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Messier 2

Coordinates: Sky map 21h 33m 27s, −00° 49′ 24″
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Messier 2
Messier 2 by Hubble Space Telescope; 2.5′ view
Observation data (J2000 epoch)
ClassII[1]
ConstellationAquarius
Right ascension21h 33m 27.02s[2]
Declination–00° 49′ 23.7″[2]
Distance55,000 ly (17 kpc)[3]
Apparent magnitude (V)6.5[4]
Apparent dimensions (V)16.0′
Physical characteristics
Mass1.04×105[5] M☉
Radius87.3 ly[6]
Metallicity = –1.65[5] dex
Estimated age12.5 Gyr[7]
Other designationsNGC 7089[8]
See also: Globular cluster, List of globular clusters

Messier 2 or M2 (also designated NGC 7089) is a globular cluster in the constellation Aquarius, five degrees north of the star Beta Aquarii. It was discovered by Jean-Dominique Maraldi in 1746, and is one of the largest known globular clusters.

Discovery and Visibility

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M2 was discovered by the French astronomer Jean-Dominique Maraldi in 1746[9] while observing a comet with Jacques Cassini.[10] Charles Messier rediscovered it in 1760, but thought that it is a nebula without any stars associated with it. William Herschel, in 1783, was the first to resolve individual stars in the cluster.[11]

M2 is, under extremely good conditions, just visible to the naked eye. Binoculars or a small telescope will identify this cluster as non-stellar, while larger telescopes will resolve individual stars, of which the brightest are of apparent magnitude 6.5.[12]

Characteristics

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Chart showing location of M2

M2 is about 55,000 light-years distant from Earth. At 175 light-years in diameter, it is one of the larger globular clusters known. The cluster is rich, compact, and significantly elliptical. It is 12.5 billion years old and one of the older globular clusters associated with the Milky Way galaxy.[7]

M2 contains about 150,000 stars, including 21 known variable stars. Its brightest stars are red and yellow giant stars. The overall spectral type is F4.[8] M2 is part of the Gaia Sausage, the hypothesized remains of a merged dwarf galaxy.[12]

Data from Gaia has led to the discovery of an extended tidal stellar stream, about 45 degrees long and 300 light-years (100 pc) wide, that is likely associated with M2. It was possibly perturbed due to the presence of the Large Magellanic Cloud.[13]

Messier 2 is located within our Milky Way galaxy, and is one of the oldest clusters of stars designated to the Milky Way. Like most globular clusters, M2 is found within the galactic halo, specifically in the southern galactic cap. This places it right below the southern pole of the Milky Way.[14]

Oosterhoff Classification

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Light curve of an RRab variable star

M2 is defined as an Oosterhoff type II globular cluster. Oosterhoff type is a classification system of globular clusters originally observed by Pieter Oosterhoff in where globular clusters are generally separated into two types. Oosterhoff type is determined by metallicity, age, and average pulsation period of type ab RR Lyrae variable stars of the cluster. A cluster metallicity below −1.6, an age above 13 billion years,[15] and an average RRab Lyrae pulsation period around .64 days indicates a type II cluster.[16] This .64 day value, coupled with a metallicity of −1.65, provides evidence that M2 follows the Oosterhoff Gap phenomena. This is an observed gap in the grouping of type I and type II clusters in the Milky Way on a metallicity vs average RRab pulsation period plot.[17]

M2 is a bit of an anomaly in reference to Oosterhoff type. While it satisfies the metallicity and RRab Lyrae pulsation period conditions, it actually has an age of 12.5 Gyr, well below the cutoff age of 13 Gyr normal for a Oosterhoff type II cluster. This is unexpected because age of a cluster is generally determined from metallicity. However, this abnormality is explained in an article by Marín-Franch.[7]

References

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  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". 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. ^ Helmi, A; van Leeuwen, F; McMillan, P J; Massari, D; Antoja, T; Robin, A; Lindegren, L; Bastian, U (2018). "Gaia Data Release 2: Kinematics of globular clusters and dwarf galaxies around the Milky Way". Astronomy and Astrophysics. 616. Gaia Collaboration: A12. arXiv:1804.09381. Bibcode:2018A&A...616A..12G. doi:10.1051/0004-6361/201832698. S2CID 260496632.
  4. ^ "Messier 2". SEDS Messier Catalog. Retrieved 21 July 2024.
  5. ^ a b Boyles, J.; et al. (November 2011). "Young Radio Pulsars in Galactic Globular Clusters". The Astrophysical Journal. 742 (1): 51. arXiv:1108.4402. Bibcode:2011ApJ...742...51B. doi:10.1088/0004-637X/742/1/51. S2CID 118649860.
  6. ^ distance × sin( diameter_angle / 2 ) = 87.3 ly. radius
  7. ^ a b c Marín-Franch, Antonio; Aparicio, Antonio; Piotto, Giampaolo; Rosenberg, Alfred; Chaboyer, Brian; Sarajedini, Ata; Siegel, Michael; Anderson, Jay; Bedin, Luigi R.; Dotter, Aaron; Hempel, Maren; King, Ivan; Majewski, Steven; Milone, Antonino P.; Paust, Nathaniel; Reid, I. Neill (2009). "The ACS Survey of Galactic Globular Clusters. VII. Relative Ages". The Astrophysical Journal. 694 (2): 1498. arXiv:0812.4541. Bibcode:2009ApJ...694.1498M. doi:10.1088/0004-637X/694/2/1498. S2CID 118407466.
  8. ^ a b "M 2". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2006-11-15.
  9. ^ Stephen James O'Meara (7 April 2014). Deep-Sky Companions: The Messier Objects. Cambridge University Press. pp. 47–. ISBN 978-1-107-01837-2.
  10. ^ "THE GLOBULAR CLUSTER M2 – Astronomy Magazine – Interactive Star Charts, Planets, Meteors, Comets, Telescopes". cs.astronomy.com. Retrieved 2023-04-29.
  11. ^ admin (2015-01-17). "Messier 2". Messier Objects. Retrieved 2023-04-29.
  12. ^ a b Myeong, G. C; Evans, N. W; Belokurov, V; Sanders, J. L; Koposov, S. E (2018). "The Sausage Globular Clusters". The Astrophysical Journal. 863 (2): L28. arXiv:1805.00453. Bibcode:2018ApJ...863L..28M. doi:10.3847/2041-8213/aad7f7. S2CID 67791285.
  13. ^ Grillmair, Carl J. (2022). "The Extended Tidal Tails of NGC 7089 (M2)". The Astrophysical Journal. 929 (1): 89. arXiv:2203.04425. Bibcode:2022ApJ...929...89G. doi:10.3847/1538-4357/ac5bd7. S2CID 247318732.
  14. ^ "M2, NGC 7089". noirlab.edu. Retrieved 2023-04-29.
  15. ^ van den Bergh, Sidney (2011). "Some Systematics of Galactic Globular Clusters". Publications of the Astronomical Society of the Pacific. 123 (907): 1044–1053. arXiv:1108.0708. Bibcode:2011PASP..123.1044V. doi:10.1086/662132. ISSN 0004-6280.
  16. ^ Stobie, R. S. (1971). "On the Difference Between the Oosterhoff Types i and II Globular Clusters". The Astrophysical Journal. 168: 381. Bibcode:1971ApJ...168..381S. doi:10.1086/151094.
  17. ^ Kuehn, Charles A.; Smith, Horace A.; Catelan, Marcio; Jeon, Young-Beom; Nemec, James M.; Walker, Alistair R.; Kunder, Andrea; Dame, Kyra; Pritzl, Barton J.; De Lee, Nathan; Borissova, Jura (2013-10-01). "RR Lyrae in the LMC: Insights Into the Oosterhoff Phenomenon". arXiv:1310.0553 [astro-ph.SR].

See also

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