NGC 5253 is one of the nearest of the known Blue Compact Dwarf (BCD) galaxies
|Right ascension||13h 39m 55.9s|
|Declination||−31° 38′ 24″|
|Redshift||407 ± 3 km/s|
|Distance||10.9 ± 0.6 Mly (3.33 ± 0.17 Mpc)|
|Apparent magnitude (V)||10.9|
|Apparent size (V)||5′.0 × 1′.9|
|UGCA 369, PGC 48334, Haro 10|
NGC 5253 is located within the M83 Subgroup of the Centaurus A/M83 Group, a relatively nearby galaxy group that includes the radio galaxy Centaurus A and the spiral galaxy M83 (the Southern Pinwheel Galaxy).
NGC 5253 is considered a dwarf starburst galaxy and also a blue compact galaxy. Supernova 1972E, the second-brightest recent supernova visible from Earth (peak visual magnitude of 8.5, fainter only than SN 1987A in the 20th century), occurred in this galaxy. Another supernova, SN 1895b, also has been recorded in the galaxy.
NGC 5352 contains a giant dust cloud, hiding a cluster of more than one million stars, among them up to 7,000 O stars. The super star cluster is 3 million years old and has a total luminosity of more than one billion suns. The amount of dust surrounding the stars is extraordinary — approximately 15,000 times the mass of our sun in elements such as carbon and oxygen. The dust cloud, called Cloud D is also very efficient in creating new stars. How much of a gas cloud gets turned into stars varies in different parts of the universe. In the Milky Way, the rate for gas clouds the size of Cloud D is less than 5 percent. In Cloud D, the rate is at least 10 times higher, and perhaps much more. In coming years, the cloud could be destroyed by stars that become supernovae, which would spin all of the gas and elements created by the stars into interstellar space.
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- Stuart Wolpert (March 18, 2015). "More than a million stars are forming in a mysterious dusty gas cloud in a nearby galaxy" (Press release). UCLA. Archived from the original on March 19, 2015.
- J. L. Turner; S. C. Beck; D. J. Benford; S. M. Consiglio; et al. (2015). "Highly efficient star formation in NGC 5253 possibly from stream-fed accretion". Nature. 519: 331–333. arXiv:1503.05254. Bibcode:2015Natur.519..331T. doi:10.1038/nature14218. PMID 25788096.