NGC 4147

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NGC 4147
NGC 4147 HST 10775 R814GB606.png
NGC 4147 by the Hubble Space Telescope
Observation data (J2000 epoch)
Class IX [1]
Constellation Coma Berenices
Right ascension 12h 10m 06.149s [2]
Declination +18° 32′ 31.78″ [2]
Distance 60  kly (19  kpc) [3]
Apparent magnitude (V)10.74 [4]
Apparent dimensions (V)1.730′ × 1.592′ [2]
Physical characteristics
Mass37,200 [5]   M☉
Tidal radius 6.6′ [6]
Metallicity  = −1.78 [4] dex
Estimated age~14 Gyr [7]
Other designationsGCl 18, C 1207+188 [8]
See also: Globular cluster, List of globular clusters

NGC 4147 is the New General Catalogue identifier for a globular cluster of stars in the northern constellation of Coma Berenices. It was discovered by English astronomer William Herschel on March 14, 1784, who described it as "very bright, pretty large, gradually brighter in the middle". [7] With an apparent visual magnitude of 10.7, [4] it is located around 60,000 [3] light years away from the Sun at a relatively high galactic latitude of 77.2°. [6]

This is a relatively small globular cluster, ranking 112th in luminosity among the Milky Way globular cluster population. It is considered an Oosterhoff type I cluster (OoI), despite having a relatively low metallicity. Indeed, it has the lowest metallicity of any OoI cluster known. There are 19 RR Lyrae variable star candidates and as many as 23 blue stragglers. A high proportion of the latter are concentrated near the dense core of the cluster, which is consistent with the idea that blue stragglers form through stellar mergers. [3] [9]

The cluster lies some 70.4 ± 7.5 kly (21.6 ± 2.3 kpc) from the Galactic Center, [6] and is relatively isolated from other globular clusters in the galaxy. [3] The position of this cluster makes it a candidate for association with the Sagittarius tidal stream, and thus it may have been captured by the Milky Way after separation from the Sagittarius Dwarf Spheroidal Galaxy. [6] A contour map of the cluster appears to show S-shaped tidal arms stretching to the north and south for several tidal radii. Such features are predicted for globular clusters that follow elliptical orbits and are near their apogalacticon. [10]

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<span class="mw-page-title-main">NGC 1261</span> Globular cluster in the constellation Horologium

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<span class="mw-page-title-main">NGC 6352</span> Globular cluster in the constellation Ara

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

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<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.

<span class="mw-page-title-main">NGC 6441</span> Globular cluster in Scorpius

NGC 6441 is a globular cluster in the southern constellation of Scorpius. It was discovered by the Scottish astronomer James Dunlop on May 13, 1826, who described it as "a small, well-defined rather bright nebula, about 20″ in diameter". The cluster is located 5 arc minutes east-northeast of the star G Scorpii, and is some 43,000 light-years from the Sun.

<span class="mw-page-title-main">NGC 5053</span> Globular cluster in the constellation Coma Berenices

NGC 5053 is the New General Catalogue designation for a globular cluster in the northern constellation of Coma Berenices. It was discovered by German-British astronomer William Herschel on March 14, 1784 and cataloged as VI-7. In his abbreviated notation, he described it as, "an extremely faint cluster of extremely small stars with resolvable nebula 8 or 10′ diameter, verified by a power of 240, beyond doubt". Danish-Irish astronomer John Louis Emil Dreyer reported in 1888 that the cluster appeared, "very faint, pretty large, irregular round shape, growing very gradually brighter at the middle".

References

  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 3 Skrutskie, Michael F.; Cutri, Roc M.; Stiening, Rae; Weinberg, Martin D.; Schneider, Stephen E.; Carpenter, John M.; Beichman, Charles A.; Capps, Richard W.; Chester, Thomas; Elias, Jonathan H.; Huchra, John P.; Liebert, James W.; Lonsdale, Carol J.; Monet, David G.; Price, Stephan; Seitzer, Patrick; Jarrett, Thomas H.; Kirkpatrick, J. Davy; Gizis, John E.; Howard, Elizabeth V.; Evans, Tracey E.; Fowler, John W.; Fullmer, Linda; Hurt, Robert L.; Light, Robert M.; Kopan, Eugene L.; Marsh, Kenneth A.; McCallon, Howard L.; Tam, Robert; Van Dyk, Schuyler D.; Wheelock, Sherry L. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode:2006AJ....131.1163S. doi:10.1086/498708. ISSN   0004-6256. S2CID   18913331.
  3. 1 2 3 4 Stetson, Peter B.; et al. (December 2005), "Homogeneous Photometry. V. The Globular Cluster NGC 4147", The Publications of the Astronomical Society of the Pacific, 117 (838): 1325–1361, arXiv: astro-ph/0508650 , Bibcode:2005PASP..117.1325S, doi:10.1086/497302, S2CID   119374637.
  4. 1 2 3 Dalessandro, Emanuele; et al. (November 2012), "Ultraviolet Properties of Galactic Globular Clusters with Galex. II. Integrated Colors", The Astronomical Journal, 144 (5): 13, arXiv: 1208.5698 , Bibcode:2012AJ....144..126D, doi:10.1088/0004-6256/144/5/126, S2CID   56419886, 126.
  5. ↑ Kimmig, Brian; et al. (February 2015), "Measuring Consistent Masses for 25 Milky Way Globular Clusters", The Astronomical Journal, 149 (2): 15, arXiv: 1411.1763 , Bibcode:2015AJ....149...53K, doi:10.1088/0004-6256/149/2/53, S2CID   119282444, 53.
  6. 1 2 3 4 Carballo-Bello, Julio A.; et al. (December 2014), "A search for stellar tidal debris of defunct dwarf galaxies around globular clusters in the inner Galactic halo", Monthly Notices of the Royal Astronomical Society, 445 (3): 2971–2993, arXiv: 1409.7390 , Bibcode:2014MNRAS.445.2971C, doi:10.1093/mnras/stu1949.
  7. 1 2 O'Meara, Stephen James (2011), Deep-Sky Companions: The Secret Deep, vol. 4, Cambridge University Press, pp. 225–228, ISBN   978-1139500074.
  8. ↑ "NGC 4147". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2021-02-19.
  9. ↑ Arellano Ferro, A.; et al. (October 2004), "CCD Photometry of the RR Lyrae Stars in NGC4147", Revista Mexicana de Astronomía y Astrofísica, 40: 209–221 (2004), Bibcode:2004RMxAA..40..209A.
  10. ↑ Jordi, K.; Grebel, E. K. (November 2010), "Search for extratidal features around 17 globular clusters in the Sloan Digital Sky Survey", Astronomy and Astrophysics, 522: 23, arXiv: 1008.2966 , Bibcode:2010A&A...522A..71J, doi:10.1051/0004-6361/201014392, S2CID   118505441, A71.


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