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NGC 5694

Coordinates:Sky map14h39m36.5s,−26° 32′ 18.0″
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(Redirected fromCaldwell 66)
NGC5694
The core of NGC 5694 imaged by theHubble Space Telescope
Observation data (J2000epoch)
ClassVII[1]
ConstellationHydra
Right ascension14h39m36.5s[2]
Declination−26° 32′ 18.0″[2]
Distance114,100ly[1]
Apparent magnitude(V)10.2[1]
Apparent dimensions(V)3.6[1]
Physical characteristics
Metallicity= –1.74[3]dex
Estimated age13.44Gyr[3]
Other designationsCaldwell66
See also:Globular cluster,List of globular clusters

NGC 5694(also known asCaldwell 66) is aglobular clusterin theconstellationHydra.It was discovered in 1784 byWilliam Herschel.

Characteristics

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This globular cluster is located at a distance of 114,000 light-years (35,000 pc) from theSunand 96,000 light-years (29,000 pc) from theGalactic Center[4]and is one of the oldest known globular clusters in theMilky Way Galaxy,forming nearly 12 billion years ago.[5]

Its chemical composition is highly peculiar, being highly (to nearly solar levels) enriched inalpha elements,suggesting an extragalactic origin before being captured by the Milky Way.[6]

See also

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References

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  1. ^abcd"Results for NGC 5694".SEDS NGC Catalog Online.Retrieved2010-12-07.
  2. ^ab"NGC 5694".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2010-12-07.
  3. ^abForbes, Duncan A.; Bridges, Terry (May 2010), "Accreted versus in situ Milky Way globular clusters",Monthly Notices of the Royal Astronomical Society,404(3): 1203–1214,arXiv:1001.4289,Bibcode:2010MNRAS.404.1203F,doi:10.1111/j.1365-2966.2010.16373.x,S2CID51825384.
  4. ^Harris, W.E. (1996)."A Catalog of Parameters for Globular Clusters in the Milky Way".The Astronomical Journal.112:1487.Bibcode:1996AJ....112.1487H.doi:10.1086/118116.
  5. ^"NGC/IC Project".Results for NGC 5694.Archived fromthe originalon 2012-05-20.Retrieved2010-12-07.
  6. ^Mucciarelli, A.; Bellazzini, M.; Catelan, M.; Dalessandro, E.; Amigo, P.; Correnti, M.; Cortés, C.; d'Orazi, V. (2013), "NGC 5694: Another foster son of the Galactic halo★",Monthly Notices of the Royal Astronomical Society,435(4): 3667–3680,arXiv:1308.6653,doi:10.1093/mnras/stt1558
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