NGC 2419

NGC 2419

NGC 2419 by HST
Credit: NASA / STScI / WikiSky
Observation data (J2000 epoch)
Class VII[1]
Constellation Lynx
Right ascension 07h 38m 08.51s[2]
Declination +38° 52′ 54.9″[2]
Distance 275 kly (from the Sun)
300 kly (from the GC) (84.2 kpc (Sun)
91.5 kpc (GC)[3])
Apparent magnitude (V) +9.06[2]
Apparent dimensions (V) 6′
Physical characteristics
Mass 9 x 10^5 M☉
Radius 260 ly[4]
VHB 20.45[3]
Metallicity  = –2.14[5] dex
Estimated age 12.3 Gyr[5]
Other designations GCl 112,[2] Caldwell 25

NGC 2419 (also known as Caldwell 25) is a globular cluster in the constellation Lynx. It was discovered by William Herschel on December 31, 1788.[6] NGC 2419 is at a distance of about 300,000 light years from the solar system and at the same distance from the galactic center.

NGC 2419 (Credit: Adam Block/Mount Lemmon SkyCenter/University of Arizona)

NGC 2419 bears the nickname "the Intergalactic Wanderer," which was bestowed when it was erroneously thought not to be in orbit around the Milky Way. Its orbit takes it further away from the galactic center than the Magellanic Clouds, but it can (with qualifications) be considered as part of the Milky Way. At this great distance it takes three billion years to make one trip around the galaxy.[7]

The cluster is dim in comparison to more famous globular clusters such as M13. Nonetheless, NGC 2419 is a 9th magnitude object and is readily viewed, in good sky conditions, with good quality telescopes as small as 102mm (four inches) in aperture. Intrinsically it is one of the brightest and most massive globular clusters of our galaxy, having an absolute magnitude of -9.42[3] and being 900,000 times more massive than our Sun.[8]

It was proposed that NGC 2419 could be, as Omega Centauri, the remnant of a dwarf spheroidal galaxy disrupted and accreted by the Milky Way.[9] However, later research seems to disprove that possibility.[10]

Astronomer Leos Ondra has noted that NGC 2419 would be the "best and brightest" for any observers in the Andromeda Galaxy, looking for globular clusters in our galaxy since it lies outside the obscuring density of the main disk.[7] This is analogous to the way the cluster G1 can be seen orbiting outside of the Andromeda Galaxy from Earth.

References

  1. ↑ Shapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters", Harvard College Observatory Bulletin (849): 11–14, Bibcode:1927BHarO.849...11S.
  2. 1 2 3 4 "SIMBAD Astronomical Database". Results for NGC 2419. Retrieved 2006-11-17.
  3. 1 2 3 Harris, W.E. (1996). "A Catalog of Parameters for Globular Clusters in the Milky Way". AJ. 112: 1487. Bibcode:1996AJ....112.1487H. doi:10.1086/118116.
  4. ↑ distance × sin( diameter_angle / 2 ) = 260 ly. radius
  5. 1 2 Forbes, 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, Bibcode:2010MNRAS.404.1203F, arXiv:1001.4289 Freely accessible, doi:10.1111/j.1365-2966.2010.16373.x.
  6. ↑ http://messier.seds.org/xtra/ngc/n2419.html NGC 4189 at SEDS
  7. 1 2 Ferris, Timothy. Seeing in the Dark. 2002. p. 244
  8. ↑ Baumgardt, H.; Côté, P.; Hilker, M.; Rejkuba, M.; et al. (2009). "The velocity dispersion and mass-to-light ratio of the remote halo globular cluster NGC2419". Monthly Notices of the Royal Astronomical Society. 396 (4): 2051–2060. Bibcode:2009MNRAS.396.2051B. arXiv:0904.3329 Freely accessible. doi:10.1111/j.1365-2966.2009.14932.x.
  9. ↑ van den Bergh, Sidney; Mackey, A. D. (2004). "Globular clusters and the formation of the outer Galactic halo". Monthly Notices of the Royal Astronomical Society. 354 (3): 713–719. Bibcode:2004MNRAS.354..713V. arXiv:astro-ph/0407346 Freely accessible. doi:10.1111/j.1365-2966.2004.08228.x.
  10. ↑ RIPEPI V.; CLEMENTINI G.; DI CRISCIENZO M.; GRECO C.; et al. (2007). "On the remote galactic globular cluster NGC 2419.". The Astrophysical Journal. 667: L61–L64. Bibcode:2007ApJ...667L..61R. arXiv:0705.0966 Freely accessible. doi:10.1086/522000.

Coordinates: 07h 38m 08.51s, +38° 52′ 54.9″

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