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Palomar 12 is a globular cluster in the constellation Capricornus, and is a member of the Palomar Globular Clusters group.

Palomar 12
Palomar 12 by Hubble Space Telescope, 3.36′ view
Observation data (J2000 epoch)
ClassXII
ConstellationCapricornus
Right ascension21h 46m 38.84s[1]
Declination–21° 15′ 09.4″[1]
Distance63.6 ± 2.9 kly (19.50 ± 0.89 kpc)[2]
Apparent magnitude (V)11.99
Apparent dimensions (V)17′.4
Physical characteristics
Mass1.59×104[3] M☉
Radius162 ± 8 ly[4]
Metallicity = –0.85[3] dex
Estimated age6.5 Gyr[5]
Notable featuresProbably extragalactic
Other designationsGCl 123[6]
See also: Globular cluster, List of globular clusters

First discovered on the National Geographic Society – Palomar Observatory Sky Survey plates by Robert George Harrington and Fritz Zwicky,[7] it was catalogued as a globular cluster. However Zwicky came to believe this was actually a nearby dwarf galaxy in the Local Group. It is a relatively young cluster, being about 30% younger than most of the globular clusters in the Milky Way.[2] It is metal-rich with a metallicity of [Fe/H] ≈ −0.8.[5] It has an average luminosity distribution of Mv = −4.48.[8]

Based on proper motion studies, this cluster was first suspected in 2000 to have been captured from the Sagittarius Dwarf Elliptical Galaxy (SagDEG) about 1.7 Ga ago.[9] It is now generally believed to have originated in that galaxy and is associated with the Sagittarius Stream.[5] It is estimated to be 6.5 Gyr old.[5]


See also



References


  1. 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.
  2. Rosenberg, A.; et al. (1998), "Young Galactic globular clusters II. The case of Palomar 12", Astronomy and Astrophysics, 339: 61–69, arXiv:astro-ph/9809112, Bibcode:1998A&A...339...61R.
  3. 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.
  4. distance × sin( diameter_angle / 2 ) = 162 ly. radius
  5. Geisler, Doug; et al. (September 2007), "Chemical Abundances and Kinematics in Globular Clusters and Local Group Dwarf Galaxies and Their Implications for Formation Theories of the Galactic Halo", The Publications of the Astronomical Society of the Pacific, 119 (859): 939–961, arXiv:0708.0570, Bibcode:2007PASP..119..939G, doi:10.1086/521990.
  6. "Cl Pal 12". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2006-11-16.
  7. Abell, George O. (1955). "Globular Clusters and Planetary Nebulae Discovered on the National Geographic Society-Palomar Observatory Sky Survey". Publications of the Astronomical Society of the Pacific. 67 (397): 258. Bibcode:1955PASP...67..258A. doi:10.1086/126815.
  8. van den Bergh, Sidney (July 2007). "The Luminosity Distribution of Globular Clusters in Dwarf Galaxies". The Astronomical Journal. 134 (1): 344–345. arXiv:0704.2226. Bibcode:2007AJ....134..344V. doi:10.1086/518868.
  9. D. I. Dinescu; S. R. Majewski; T. M. Girard; K. M. Cudworth (2000). "The Absolute Proper Motion of Palomar 12: A Case for Tidal Capture from the Sagittarius Dwarf Spheroidal Galaxy". The Astronomical Journal. 120 (4): 1892–1905. arXiv:astro-ph/0006314. Bibcode:2000AJ....120.1892D. doi:10.1086/301552.




На других языках

[de] Palomar 12

Palomar 12 (kurz: Pal 12) ist ein Kugelsternhaufen in einer Entfernung von rund 62.000 Lichtjahren im Sternbild Steinbock. Das Objekt wurde 1953 von Robert G. Harrington und Fritz Zwicky entdeckt.
- [en] Palomar 12

[ru] Паломар 12

Паломар 12 представляет собой шаровое скопление (тип XII) в созвездии Козерога и относится к гало галактики Млечный Путь. Оно сравнительно молодое, на 30 % моложе большинства шаровых скоплений Местной группы, его возраст составляет всего 6.5 млрд лет. Однако скопление богато металлами с металличностью [Fe/H] ≈ −0,8[1]. Средняя светимость Mv = −4,48. Радиус скопления 162 ± 8 св. лет.


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