NGC 2070

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NGC 2070
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NGC 2070 (ESO)
Credit: ESO/IDA/Danish 1.5 m/R. Gendler, C. C. Thöne, C. Féron, and J.-E. Ovaldsen
Observation data (J2000 epoch)
Right ascensionTemplate:RA[1]
DeclinationTemplate:DEC[1]
Distance157 kly (48.5 kpc)
Apparent magnitude (V)7.25[1]
Apparent dimensions (V)3.50Template:Prime × 3.50Template:Prime
Physical characteristics
Other designationsCaldwell 103, PKS 0539-69
Associations
ConstellationDorado
See also: Open cluster, List of open clusters

NGC 2070 (also known as Caldwell 103) is a large open cluster and candidate super star cluster forming the heart of the bright region in the centre-south-east of the Large Magellanic Cloud.[2] This cluster was discovered by French astronomer Nicolas-Louis de Lacaille in 1752.[3] It is at the centre of the Tarantula Nebula and produces most of the energy that makes the latter's gas and dust visible. Its central condensation is the star cluster R136, one of the most energetic star clusters known.[4] Among its stars are many of great dimension, including one of the most massive stars known (if not the most massive), R136a1, at roughly 300 M and over 7 million L.

File:Dorado IAU.svg
Sky map position of NGC 2070 (green square)

References

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  1. ^ a b c Page Module:Citation/CS1/styles.css has no content."NGC 2070". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 11 August 2017. {{cite web}}: Invalid |mode=Script error: No such module "Citation mode". (help)
  2. ^ Page Module:Citation/CS1/styles.css has no content.Shapley, H.; Lindsay, E. M. (1963). "A Catalogue of Clusters in The LMC". Irish Astronomical Journal. 6: 74. Bibcode:1963IrAJ....6...74S.
  3. ^ Page Module:Citation/CS1/styles.css has no content.Jones, K. G. (March 1969). "The search for the nebulae - VI". Journal of the British Astronomical Association. 79: 213–222. Bibcode:1969JBAA...79..213J.
  4. ^ Page Module:Citation/CS1/styles.css has no content.Bosch, Guillermo; Terlevich, Elena; Terlevich, Roberto (2009). "Gemini/GMOS Search for Massive Binaries in the Ionizing Cluster of 30 Dor". Astronomical Journal. 137 (2): 3437–3441. arXiv:0811.4748. Bibcode:2009AJ....137.3437B. doi:10.1088/0004-6256/137/2/3437. S2CID 17976455.


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