Coordinates: Sky map 17h 17m 07.27s, +43° 08′ 11.5″

Messier 92

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Messier 92
M92 Hubble WikiSky.jpg
Center of M92 by HST; 1.44 view
Observation data (J2000 epoch)
Right ascension17h 17m 07.39s[2]
Declination+43° 08′ 09.4″[2]
Distance26.7×10^3 ly (8.2 kpc)[3]
Apparent magnitude (V)6.4[4]
Apparent dimensions (V)14' arc minutes
Physical characteristics
Mass2.0×105[5] M
Metallicity = –2.32[6] dex
Estimated age14.2 ± 1.2 Gyr[7]
Other designationsM92, NGC 6341, GCl 59[8]
See also: Globular cluster, List of globular clusters

Messier 92 (also known as M92, M 92, or NGC 6341) is a globular cluster of stars in the northern constellation of Hercules.


It was discovered by Johann Elert Bode on December 27, 1777, then published in the Jahrbuch during 1779.[9] It was inadvertently rediscovered by Charles Messier on March 18, 1781,[a] and added as the 92nd entry in his catalogue.[10] William Herschel first resolved individual stars in 1783.


It is one of the brighter of its sort in apparent magnitude in the northern hemisphere and in its absolute magnitude in the galaxy, but it is often overlooked by amateur astronomers due to angular proximity to bright cluster Messier 13, about 20% closer. Though when compared to M13, M92 is only slightly less bright, but about 1/3 less extended. It is visible to the naked eye under very good viewing conditions.[11] With a small telescope, M92 can be seen as a nebulous smudge even in a severely light-polluted sky, and can be further resolved in darker conditions.


It is also one of the galaxy's oldest clusters. It is around 16×10^3 ly (4.9 kpc) above/below the galactic plane and 33×10^3 ly (10 kpc) from the Galactic Center.[12] It is about 26,700 light-years away from the Solar System.The half-light radius, or radius containing the upper half of its light emission, is 1.09 arcminutes (), while the tidal radius, the broadest standard measure, is 15.17. It appears only slightly flattened: its minor axis is about 89% ± 3% of the major.[3]

Characteristic of other globulars, it has little of the elements other than hydrogen and helium; astronomers term this low metallicity. Specifically, relative to the Sun, its iron abundance is [Fe/H] = –2.32 dex,[12] which is 0.5% of 1.0, on this logarithmic scale, the solar abundance.[13] This puts the estimated age range for the cluster at 11 ± 1.5 billion years.[14]

Its true diameter is 109 ly, and may have a mass corresponding to 330,000 suns.[15]

The cluster is not yet in, nor guaranteed to undergo, core collapse and the core radius figures as about 2 arcseconds (″).[12] It is an Oosterhoff type II (OoII) globular cluster, which means it belongs to the group of metal-poor clusters with longer period RR Lyrae variable stars. The 1997 Catalogue of Variable Stars in Globular Clusters listed 28 candidate variable stars in the cluster, although only 20 have been confirmed. As of 2001, there are 17 known RR Lyrae variables in Messier 92.[16] 10 X-ray sources have been detected within the 1.02 arcminute half-mass radius of the cluster, of which half are candidate cataclysmic variable stars.[17][18]

M92 is approaching us at 112 km/sec. Its coordinates indicate that the Earth's North Celestial Pole periodically passes less than one degree of this cluster during the precession of Earth's axis. Thus, M92 was a "Polarissima Borealis", or "North Cluster", about 12,000 years ago (10,000 BC), and it will again in about 14,000 years (16,000 AD).[15]


See also[edit]

References and footnotes[edit]

  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. ^ a b Goldsbury, Ryan; et al. (December 2010), "The ACS Survey of Galactic Globular Clusters. X. New Determinations of Centers for 65 Clusters [ Erratum: 2011AJ....142...66G ]", 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. ^ a b Chen, C. W.; Chen, W. P. (October 2010), "Morphological Distortion of Galactic Globular Clusters", The Astrophysical Journal, 721 (2): 1790–1819, Bibcode:2010ApJ...721.1790C, doi:10.1088/0004-637X/721/2/1790
  4. ^ "Messier 92". SEDS Messier Catalog. Retrieved 30 April 2022.
  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. ^ 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.
  7. ^ Paust, Nathaniel E. Q.; Chaboyer, Brian; Sarajedini, Ata (June 2007), "BVI Photometry and the Luminosity Functions of the Globular Cluster M92", The Astronomical Journal, 133 (6): 2787–2798, arXiv:astro-ph/0703167, Bibcode:2007AJ....133.2787P, doi:10.1086/513511, S2CID 13160815
  8. ^ "M 92". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2006-11-17.
  9. ^ Kanas, Nick (2007), Star maps: history, artistry, and cartography, Springer-Praxis books in popular astronomy, Springer, p. 180, ISBN 978-0387716688
  10. ^ Garfinkle, Robert A. (1997), Star-Hopping: Your Visa to Viewing the Universe, Cambridge University Press, p. 131, ISBN 978-0521598897
  11. ^ Frommert, Hartmut; Kronberg, Christine (September 2, 2007), "Messier 92", SEDS, The Munich Astro Archive, retrieved 2012-04-08
  12. ^ a b c Drukier, G. A.; et al. (March 2007), "The Global Kinematics of the Globular Cluster M92", The Astronomical Journal, 133 (3): 1041–1057, arXiv:astro-ph/0611246, Bibcode:2007AJ....133.1041D, doi:10.1086/510721, S2CID 15452502
  13. ^ Since 10−2.29 = 0.00513.
  14. ^ Di Cecco, A.; Becucci, R.; Bono, G.; Monelli, M.; Stetson, P. B.; Degl'Innocenti, S.; Moroni, P. G. Prada; Nonino, M.; Weiss, A.; Buonanno, R.; Calamida, A. (2010-06-27). "On the absolute age of the Globular Cluster M92". Publications of the Astronomical Society of the Pacific. 122 (895): 991–999. arXiv:1006.5217. Bibcode:2010PASP..122..991D. doi:10.1086/656017.
  15. ^ a b "Messier Object 92". Retrieved 2022-05-28.
  16. ^ Kopacki, G. (2003), "Variable stars in the globular cluster M 92", Astronomy and Astrophysics, 369 (3): 862–870, arXiv:astro-ph/0211042, Bibcode:2001A&A...369..862K, doi:10.1051/0004-6361:20010155, S2CID 116811988
  17. ^ Lu, Ting-Ni; et al. (August 2011), "Chandra and HST Studies of the X-Ray Sources in Galactic Globular Cluster M92" (PDF), The Astrophysical Journal, 736 (2): 158, Bibcode:2011ApJ...736..158L, doi:10.1088/0004-637X/736/2/158, hdl:1721.1/95659, S2CID 54766335
  18. ^ Ferraro, F. R.; Paltrinieri, B.; Fusi Pecci, F.; Rood, R. T.; Dorman, B. (1998-01-01). "Faint UV Objects in the Core of Ggcs: a New Subclass of Cvs?". Ultraviolet Astrophysics Beyond the IUE Final Archive. 413: 561. Bibcode:1998ESASP.413..561F.
  1. ^ On March 18

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