Omega Centauri
| Omega Centauri | |
|---|---|
The globular cluster Omega Centauri | |
| Observation data (J2000 epoch) | |
| Class | VIII |
| Constellation | Centaurus |
| Right ascension | 13h 26m 47.28s |
| Declination | −47° 28′ 46.1″ |
| Distance | 15.8 ± 1.1 kly (4.84 ± 0.34 kpc) |
| Apparent magnitude (V) | 3.9 |
| Apparent dimensions (V) | 36′.3 |
| Physical characteristics | |
| Mass | (4.05±0.1)×106 M☉ |
| Radius | 86 ± 6 ly |
| Metallicity | = –1.35 dex |
| Estimated age | 11.52 Gyr |
| Other designations | NGC 5139, GCl 24, ω Centauri, Caldwell 80, Mel 118 |
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Omega Centauri (ω Cen, NGC 5139, or Caldwell 80) is a globular cluster in the constellation of Centaurus that was first identified as a non-stellar object by Edmond Halley in 1677. Located at a distance of 17,090 light-years (5,240 parsecs), it is the largest known globular cluster in the Milky Way at a diameter of roughly 150 light-years. It is estimated to contain approximately 10 million stars, with a total mass of 4 million solar masses, making it the most massive known globular cluster in the Milky Way.
Omega Centauri is very different from most other galactic globular clusters to the extent that it is thought to have originated as the core remnant of a disrupted dwarf galaxy.