NGC 6352 | |
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Observation data ( J2000 epoch) | |
Class | XI: [1] |
Constellation | Ara |
Right ascension | 17h 25m 29.11s [2] |
Declination | –48° 25′ 19.8″ [2] |
Distance | 18.3 kly (5.6 kpc) [3] |
Apparent magnitude (V) | +7.8 [4] |
Apparent dimensions (V) | 7.1′ [5] |
Physical characteristics | |
Mass | 3.7×104 [6] M☉ |
Tidal radius | 10.5″ [7] |
Metallicity | = –0.70 [8] dex |
Estimated age | 12.67 Gyr [8] |
Other designations | Caldwell 81, Cr 328, NGC 6352 [9] |
NGC 6352 (also known as Caldwell 81) is a globular cluster of stars in the southern constellation of Ara, located approximately 18.3 kly [3] from the Sun. It was discovered by Scottish astronomer James Dunlop on May 14, 1826. [10] The cluster has a Shapley–Sawyer Concentration Class of XI:. [1] A telescope with a 15 cm (5.9 in) aperture is required to resolve the stars within this loose cluster. [4]
This cluster is about 12.67 [8] billion years old with two distinct stellar populations; the second generation is only around 10 million years younger than the first. [3] It lies approximately 13 kly (4 kpc) from the Galactic Center and 1.6 kly (0.5 kpc) from the galactic plane. [11] The orbital motion of this cluster through the Milky Way suggests it is a member of the bulge or disk population. [12] It is relatively metal-rich for an object of this class, [3] having a metallicity of –0.70. [8] The core radius is 49.8″ [3] and the tidal radius is 10.5″. [7]
NGC 6352 | |
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![]() | |
Observation data ( J2000 epoch) | |
Class | XI: [1] |
Constellation | Ara |
Right ascension | 17h 25m 29.11s [2] |
Declination | –48° 25′ 19.8″ [2] |
Distance | 18.3 kly (5.6 kpc) [3] |
Apparent magnitude (V) | +7.8 [4] |
Apparent dimensions (V) | 7.1′ [5] |
Physical characteristics | |
Mass | 3.7×104 [6] M☉ |
Tidal radius | 10.5″ [7] |
Metallicity | = –0.70 [8] dex |
Estimated age | 12.67 Gyr [8] |
Other designations | Caldwell 81, Cr 328, NGC 6352 [9] |
NGC 6352 (also known as Caldwell 81) is a globular cluster of stars in the southern constellation of Ara, located approximately 18.3 kly [3] from the Sun. It was discovered by Scottish astronomer James Dunlop on May 14, 1826. [10] The cluster has a Shapley–Sawyer Concentration Class of XI:. [1] A telescope with a 15 cm (5.9 in) aperture is required to resolve the stars within this loose cluster. [4]
This cluster is about 12.67 [8] billion years old with two distinct stellar populations; the second generation is only around 10 million years younger than the first. [3] It lies approximately 13 kly (4 kpc) from the Galactic Center and 1.6 kly (0.5 kpc) from the galactic plane. [11] The orbital motion of this cluster through the Milky Way suggests it is a member of the bulge or disk population. [12] It is relatively metal-rich for an object of this class, [3] having a metallicity of –0.70. [8] The core radius is 49.8″ [3] and the tidal radius is 10.5″. [7]