Messier 107
Messier 107 | |
---|---|
| |
Observation data (J2000 epoch) | |
Class | X[1] |
Right ascension | 16h 32m 31.86s[2] |
Declination | –13° 03′ 13.6″[2] |
Distance | 20.9 kly (6.4 kpc)[3] |
Apparent magnitude (V) | +8.85[4] |
Apparent dimensions (V) | 13′.0 |
Physical characteristics | |
Mass | ×105 1.82[3] M☉ |
Radius | 39.5 ly[5] |
Metallicity | = –0.95[6] dex |
Estimated age | 13.95 Gyr[6] |
Other designations | NGC 6171, GCl 44[4] |
Wikimedia Commons has media related to Messier 107. |
Globular Cluster M107 (also known as Messier Object 107 or NGC 6171) is the last globular cluster in the Messier Catalogue. It is a very loose globular cluster in the constellation Ophiuchus. It was discovered by Pierre Méchain in April 1782 and independently by William Herschel in 1793. It was not until 1947 that Helen Sawyer Hogg added it and three other objects discovered by Méchain to the list of Messier objects.
M107 is close to the galactic plane at a distance of about 20,900 light-years from Earth.[3] There are 25 known variable stars in this cluster.
Gallery
- The globular star cluster Messier 107 image taken by the Wide Field Imager (WFI) on the MPG/ESO 2.2-metre telescope.
- Map showing the location of M107.
See also
- New General Catalogue
- Wikipedia Project: Astronomical Objects
References
- ↑ Shapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters", Harvard College Observatory Bulletin (849): 11–14, Bibcode:1927BHarO.849...11S.
- 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.
- 1 2 3 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.
- 1 2 "NGC 6171". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2006-11-16.
- ↑ distance × sin( diameter_angle / 2 )=39.5 ly. radius
- 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.
External links
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