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Palomar 6

Coordinates: Sky map 17h 43m 42.20s, −26° 13′ 21.0″
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Palomar 6
Observation data (J2000 epoch)
ClassXI
ConstellationOphiuchus
Right ascension17h 43m 42.20s[1]
Declination−26° 13′ 21.0″[1]
Distance25.02 ± 0.62 kly (7.67 ± 0.19 kpc)[2]
Physical characteristics
Mass2.28×105[3] M
Metallicity = –0.91[3] dex
Estimated age12.4 ± 0.9 Gyr[2]
Other designationsESO 520-21, GCl 75, 1740-262[1]
See also: Globular cluster, List of globular clusters

Palomar 6 is a loose globular cluster in the constellation Ophiuchus that belongs to the Milky Way galaxy. It is a member of the Palomar Globular Clusters group. It is located about 25,000 light-years (7,700 parsecs) away from the Sun.[2] It formed in what would become the bulge of the Milky Way. It is similar to other old-bulge globular clusters such as Messier 62, NGC 6522, NGC 6558, and Haute-Provence 1.[2]

First discovered on the National Geographic Society – Palomar Observatory Sky Survey plates by Robert G. Harrington and Fritz Zwicky,[4] it was catalogued as a globular cluster, and is one of four globulars known to contain a planetary nebula.

References

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  1. ^ a b c "SIMBAD Astronomical Database". Results for Palomar 6. Retrieved 2009-10-04.
  2. ^ a b c d Souza, S. O.; Valentini, M.; Barbuy, B.; Pérez-Villegas, A.; Chiappini, C.; Ortolani, S.; Nardiello, D.; Dias, B.; Anders, F.; Bica, E. (2021). "Photo-chemo-dynamical analysis and the origin of the bulge globular cluster Palomar 6". Astronomy & Astrophysics. 656: A78. arXiv:2109.04483. doi:10.1051/0004-6361/202141768. S2CID 237485386.
  3. ^ 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.
  4. ^ 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.
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