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Messier 53

Messier 53
Globular cluster Messier 53 in Coma Berenices
Observation data (J2000 epoch)
ClassV[1]
ConstellationComa Berenices
Right ascension13h 12m 55.25s[2]
Declination+18° 10′ 05.4″[2]
Distance5.8×104 ly (18 kpc)[3]
Apparent magnitude (V)7.6[4]
Apparent dimensions (V)13.0′[4]
Physical characteristics
Mass8.26×105[5] M☉
Metallicity[Fe/H] = –1.86[6] dex
Estimated age12.67 Gyr[6]
Other designationsM53, NGC 5024, GCl 22, C 1310+184[7]
See also: Globular cluster, List of globular clusters

Messier 53 (also known as M53 or NGC 5024) is a globular cluster in the Coma Berenices constellation. It was discovered by Johann Elert Bode in 1775. M53 is about 60,000 light-years (18.4 kpc) light-years away from the Galactic Center, and almost the same distance (about 58,000 light-years (17.9 kpc)) from the Solar System. The cluster has a diameter of about 12 parsecs.[8]

M53 is a metal-poor cluster and at one time was thought to be the most metal-poor cluster in the Milky Way.[8] Most of the red giant branch in the cluster are first-generation stars. That is, they did not form from gas recycled from previous generations of stars in the cluster. This differs from the majority of globular clusters that are more dominated by second generation stars.[citation needed] The second generation stars in NGC 5024 tend to be more concentrated in the core region. Overall, the stellar composition of cluster members is similar to members of the Milky Way halo.[9]

The cluster displays tidal features including clumps and ripples, and tails[clarification needed] along its orbit in an east–west direction. A tidal bridge-like structure appears to connect M53 with the globular cluster NGC 5053, and an envelope[clarification needed] surrounding both clusters. These may indicate that a dynamic tidal interaction has occurred between the two clusters, a situation that may be unique within the Milky Way.[10] In addition, M53 is a candidate member of the Sagittarius dwarf galaxy tidal stream.[8]

Among the variable star population in the cluster, there are 55 RR Lyrae variables.[11] There are also at least three variables of type SX Phe and a semi-regular red giant.[12]

See also

Notes

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. ^ 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. ^ Hessels, J. W. T.; et al. (November 2007), "A 1.4 GHz Arecibo Survey for Pulsars in Globular Clusters", The Astrophysical Journal, 670 (1): 363–378, arXiv:0707.1602, Bibcode:2007ApJ...670..363H, doi:10.1086/521780, S2CID 16914232
  4. ^ a b "Messier 53". SEDS Messier Catalog. Retrieved 29 April 2022.
  5. ^ 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. ^ a b 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. ^ "NGC 5024". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 16 November 2006.
  8. ^ a b c Boberg, Owen M.; et al. (May 2015), "Chemical Abundances in NGC 5053: A Very Metal-poor and Dynamically Complex Globular Cluster", The Astrophysical Journal, 804 (2): 12, arXiv:1504.01791, Bibcode:2015ApJ...804..109B, doi:10.1088/0004-637X/804/2/109, S2CID 117834526, 109.
  9. ^ Boberg, Owen M.; et al. (June 2016), "Chemical Abundances in NGC 5024 (M53): A Mostly First Generation Globular Cluster", The Astrophysical Journal, 824 (1): 15, Bibcode:2016ApJ...824....5B, doi:10.3847/0004-637X/824/1/5, 5.
  10. ^ Chun, Sang-Hyun; et al. (February 2010), "A Wide-Field Photometric Survey for Extratidal Tails Around Five Metal-Poor Globular Clusters in the Galactic Halo", The Astronomical Journal, 139 (2): 606−625, arXiv:0912.3540, Bibcode:2010AJ....139..606C, doi:10.1088/0004-6256/139/2/606, S2CID 119232324
  11. ^ Arellano Ferro, A.; et al. (February 2012), "The unusually large population of Blazhko variables in the globular cluster NGC 5024 (M53)", Monthly Notices of the Royal Astronomical Society, 420 (2): 1333−1346, arXiv:1111.0216, Bibcode:2012MNRAS.420.1333A, doi:10.1111/j.1365-2966.2011.20119.x, S2CID 119276561.
  12. ^ Bramich, D. M.; et al. (August 2012), "Investigation of variable star candidates in the globular cluster NGC 5024 (M53)", Monthly Notices of the Royal Astronomical Society, 424 (4): 2722−2732, arXiv:1205.5112, Bibcode:2012MNRAS.424.2722B, doi:10.1111/j.1365-2966.2012.21360.x, S2CID 119190044.
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