18. ↑ Dunstone, N.J.; Barnes, J.R.; Collier Cameron, A.; Jardine, M. (2006). "The coronal structure of Speedy Mic - I. A densely packed prominence system beyond corotation". Monthly Notices of the Royal Astronomical Society. 365 (2): 530–538. Bibcode:2006MNRAS.365..530D. arXiv:astro-ph/0510739 Freely accessible. doi:10.1111/j.1365-2966.2005.09729.x.
  19. ↑ Wolter, U.; Robrade, J.; Schmitt, J.H.M.M.; Ness, J. U. (2008). "Doppler imaging an X-ray flare on the ultrafast rotator BO Mic. A contemporaneous multiwavelength study using XMM-Newton and VLT". Astronomy and Astrophysics. 478 (1): L11–L14. Bibcode:2008A&A...478L..11W. arXiv:0712.0899 Freely accessible. doi:10.1051/0004-6361:20078838.
  20. ↑ Caballero, J.A. (November 2009). "Reaching the boundary between stellar kinematic groups and very wide binaries. The Washington double stars with the widest angular separations". Astronomy and Astrophysics. 507 (1): 251–259. Bibcode:2009A&A...507..251C. arXiv:0908.2761 Freely accessible. doi:10.1051/0004-6361/200912596.
  21. ↑ McCarthy, Kyle; White, Russel J. (2012). "The Sizes of the Nearest Young Stars". The Astronomical Journal. 143 (6): 134–168. Bibcode:2012AJ....143..134M. arXiv:1201.6600 Freely accessible. doi:10.1088/0004-6256/143/6/134.
  22. 1 2 Cooper, Tim (2003). "Presidential address: Amateur Observations - Successes and Opportunities". Monthly Notes of the Astronomical Society of Southern Africa. 62: 234–240. Bibcode:2003MNSSA..62..234C.
  23. ↑ Levy, David H. (1998). Observing Variable Stars: A Guide for the Beginner. Cambridge, United Kingdom: Cambridge University Press. p. 172. ISBN 978-0-521-62755-9.
  24. ↑ Arnold, H.J.P; Doherty, Paul; Moore, Patrick (1999). The Photographic Atlas of the Stars. Boca Raton, Florida: CRC Press. p. 53. ISBN 978-0-7503-0654-6.
  25. ↑ Pereira, C.B.; Roig, F. (2009). "High-Resolution Spectroscopic Observations of Four Yellow-Type Symbiotic Stars: CD-43°14304, Hen 3-1213, Hen 3-863, and StHα 176". The Astronomical Journal. 137 (1): 118–128. Bibcode:2009AJ....137..118P. doi:10.1088/0004-6256/137/1/118.
  26. ↑ López-Morales, Mercedes; Butler, R. Paul; Fischer, Debra A.; Minniti, Dante; Shectman, Stephen A.; Takeda, Genya; Adams, Fred C.; Wright, Jason T.; Arriagada, Pamela (2008). "Two Jupiter-Mass Planets Orbiting HD 154672 and HD 205739". The Astronomical Journal. 136 (5): 1901–1905. Bibcode:2008AJ....136.1901L. arXiv:0809.1037 Freely accessible. doi:10.1088/0004-6256/136/5/1901.
  27. ↑ Hellier, Coel; Anderson, D.R.; Gillon, M.; Lister, T.A.; Maxted, P.F.L.; Queloz, D.; Smalley, B.; Triaud, A.H.M.J.; West, R.G.; Wilson, D.M.; Alsubai, K.; Bentley, S.J.; Cameron, A. Collier; Hebb, L.; Horne, K.; Irwin, J.; Kane, S.R.; Mayor, M.; Pepe, F.; Pollacco, D.; Skillen, I.; Udry, S.; Wheatley, P.J.; Christian, D.J.; Enoch, R.; Haswell, C.A.; Joshi, Y.C.; Norton, A.J.; Parley, N.; Ryans, R. (2008). "Wasp-7: A Bright Transiting-Exoplanet System in the Southern Hemisphere". The Astrophysical Journal Letters. 690 (1): L89–L91. Bibcode:2009ApJ...690L..89H. arXiv:0805.2600 Freely accessible. doi:10.1088/0004-637X/690/1/L89.
  28. ↑ Nesvold, Erika R.; Kuchner, Marc J. (2015). "Gap Clearing by Planets in a Collisional Debris Disk". The Astrophysical Journal. 798: 10. Bibcode:2015ApJ...798...83N. arXiv:1410.7784 Freely accessible. doi:10.1088/0004-637X/798/2/83. 83.
  29. ↑ Moore, Patrick (2000). Exploring the Night Sky with Binoculars. Cambridge, United Kingdom: Cambridge University Press. p. 110. ISBN 978-0-521-79390-2.
  30. ↑ Bakich, Michael E. (2010). 1001 Celestial Wonders to See Before You Die: The Best Sky Objects for Star Gazers. Patrick Moore's Practical Astronomy Series. Springer. p. 289. ISBN 1-4419-1776-4.
  31. ↑ "Supernova 2011ei in NGC 6925". Rochester Astronomy. Archived from the original on 20 June 2015. Retrieved 20 June 2015.
  32. ↑ Moore, Patrick; Tirion, Wil (1997). Cambridge Guide to Stars and Planets. Cambridge, United Kingdom: Cambridge University Press. p. 210. ISBN 0-521-58582-1.
  33. ↑ Maurellis, A.; Fairall, A.P.; Matravers, D.R.; Ellis, G.F.R. (1990). "A two-dimensional sheet of galaxies between two southern voids". Astronomy and Astrophysics. 229 (1): 75–79. Bibcode:1990A&A...229...75M. ISSN 0004-6361.
  34. ↑ Pearson, David W.; Batuski, David J. (2013). "Locating bound structure in an accelerating universe". Monthly Notices of the Royal Astronomical Society. 000: 1–12. Bibcode:2013MNRAS.436..796P. arXiv:1308.5154 Freely accessible. doi:10.1093/mnras/stt1614.
  35. ↑ Molau, Sirko; Kac, Javor; Berko, Erno; Crivello, Stefano; Stomeo, Enrico; Igaz, Antal; Barentsen, Geert (2012). "Results of the IMO Video Meteor Network - July 2012". WGN, Journal of the International Meteor Organization. 40 (5): 181–186. Bibcode:2012JIMO...40..181M.
  36. ↑ Rubie, G. (1830). The British Celestial Atlas. London, United Kingdom: Baldwin & Cradock. p. 36.
  37. ↑ Gore, John Ellard (1909). Astronomical Curiosities: Facts and Fallacies. Library of Alexandria. ISBN 978-1-4655-2442-3.
  38. 1 2 Ridpath, Ian. "Lacaille’s Southern Planisphere of 1756". Star Tales. Self-published. Retrieved 19 March 2015.
  39. ↑ Lacaille, Nicolas Louis (1756). "Relation abrégée du Voyage fait par ordre du Roi au cap de Bonne-espérance". Mémoires de l'Académie Royale des Sciences (in French): 519–592 [589].
  40. ↑ Wagman 2003, pp. 6–7.
  41. ↑ Ridpath, Ian. "Microscopium the Microscope". Star Tales. Self-published. Retrieved 19 March 2015.

Cited texts

Coordinates: 21h 00m 00s, −36° 00′ 00″

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