Messier 30

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Messier 30
M30 NASA.jpg
Open cluster Messier 30 in Capricornus
Observation data (J2000 epoch)
Class V [1]
Constellation Capricornus
Right ascension 21h 40m 22.12s [2]
Declination –23° 10′ 47.5″ [2]
Distance 27.14 ± 0.65  kly (8.3 ± 0.20  kpc) [3] [4]
Apparent magnitude (V)7.2 [5]
Apparent dimensions (V)12'.0
Physical characteristics
Mass1.6×105 [6]   M☉
Metallicity  = –2.27 [7] dex
Estimated age12.93  Gyr [8]
Other designationsM30, NGC 7099, GCl 122 [9]
See also: Globular cluster, List of globular clusters

Messier 30 (also known as M30, NGC 7099, or the Jellyfish Cluster) 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. [a] 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, [10] forming a patch of hazy light some 4  arcminutes wide that is slightly elongated along the east–west axis. [10] 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. [11]

Contents

It is longest observable (opposed to the Sun) in the first half of August. [b] [10]

M30 is centered 27,100 light-years away from Earth with a roughly 2.5% margin of error, [4] and is about 93 light-years across. [11] The estimated age is roughly 12.9 billion years [8] and it forms a mass of about 160,000 times the mass of the Sun (M☉). [6] The cluster is following a retrograde orbit (against the general flow) through the inner galactic halo, suggesting that it was acquired from a satellite galaxy rather than forming within the Milky Way. [8] It is in this epoch 22.2 kly (6.8 kpc), from the center of the galaxy, compared to an estimated 26 kly (8.0 kpc) for the Sun. [12]

The cluster has passed through a dynamic process called core collapse and now has a concentration of mass at its core of about a million times the Sun's mass per cubic parsec. This makes it one of the highest density regions in the Milky Way galaxy. Stars in such close proximity will experience a high rate of interactions that can create binary star systems, as well as a type of star called a blue straggler that is formed by mass transfer. [3] A process of mass segregation may have caused the central region to gain a greater proportion of higher mass stars, creating a color gradient with increasing blueness toward the middle of the cluster. [13]

Masp showing the location of M30 M30map.png
Masp showing the location of M30


See also

References and footnotes

  1. ↑ Shapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters", Harvard College Observatory Bulletin, 849 (849): 11–14, Bibcode:1927BHarO.849...11S.
  2. 1 2 Goldsbury, Ryan; et al. (December 2010), "The ACS Survey of Galactic Globular Clusters. X. New Determinations of Centers for 65 Clusters", The Astronomical Journal, 140 (6): 1830–1837, arXiv: 1008.2755 , Bibcode:2010AJ....140.1830G, doi:10.1088/0004-6256/140/6/1830, S2CID   119183070.
  3. 1 2 Lugger, Phyllis M.; et al. (March 2007), "Chandra X-Ray Sources in the Collapsed-Core Globular Cluster M30 (NGC 7099)", The Astrophysical Journal, 657 (1): 286–301, arXiv: astro-ph/0606382 , Bibcode:2007ApJ...657..286L, doi:10.1086/507572, S2CID   14188771
  4. 1 2 Kains, N.; et al. (2016), "Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry", Astronomy and Astrophysics, 555 (1): 36–50, arXiv: 1305.3606 , Bibcode:2013A&A...555A..36K, doi:10.1051/0004-6361/201321819, S2CID   53669510
  5. ↑ "Messier 30". SEDS Messier Catalog. Retrieved 22 July 2024.
  6. 1 2 Vande Putte, D.; Cropper, Mark (January 2009), "Detecting the effect of globular cluster impacts on the disc of the Milky Way", Monthly Notices of the Royal Astronomical Society, 392 (1): 113–124, arXiv: 0811.3106 , Bibcode:2009MNRAS.392..113V, doi: 10.1111/j.1365-2966.2008.14072.x , S2CID   17244698
  7. ↑ Boyles, J.; et al. (November 2011), "Young Radio Pulsars in Galactic Globular Clusters", The Astrophysical Journal, 742 (1): 51, arXiv: 1108.4402 , Bibcode:2011ApJ...742...51B, doi:10.1088/0004-637X/742/1/51, S2CID   118649860.
  8. 1 2 3 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
  9. ↑ "M 30". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 16 November 2006.
  10. 1 2 3 Bone, N. M. (August 2008), "Sky notes, 2008 August & September", Journal of the British Astronomical Association, 118 (4): 231–232, Bibcode:2008JBAA..118..231B
  11. 1 2 O'Meara, Stephen James (1998), The Messier objects, Deep-sky companions, Cambridge University Press, p. 108, ISBN   978-0-521-55332-2
  12. ↑ Dinescu, Dana I.; et al. (January 1999), "Space Velocities of Southern Globular Clusters. II. New Results for 10 Clusters", The Astronomical Journal, 117 (1): 277–285, Bibcode:1999AJ....117..277D, doi: 10.1086/300699
  13. ↑ Howell, Justin H.; Guhathakurta, Puragra; Tan, Amy (March 2000), "Radial Color Gradient and Main-Sequence Mass Segregation in M30 (NGC 7099)", The Astronomical Journal, 119 (3): 1259–1267, arXiv: astro-ph/9912002 , Bibcode:2000AJ....119.1259H, doi:10.1086/301270, S2CID   15083719

Notes

  1. ↑ Thus, its northern limit for good visibility is a few degrees south of the Arctic Circle, all year
  2. ↑ This is when it is risen, throughout the night, so culminates about midnight. The Earth's orbit means the sun leaves Capricornus, as if it heads east a few degrees NNE, on about 15 or 16 February, having figured in the constellation for a month.
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