NGC 2419

Last updated
NGC 2419
Caldwell 25.jpg
NGC 2419 by HST [1]
Observation data (J2000 epoch)
Class VII [2]
Constellation Lynx
Right ascension 07h 38m 08.51s [3]
Declination +38° 52′ 54.9″ [3]
Distance 275 kly (from the Sun)
300 kly (from the GC) (84.2 kpc (Sun)
91.5 kpc (GC) [4] )
Apparent magnitude (V)+9.06 [3]
Apparent dimensions (V)6′
Physical characteristics
Mass9 x 10^5  M☉
Radius260 ly [5]
VHB20.45 [4]
Metallicity  = –2.14 [6] dex
Estimated age12.3  Gyr [6]
Other designationsGCl 112, [3] Caldwell  25
See also: Globular cluster, List of globular clusters

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. [7] 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.

Contents

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 farther 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. [8]

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 [4] and being 900,000 times more massive than the Sun. [9]

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. [10] However, that hypothesis has been disputed. [11]

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. [8] This is analogous to the way the cluster G1 can be seen orbiting outside of the Andromeda Galaxy from Earth.

It was found to be composed of two different populations, one being more helium-rich than the other, which does not fit the current model for globular cluster formation (which leads to a very homogeneous population in the cluster). This raises new questions on how this globular cluster was formed. [12]

Related Research Articles

<span class="mw-page-title-main">Messier 107</span> Globular cluster in Ophiuchus

Messier 107 or M107, also known as NGC 6171 or the Crucifix Cluster, is a very loose globular cluster in a very mildly southern part of the sky close to the equator in Ophiuchus, and is the last such object in the Messier Catalogue.

<span class="mw-page-title-main">NGC 6397</span> Globular cluster of stars in the Milky Way

NGC 6397 is a globular cluster in the constellation Ara that was discovered by French astronomer Nicolas-Louis de Lacaille in 1752. It is located about 7,800 light-years from Earth, making it one of the two nearest globular clusters to Earth. The cluster contains around 400,000 stars, and can be seen with the naked eye under good observing conditions.

<span class="mw-page-title-main">Messier 80</span> Globular cluster in the constellation Scorpius

Messier 80 is a globular cluster in the constellation Scorpius. It was discovered by Charles Messier in 1781, being one of his first discoveries.

<span class="mw-page-title-main">Messier 12</span> Globular cluster in the constellation Ophiuchus

Messier 12 or M 12 is a globular cluster in the constellation of Ophiuchus. It was discovered by the French astronomer Charles Messier on May 30, 1764, who described it as a "nebula without stars". In dark conditions this cluster can be faintly seen with a pair of binoculars. Resolving the stellar components requires a telescope with an aperture of 8 in (20 cm) or greater. In a 10 in (25 cm) scope, the granular core shows a diameter of 3′ (arcminutes) surrounded by a 10′ halo of stars.

<span class="mw-page-title-main">Messier 30</span> Globular cluster in the constellation Capricornus

Messier 30 is a globular cluster of stars in the southeast of the southern constellation of Capricornus, at about the declination of the Sun when the latter is at December solstice. It was discovered by the French astronomer Charles Messier in 1764, who described it as a circular nebula without a star. In the New General Catalogue, compiled during the 1880s, it was described as a "remarkable globular, bright, large, slightly oval." It can be easily viewed with a pair of 10×50 binoculars, forming a patch of hazy light some 4 arcminutes wide that is slightly elongated along the east–west axis. With a larger instrument, individual stars can be resolved and the cluster will cover an angle of up to 12 arcminutes across graduating into a compressed core about one arcminute wide that has further star density within.

<span class="mw-page-title-main">Messier 53</span> Globular cluster in the constellation Coma Berenices

Messier 53 is a globular cluster in the Coma Berenices constellation. It was discovered by Johann Elert Bode in 1775. M53 is one of the more outlying globular clusters, being about 60,000 light-years (18.4 kpc) light-years away from the Galactic Center, and almost the same distance from the Solar System. The cluster has a core radius (rc) of 2.18 pc, a half-light radius (rh) of 5.84 pc, and a tidal radius (rtr) of 239.9 pc.

<span class="mw-page-title-main">Messier 56</span> Globular cluster in the constellation Lyra

Messier 56 is a globular cluster in the constellation Lyra. It was discovered by Charles Messier in 1779. It is angularly found about midway between Albireo and Sulafat. In a good night sky it is tricky to find with large (50–80 mm) binoculars, appearing as a slightly fuzzy star. The cluster can be resolved using a telescope with an aperture of 8 in (20 cm) or larger.

<span class="mw-page-title-main">Messier 62</span> Globular cluster in the constellation Ophiuchus

Messier 62 or M62, also known as NGC 6266 or the Flickering Globular Cluster, is a globular cluster of stars in the south of the equatorial constellation of Ophiuchus. It was discovered in 1771 by Charles Messier, then added to his catalogue eight years later.

<span class="mw-page-title-main">Messier 70</span> Globular cluster in the constellation Sagittarius

Messier 70 or M70, also known as NGC 6681, is a globular cluster of stars to be found in the south of Sagittarius. It was discovered by Charles Messier in 1780. The famous comet Hale–Bopp was discovered near this cluster in 1995.

<span class="mw-page-title-main">NGC 4833</span> Globular cluster in the constellation Musca

NGC 4833 is a globular cluster discovered by Abbe Lacaille during his 1751-1752 journey to South Africa, and catalogued in 1755. It was subsequently observed and catalogued by James Dunlop and Sir John Herschel whose instruments could resolve it into individual stars.

<span class="mw-page-title-main">NGC 3201</span> Globular cluster in the constellation Vela

NGC 3201 is a low galactic latitude globular cluster in the southern constellation of Vela. It has a very low central concentration of stars. This cluster was discovered by James Dunlop on May 28, 1826 and listed in his 1827 catalogue. He described it as "a pretty large pretty bright round nebula, 4′ or 5′ diameter, very gradually condensed towards the centre, easily resolved into stars; the figure is rather irregular, and the stars are considerably scattered on the south".

<span class="mw-page-title-main">NGC 5986</span> Globular cluster in the constellation Lupus

NGC 5986 is a globular cluster of stars in the southern constellation of Lupus, located at a distance of approximately 34 kilolight-years from the Sun. It was discovered by Scottish astronomer James Dunlop on May 10, 1826. John L. E. Dreyer described it as, "a remarkable object, a globular cluster, very bright, large, round, very gradually brighter middle, stars of 13th to 15th magnitude". Its prograde–retrograde orbit through the Milky Way galaxy is considered irregular and highly eccentric. It has a mean heliocentric radial velocity of +100 km/s. The galacto-centric distance is 17 kly (5.2 kpc), which puts it in the galaxy's inner halo.

<span class="mw-page-title-main">NGC 6752</span> Globular cluster in the constellation Pavo

NGC 6752 is a globular cluster in the constellation Pavo. It is the fourth-brightest globular cluster in the sky, after Omega Centauri, 47 Tucanae and Messier 22, respectively. It is best seen from June to October in the Southern Hemisphere.

<span class="mw-page-title-main">NGC 6934</span> Globular cluster in the constellation Delphinus

NGC 6934 is a globular cluster of stars in the northern constellation of Delphinus, about 52 kilolight-years distant from the Sun. It was discovered by the German-born astronomer William Herschel on 24 September 1785. The cluster is following a highly eccentric orbit through the Milky Way along an orbital plane that is inclined by 73° to the galactic plane. It may share a common dynamic origin with NGC 5466. As of 2018, it has been poorly studied.

<span class="mw-page-title-main">NGC 1851</span> Globular cluster in the constellation Columba

NGC 1851 is a relatively massive globular cluster located in the southern constellation of Columba. Astronomer John Dreyer described it as not very bright but very large, round, well resolved, and clearly consisting of stars. It is located 39.5 kilolight-years from the Sun, and 54.1 kilolight-years from the Galactic Center. The cluster is following a highly eccentric orbit through the galaxy, with an eccentricity of about 0.7.

<span class="mw-page-title-main">NGC 362</span> Globular cluster located in the constellation Tucana

NGC 362 is a globular cluster located in the constellation Tucana in the Southern Hemisphere, slightly north of the Small Magellanic Cloud, to which it is completely unrelated. It was discovered on August 1, 1826, by James Dunlop. It is visible to the naked eye in dark skies, and is an impressive sight in a telescope, although it is somewhat overshadowed by its larger and brighter neighbour 47 Tucanae.

<span class="mw-page-title-main">NGC 5694</span> Globular cluster in the constellation Hydra

NGC 5694 is a globular cluster in the constellation Hydra. It was discovered in 1784 by William Herschel.

<span class="mw-page-title-main">NGC 6496</span> Globular cluster in the constellation Scorpius

NGC 6496 is a globular cluster which is in the direction of the Milky Way's galactic bulge based on observations collected with the WFPC2 on board the Hubble Space Telescope. NGC 6496 was originally believed to be a member of the disc system of the Galactic Center, but scientists questioned this classification. It was instead suggested that NGC 6496, together with two other clusters, NGC 6624 and NGC 6637, could be halo clusters with strongly inclined orbits. NGC 6496 lies in the Southern sky at RA=17:59:03.68 and Dec=-44:15:57.4.

<span class="mw-page-title-main">NGC 6541</span> Globular cluster in the constellation Corona Australis

NGC 6541 is a globular cluster in the southern constellation of Corona Australis. It is estimated to be around 14 billion years old.

<span class="mw-page-title-main">NGC 5286</span> Globular cluster in the constellation Centaurus

NGC 5286 is a globular cluster of stars located some 35,900 light years away in the constellation Centaurus. At this distance, the light from the cluster has undergone reddening from interstellar gas and dust equal to E(B – V) = 0.24 magnitude in the UBV photometric system. The cluster lies 4 arc-minutes north of the naked-eye star M Centauri. It was discovered by Scottish astronomer James Dunlop, active in Australia, and listed in his 1827 catalog.

References

  1. ↑ "The two mysterious populations of NGC 2419". www.spacetelescope.org. Retrieved 25 February 2019.
  2. ↑ Shapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters", Harvard College Observatory Bulletin, 849 (849): 11–14, Bibcode:1927BHarO.849...11S.
  3. 1 2 3 4 "NGC 2419". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2006-11-17.
  4. 1 2 3 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. ↑ distance × sin( diameter_angle / 2 ) = 260 ly. radius
  6. 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, arXiv: 1001.4289 , Bibcode:2010MNRAS.404.1203F, doi: 10.1111/j.1365-2966.2010.16373.x , S2CID   51825384.
  7. ↑ http://messier.seds.org/xtra/ngc/n2419.html NGC 4189 at SEDS
  8. 1 2 Ferris, Timothy. Seeing in the Dark. 2002. p. 244
  9. ↑ 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. arXiv: 0904.3329 . Bibcode:2009MNRAS.396.2051B. doi: 10.1111/j.1365-2966.2009.14932.x . S2CID   7956224.
  10. ↑ 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. arXiv: astro-ph/0407346 . Bibcode:2004MNRAS.354..713V. doi: 10.1111/j.1365-2966.2004.08228.x . S2CID   15407602.
  11. ↑ RIPEPI V.; CLEMENTINI G.; DI CRISCIENZO M.; GRECO C.; et al. (2007). "On the remote galactic globular cluster NGC 2419". The Astrophysical Journal. 667 (1): L61–L64. arXiv: 0705.0966 . Bibcode:2007ApJ...667L..61R. doi:10.1086/522000. S2CID   15186576.
  12. ↑ "The two mysterious populations of NGC 2419". www.spacetelescope.org. February 2019. Retrieved 2021-02-25.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.