Messier 22

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Messier 22
The crammed centre of Messier 22.jpg
Core of Messier 22
Observation data (J2000 epoch)
Class VII [1]
Constellation Sagittarius
Right ascension 18h 36m 23.94s [2]
Declination –23° 54′ 17.1″ [2]
Distance 10.6 ± 1.0  kly (3 ± 0.3  kpc) [3]
Apparent magnitude (V)5.1 [4]
Apparent dimensions (V)32 arcmins
Physical characteristics
Mass2.9×105 [5]   M☉
Radius50 ± 5 ly [6]
VHB14.2
Metallicity  = –1.49 [7] dex
Estimated age12  Gyr [8]
Notable featuresOne of four globulars known to contain a planetary nebula.
Other designations NGC 6656, GCl 99 [9]
See also: Globular cluster, List of globular clusters

Messier 22 or M22, also known as NGC 6656 or the Great Sagittarius Cluster, is an elliptical globular cluster of stars in the constellation Sagittarius, near the Galactic bulge region. It is one of the brightest globulars visible in the night sky. The brightest stars are 11th magnitude, with hundreds of stars bright enough to resolve with an 8" telescope. [10] It is just south of the sun's position in mid-December, and northeast of Lambda Sagittarii (Kaus Borealis), the northernmost star of the "Teapot" asterism.

Contents

M22 was one of the first globulars to be discovered, in 1665 [lower-alpha 1] by Abraham Ihle [11] [3] and it was included in Charles Messier's catalog of comet-like objects in 1764. [lower-alpha 2] It was one of the first globular clusters to be carefully studied – first by Harlow Shapley in 1930. He placed within it roughly 70,000 stars and found it had a dense core. [12] Then Halton Arp and William G. Melbourne continued studies in 1959. [13] Due to the large color spread of its red giant branch (RGB) sequence, akin to that in Omega Centauri, it became the object of intense scrutiny starting in 1977 with James E. Hesser et al. [3] [14]

M22 is one of the nearer globular clusters to Earth – at about 10,600 light-years away. It spans 32′ on the sky which means its diameter (width across) is 99 ± 9 light-years, given its estimated distance. 32 variable stars have been recorded in M22. It is in front of part of the galactic bulge and is therefore useful for its microlensing effect on those background stars. [8]

Despite its relative proximity to us, this metal-poor cluster's light is limited by dust extinction, giving it an apparent magnitude of 5.5; even so, it is the brightest globular cluster visible from mid-northern latitudes (such as Japan, Korea, Europe and most of North America). [15] From those latitudes due to its declination of nearly 24° south of the (celestial) equator, its daily path is low in the southern sky. It thus appears less impressive to people in the temperate northern hemisphere than counterparts fairly near in angle (best viewed in the Summer night sky) such as M13 and M5.

M22 is one of only four globulars of our galaxy [lower-alpha 3] known to contain a planetary nebula (an expanding, glowing gas swell from a massive star, often a red giant). It was an object first noted of interest using the IRAS satellite by Fred Gillett and his associates in 1986, as a pointlike light source [lower-alpha 4] [16] and its nature was found in 1989 by Gillett et al. [17] The planetary nebula's central star is a blue star. The nebula, designated GJJC1, is likely about only 6,000 years old. [3]

Two black holes of between 10 and 20 solar masses (M☉) each were unearthed with the Very Large Array radio telescope in New Mexico and corroborated by the Chandra X-ray telescope in 2012. [18] These imply that gravitational ejection of black holes from clusters is not as efficient as was previously thought, and leads to estimates of a total 5 to 100 black holes within M22. [19] Interactions between stars and black holes could explain the unusually large core of the cluster. [19]

See also

Footnotes and references

Footnotes

  1. ↑ on August 26
  2. ↑ on June 5
  3. ↑ the others being M15, NGC 6441 and Palomar 6
  4. ↑ IRAS 18333-2357

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<span class="mw-page-title-main">Messier 5</span> Globular cluster in the constellation Serpens

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<span class="mw-page-title-main">Messier 107</span> Globular cluster in Ophiuchus

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<span class="mw-page-title-main">Messier 3</span> Globular cluster in the constellation Canes Venatici

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<span class="mw-page-title-main">Messier 9</span> Globular cluster in Ophiuchus

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<span class="mw-page-title-main">Messier 10</span> Globular cluster in the constellation Ophiuchus

Messier 10 or M10 is a globular cluster of stars in the equatorial constellation of Ophiuchus. The object was discovered by the French astronomer Charles Messier on May 29, 1764, who cataloged it as number 10 in his catalogue and described it as a "nebula without stars". In 1774, German astronomer Johann Elert Bode likewise called it a "nebulous patch without stars; very pale". Using larger instrumentation, German-born astronomer William Herschel was able to resolve the cluster into its individual members. He described it as a "beautiful cluster of extremely compressed stars". William Parsons, 3rd Earl of Rosse thought he could distinguish a dark lane through part of the cluster. The first to estimate the distance to the cluster was Harlow Shapley, although his derivation of 33,000 light years was much further than the modern value.

<span class="mw-page-title-main">Messier 12</span> Globular cluster in the constellation Ophiuchus

Messier 12 or M 12 is a globular cluster in the constellation of Ophiuchus. It was discovered by the French astronomer Charles Messier on May 30, 1764, who described it as a "nebula without stars". In dark conditions this cluster can be faintly seen with a pair of binoculars. Resolving the stellar components requires a telescope with an aperture of 8 in (20 cm) or greater. In a 10 in (25 cm) scope, the granular core shows a diameter of 3′ (arcminutes) surrounded by a 10′ halo of stars.

<span class="mw-page-title-main">Messier 15</span> Globular cluster in the constellation Pegasus

Messier 15 or M15 is a globular cluster in the constellation Pegasus. It was discovered by Jean-Dominique Maraldi in 1746 and included in Charles Messier's catalogue of comet-like objects in 1764. At an estimated 12.5±1.3 billion years old, it is one of the oldest known globular clusters.

<span class="mw-page-title-main">Messier 28</span> Globular cluster in the constellation of Sagittarius

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<span class="mw-page-title-main">Messier 30</span> Globular cluster in the constellation Capricornus

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<span class="mw-page-title-main">Messier 54</span> Globular cluster in Sagittarius

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<span class="mw-page-title-main">Messier 53</span> Globular cluster in the constellation Coma Berenices

Messier 53 is a globular cluster in the Coma Berenices constellation. It was discovered by Johann Elert Bode in 1775. M53 is one of the more outlying globular clusters, being about 60,000 light-years (18.4 kpc) light-years away from the Galactic Center, and almost the same distance from the Solar System. The cluster has a core radius (rc) of 2.18 pc, a half-light radius (rh) of 5.84 pc, and a tidal radius (rtr) of 239.9 pc.

<span class="mw-page-title-main">Messier 56</span> Globular cluster in the constellation Lyra

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<span class="mw-page-title-main">Messier 62</span> Globular cluster in the constellation Ophiuchus

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<span class="mw-page-title-main">Messier 70</span> Globular cluster in the constellation Sagittarius

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<span class="mw-page-title-main">Messier 75</span> Globular cluster in the constellation Sagittarius

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<span class="mw-page-title-main">NGC 3201</span> Globular cluster in the constellation Vela

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<span class="mw-page-title-main">NGC 6723</span> Globular cluster in the constellation Sagittarius

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<span class="mw-page-title-main">NGC 6752</span> Globular cluster in the constellation Pavo

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<span class="mw-page-title-main">NGC 6934</span> Globular cluster in the constellation Delphinus

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References

  1. ↑ Shapley, Harlow; Sawyer, Helen B. (August 1927). "A Classification of Globular Clusters". Harvard College Observatory Bulletin. 849 (849): 11–14. Bibcode:1927BHarO.849...11S.
  2. 1 2 Goldsbury, Ryan; et al. (December 2010). "The ACS Survey of Galactic Globular Clusters. X. New Determinations of Centers for 65 Clusters". The Astronomical Journal. 140 (6): 1830–1837. arXiv: 1008.2755 . Bibcode:2010AJ....140.1830G. doi:10.1088/0004-6256/140/6/1830. S2CID   119183070.
  3. 1 2 3 4 Monaco, L.; Pancino, E.; Ferraro, F. R.; Bellazzini, M. (2004). "Wide-field photometry of the Galactic globular cluster M22". Monthly Notices of the Royal Astronomical Society . 349 (4): 1278–1290. arXiv: astro-ph/0401392 . Bibcode:2004MNRAS.349.1278M. doi:10.1111/j.1365-2966.2004.07599.x. S2CID   18252633.
  4. ↑ "Galactic Globular Clusters Database (M22)". Archived from the original on 2009-06-03.
  5. ↑ Marks, Michael; Kroupa, Pavel (August 2010). "Initial conditions for globular clusters and assembly of the old globular cluster population of the Milky Way". Monthly Notices of the Royal Astronomical Society. 406 (3): 2000–2012. arXiv: 1004.2255 . Bibcode:2010MNRAS.406.2000M. doi:10.1111/j.1365-2966.2010.16813.x. S2CID   118652005. Mass is from MPD on Table 1.
  6. ↑ From trigonometry: radius = distance × sin( diameter_angle / 2 ) = 50 ly
  7. ↑ Forbes, Duncan A.; Bridges, Terry (May 2010). "Accreted versus in situ Milky Way globular clusters". Monthly Notices of the Royal Astronomical Society. 404 (3): 1203–1214. arXiv: 1001.4289 . Bibcode:2010MNRAS.404.1203F. doi:10.1111/j.1365-2966.2010.16373.x. S2CID   51825384.
  8. 1 2 Gaudi, B. Scott (2002). "Interpreting the M22 Spike Events". Astrophysical Journal . 566 (1): 452–462. arXiv: astro-ph/0108301 . Bibcode:2002ApJ...566..452G. doi:10.1086/338041. S2CID   29501317.
  9. ↑ "M 22". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2006-11-15.
  10. ↑ Burnham's Celestial Handbook vol.3, Robert Burnham (ed.), 1978, Dover (publisher), at pages 1594–1599; this statement applies in a dark, clear, night sky.
  11. ↑ Kirch, Gottfried (1682) Annus II. Ephemeridum Motuum Coelestium Ad Annum Aerae Christianae M. DC. LXXXII. … [Second year. Ephemerides of the celestial motions for the year of the Christian era 1682.] Leipzig, (Germany): Heirs of Friedrich Lanckisch. (in Latin) 54 pages. The pages of this book are not numbered. However, in the Appendix, section III. Stella nebulosa prope pedem borealem Ganymedis observata, Lipsia, die 1. Sept. 1681. (III. Nebula near the northern foot of Ganymede observed, Leipzig, 1. September 1681.), first paragraph, Kirch enumerated recently discovered nebulae: " […] & tertia in Sagittaris, quam Dn. Joh. Abrah. Ihle Anno 1665. deprehendit; […] " ([…] and the third [nebula] in Sagittarius, which Mr. Johann Abraham Ihle discovered in the year 1665; […]) Downloadable at: Digitale Sammlungen der Universitäts- und Landesbibliothek Sachsen-Anhalt (Digital collections of the university- and state library of Sachsen-Anhalt)
  12. ↑ Shapley, Harlow (1930). "The Mass-Spectrum Relation for Giant Stars in the Globular Cluster Messier 22". Harvard College Observatory Bulletin . 874: 4–9. Bibcode:1930BHarO.874....4S.
  13. ↑ Arp, H. C.; Melbourne, W. G. (1959). "Color-magnitude diagram for the globular cluster M22". Astronomical Journal . 64: 28. Bibcode:1959AJ.....64...28A. doi:10.1086/107848.
  14. ↑ Hesser, J. E.; Hartwick, F. D. A.; McClure, R. D. (1977). "Cyanogen strengths and ultraviolet excesses of evolved stars in 17 globular clusters from DDO photometry". Astrophysical Journal Supplement Series . 33: 471. Bibcode:1977ApJS...33..471H. doi: 10.1086/190438 .
  15. ↑ Ivans, I.; Sneden, C.; Wallerstein, G.; Kraft, R. P.; Norris, J. E.; Fulbright, J. P. & Gonzalez, G. (2004). "On the Question of a Metallicity Spread in Globular Cluster M22 (NGC 6656)". Memorie della Società Astronomica Italiana . 75: 286. Bibcode:2004MmSAI..75..286I.
  16. ↑ Gillett, F. C.; Neugebauer, G.; Emerson, J. P.; Rice, W. L. (1986). "IRAS 18333-2357 – an unusual source in M22". Astrophysical Journal . 300: 722–728. Bibcode:1986ApJ...300..722G. doi: 10.1086/163846 .
  17. ↑ Cohen, J. G.; Gillett, F. C. (1989). "The peculiar planetary nebula in M22" (PDF). Astrophysical Journal . 346: 803–807. Bibcode:1989ApJ...346..803C. doi:10.1086/168061. S2CID   119770028.
  18. ↑ Gary, Stuart (4 October 2012). "Astronomers discover twin black holes". ABC Science News. Australian Broadcasting Corporation . Retrieved 5 October 2012.
  19. 1 2 Strader, J.; Chomiuk, L.; MacCarone, T. J.; Miller-Jones, J. C. A.; Seth, A. C. (2012). "Two stellar-mass black holes in the globular cluster M22". Nature. 490 (7418): 71–73. arXiv: 1210.0901 . Bibcode:2012Natur.490...71S. doi:10.1038/nature11490. PMID   23038466. S2CID   4395101.
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