It is a rich cluster (Trumpler class II3r), with 295 stars according to Haug (1978) and 280 according with Archinal, Hynes (2003).[4] One of its members, V Centauri, is a cepheid variable. Despite its large distance from the cluster centre, it has high likelihood of being a member of it.[5] The tidal radius of the cluster is 6.4 - 12.4 parsecs (21 - 40 light years) and represents the average outer limit of NGC 5662, beyond which a star is unlikely to remain gravitationally bound to the cluster core.[3]
^Anderson, Richard I.; Eyer, Laurent; Mowlavi, Nami (July 2013). "Cepheids in open clusters: an 8D all-sky census". Monthly Notices of the Royal Astronomical Society. 434 (3): 2238–2261. arXiv:1212.5119. Bibcode:2013MNRAS.434.2238A. doi:10.1093/mnras/stt1160.
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NGC 5662 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
February 04, 2023
5662, open, cluster, constellation, centaurus, discovered, nicolas, louis, lacaille, 1752, from, south, africa, james, dunlop, observed, july, 1826, from, parramatta, australia, added, catalog, observation, data, j2000, epoch, constellationcentaurusright, asce. NGC 5662 is an open cluster in the constellation Centaurus It was discovered by Nicolas Louis de Lacaille on May 17 1752 from South Africa James Dunlop observed it on July 10 1826 from Parramatta Australia and added it to his catalog as No 342 4 NGC 5662Observation data J2000 epoch ConstellationCentaurusRight ascension14h 35m 37s 1 Declination 56 37 06 1 Distance2 170 ly 666 pc 2 Apparent magnitude V 5 5 1 Apparent dimensions V 12 Physical characteristicsMass348 3 M Estimated age93 million years 2 Other designationsMelotte 127 Colinder 284 vdBH 162See also Open cluster List of open clustersIt is a rich cluster Trumpler class II3r with 295 stars according to Haug 1978 and 280 according with Archinal Hynes 2003 4 One of its members V Centauri is a cepheid variable Despite its large distance from the cluster centre it has high likelihood of being a member of it 5 The tidal radius of the cluster is 6 4 12 4 parsecs 21 40 light years and represents the average outer limit of NGC 5662 beyond which a star is unlikely to remain gravitationally bound to the cluster core 3 References Edit a b c NGC 5662 SIMBAD Centre de donnees astronomiques de Strasbourg Retrieved 2015 06 19 a b WEBDA NGC 5662 a b Piskunov A E Schilbach E Kharchenko N V Roser S Scholz R D 6 November 2007 Tidal radii and masses of open clusters Astronomy amp Astrophysics 477 1 165 172 Bibcode 2008A amp A 477 165P doi 10 1051 0004 6361 20078525 a b Kronberg Christine Frommert Hartmut NGC 5662 messier seds org Anderson Richard I Eyer Laurent Mowlavi Nami July 2013 Cepheids in open clusters an 8D all sky census Monthly Notices of the Royal Astronomical Society 434 3 2238 2261 arXiv 1212 5119 Bibcode 2013MNRAS 434 2238A doi 10 1093 mnras stt1160 External links Edit Wikimedia Commons has media related to NGC 5662 NGC 5662 on WikiSky DSS2 SDSS GALEX IRAS Hydrogen a X Ray Astrophoto Sky Map Articles and images Retrieved from https en wikipedia org w index php title NGC 5662 amp oldid 1019580627, wikipedia, wiki, book, books, library,
