Messier 80

Messier 80
Messier 80 captured in 2026
Observation data (J2000 epoch)
ClassII
ConstellationScorpius
Right ascension16h 17m 02.41s
Declination–22° 58′ 33.9″
Distance32.6 kly (10.0 kpc)
Apparent magnitude (V)7.3
Apparent dimensions (V)10.0′
Physical characteristics
Mass5.02×105 M☉
Radius48 ly
Metallicity[Fe/H] = –1.47 dex
Estimated age13.5 ± 1.0 Gyr
Other designationsM80, NGC 6093, GCl 39
See also: Globular cluster, List of globular clusters

Messier 80 (also known as M80 or NGC 6093) is a globular cluster located approximately 32,600 light-years (10,000 pc) from Earth in the constellation Scorpius. Discovered by Charles Messier in 1781, it is one of the densest globular clusters in the Milky Way, containing several hundred thousand stars within a spatial diameter of about 95 light-years.

The cluster is situated in the Galactic halo, more than twice as distant as the Galactic Center, and lies midway between the stars α Scorpii (Antares) and β Scorpii in a region rich with nebulæ. With an apparent angular diameter of 10 arcminutes, it can be observed from locations below the 67th parallel north using modest amateur telescopes, where it appears as a mottled ball of light under low light pollution conditions.

Messier 80 is notable for its high population of blue stragglers, stars that appear younger than the cluster itself. Hubble Space Telescope observations reveal these stars are concentrated in distinct regions, suggesting frequent stellar interactions or collisions in the cluster's dense core. On May 21, 1860, the cluster hosted the nova T Scorpii, which briefly outshone the entire cluster with an absolute magnitude of −8.5 and reached an apparent magnitude of +7.0, visible through telescopes and binoculars.

See also

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. ↑ Paust, Nathaniel E. Q.; et al. (February 2010), "The ACS Survey of Galactic Globular Clusters. VIII. Effects of Environment on Globular Cluster Global Mass Functions", The Astronomical Journal, 139 (2): 476–491, Bibcode:2010AJ....139..476P, doi:10.1088/0004-6256/139/2/476, hdl:2152/34371, S2CID 120965440.
  4. ↑ "Messier 80". SEDS Messier Catalog. Archived from the original on April 30, 2022. Retrieved April 30, 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. ↑ 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. ↑ Göttgens, Fabian; Kamann, Sebastian; Baumgardt, Holger; Dreizler, Stefan; Giesers, Benjamin; Husser, Tim-Oliver; Den Brok, Mark; Fétick, Romain; Krajnovic, Davor; Weilbacher, Peter M. (2021). "Central kinematics of the Galactic globular cluster M80". Monthly Notices of the Royal Astronomical Society. 507 (4): 4788–4803. arXiv:2108.11393. doi:10.1093/mnras/stab2449.
  8. ↑ "M 80". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved November 16, 2006.
  9. 1 2 3 4 "Messier 80". SEDS Messier Database. Students for the Exploration and Development of Space. Archived from the original on January 14, 2022. Retrieved December 19, 2021.