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Messier 54

Coordinates: Sky map 18h 55m 03.28s, −30° 28′ 42.6″
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Messier 54
M54 by Hubble Space Telescope; 3.4′ view
Observation data (J2000 epoch)
ClassIII[1]
ConstellationSagittarius
Right ascension18h 55m 03.33s[2]
Declination−30° 28′ 47.5″[2]
Distance87.4 kly (26.8 kpc)[3]
Apparent magnitude (V)7.6[4]
Apparent dimensions (V)12.0′
Physical characteristics
Radius153 ly[5]
Estimated age13 Gyr[6]
Notable featuresProbably extragalactic
Other designationsM54,[7] NGC 6715,[7] GCl 104,[7] C 1851-305[7]
See also: Globular cluster, List of globular clusters

Messier 54 (also known as M54 or NGC 6715) is a globular cluster in the constellation Sagittarius.[a] It was discovered by Charles Messier in 1778 and then included in his catalog of comet-like objects.

It is easily found in the sky, being close to the star ζ Sagittarii. It is, however, not resolvable into individual stars even with larger amateur telescopes.

In July 2009, a team of astronomers reported that they had found evidence of an intermediate-mass black hole in the core of M54.[8]

Distance

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Previously thought to belong to the Milky Way at a distance from Earth of about 50,000 light-years, it was discovered in 1994 that M54 most likely belongs to the Sagittarius Dwarf Elliptical Galaxy (SagDEG),[9] making it the first globular cluster formerly thought to be part of our galaxy reassigned to extragalactic status, even if not recognized as such for more than two centuries. As it is located in SagDEG's center, some authors think it actually may be its core;[10] however others have proposed that it is a real globular cluster that fell to the center of this galaxy due to decay of its orbit caused by dynamical friction.[11]

Modern estimates now place M54 at a distance of some 87,000 light-years,[3] translating into a true radius of 150 light-years across.[5] It is one of the denser of the globulars, being of class III[1] (I being densest and XII being the least dense). It shines with the luminosity of roughly 850,000 times that of the Sun and has an absolute magnitude of −10.0.

Map showing location of M54

See also

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References and footnotes

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  1. ^ a b 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". 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 Ramsay, Gavin; Wu, Kinwah (2005). "Chandra observations of the globular cluster M54". Astronomy and Astrophysics. 447 (1): 199–203. arXiv:astro-ph/0510217. Bibcode:2006A&A...447..199R. doi:10.1051/0004-6361:20053855. S2CID 18038770.
  4. ^ "Messier 54". SEDS Messier Catalog. Retrieved 29 April 2022.
  5. ^ a b From trigonometry: radius = distance × sin( diameter_angle / 2 ) = 153 ly.
  6. ^ Geisler, Doug; Wallerstein, George; Smith, Verne V.; Casetti-Dinescu, Dana I. (2007). "Chemical Abundances and Kinematics in Globular Clusters and Local Group Dwarf Galaxies and Their Implications for Formation Theories of the Galactic Halo". Publications of the Astronomical Society of the Pacific. 119 (859): 939–961. arXiv:0708.0570. Bibcode:2007PASP..119..939G. doi:10.1086/521990. S2CID 119599242.
  7. ^ a b c d "M 54". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2006-11-16.
  8. ^ Ibata, R.; Bellazzini, M.; Chapman, S. C.; Dalessandro, E.; et al. (2009). "Density and Kinematic Cusps in M54 at the Heart of the Sagittarius Dwarf Galaxy: Evidence for a 104 M☉ Black Hole?". Astrophysical Journal Letters. 699 (2): L169–L173. arXiv:0906.4894. Bibcode:2009ApJ...699L.169I. doi:10.1088/0004-637X/699/2/L169. S2CID 15976588.
  9. ^ Siegel, Michael H.; Dotter, Aaron; Majewski, Steven R.; Sarajedini, Ata; et al. (2007). "The ACS Survey of Galactic Globular Clusters: M54 and Young Populations in the Sagittarius Dwarf Spheroidal Galaxy". Astrophysical Journal Letters. 667 (1): L57–L60. arXiv:0708.0027. Bibcode:2007ApJ...667L..57S. doi:10.1086/522003. S2CID 119626792.
  10. ^ Carretta, E.; Bragaglia, A.; Gratton, R. G.; Lucatello, S.; et al. (2010). "M54 + Sagittarius = ω Centauri". The Astrophysical Journal Letters. 714 (1): L7–L11. arXiv:1002.1963. Bibcode:2010ApJ...714L...7C. doi:10.1088/2041-8205/714/1/L7. S2CID 118440761.
  11. ^ Bellazzini, M.; Ibata, R. A.; Chapman, S. C.; Mackey, A. D.; et al. (2008). "The Nucleus of the Sagittarius Dsph Galaxy and M54: a Window on the Process of Galaxy Nucleation". The Astronomical Journal. 136 (3): 1147–1170. arXiv:0807.0105. Bibcode:2008AJ....136.1147B. doi:10.1088/0004-6256/136/3/1147. S2CID 53486171.
  1. ^ Specifically in centre this very mildly southern zone of the sky which is well observable from everywhere except the Arctic Circle. However the Sun, considered from our orbit, passes through this zone throughout December. This also makes the cluster mostly risen during day, not night, in the nearest months.
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