1806−20 cluster: Difference between revisions
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'''Cl* 1806-20''' is a heavily-obscured [[star cluster]] on the far side of the [[Milky Way Galaxy]], approximately 50,000 light years distant. It contains the [[Soft gamma repeater|Soft Gamma-Ray Repeater]] [[SGR 1806-20]] and the [[Luminous blue variable|luminous blue variable]] [[hypergiant]] star [[LBV 1806-20]], a candidate for the most luminous star in the Galaxy. LBV 1806-20 and many of the other massive stars in the cluster are believed likely end as [[supernova]]s in a few million years, leaving only [[neutron star]]s or [[black hole]]s as remnants. |
'''Cl* 1806-20''' is a heavily-obscured [[star cluster]] on the far side of the [[Milky Way Galaxy]], approximately 50,000 light years distant. It contains the [[Soft gamma repeater|Soft Gamma-Ray Repeater]] [[SGR 1806-20]] and the [[Luminous blue variable|luminous blue variable]] [[hypergiant]] star [[LBV 1806-20]], a candidate for the most luminous star in the Galaxy. LBV 1806-20 and many of the other massive stars in the cluster are believed likely to end as [[supernova]]s in a few million years, leaving only [[neutron star]]s or [[black hole]]s as remnants. |
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The cluster is heavily obscured by intervening dust, and mostly visible in the [[infrared astronomy|infrared]]. |
The cluster is heavily obscured by intervening dust, and mostly visible in the [[infrared astronomy|infrared]]. |
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Revision as of 23:46, 17 June 2009
| Cl* 1806-20 | |
|---|---|
| Observation data (2000 epoch) | |
| Right ascension | 18h 08m 39.33s[1] |
| Declination | −20° 24′ 40.0″[1] |
| Distance | ~50000 ly (~15000 pc) |
| Physical characteristics | |
| Contains SGR 1806-20 and LBV 1806-20. | |
| Other designations | G10.0-0.3, W31 |
| Associations | |
| Constellation | Sagittarius |
Cl* 1806-20 is a heavily-obscured star cluster on the far side of the Milky Way Galaxy, approximately 50,000 light years distant. It contains the Soft Gamma-Ray Repeater SGR 1806-20 and the luminous blue variable hypergiant star LBV 1806-20, a candidate for the most luminous star in the Galaxy. LBV 1806-20 and many of the other massive stars in the cluster are believed likely to end as supernovas in a few million years, leaving only neutron stars or black holes as remnants.
The cluster is heavily obscured by intervening dust, and mostly visible in the infrared. It is part of the larger W31 H II region and giant molecular cloud. It has a compact core (diam ~0.2 pc) with a more extended halo (diam ~2 pc) containing the LBV,[1] and also contains at least three Wolf-Rayet stars (of types WC8, WN6, and WN7) and an OB supergiant, plus other young massive stars[2].
See also
References
External links
- The Unusual High-Mass Star Cluster 1806-20 [2]
 | This star cluster–related article is a stub. You can help Wikipedia by expanding it. |
