16h 32m 31.91s, −13° 03′ 13.1″Messier 107
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| Messier 107 | |
|---|---|
| Lua error in package.lua at line 80: module 'Module:InfoboxImage/data' not found. M107 from Hubble Space Telescope; 3.5Template:Prime view | |
| Observation data (J2000 epoch) | |
| Class | X[1] |
| Right ascension | Template:RA[2] |
| Declination | Template:DEC[2] |
| Distance | 20.9 kly (6.4 kpc)[3] |
| Apparent magnitude (V) | 7.9[4] |
| Apparent dimensions (V) | 10′[5] |
| Physical characteristics | |
| Mass | 1.82×105[3] M☉ |
| Radius | 30 ly[6] |
| Metallicity | [Fe/H] = –0.95[7] dex |
| Estimated age | 13.95 Gyr[7] |
| Other designations | C 1629-129, GCl 44, M 107, NGC 6171[8] |
Messier 107 or M107, also known as NGC 6171 or the Crucifix Cluster, is a very loose globular cluster close to the equator in Ophiuchus, and is the last such object in the Messier Catalogue.
Observational history, namings and guide
It was discovered by Pierre Méchain in April 1782, then independently by William Herschel in 1793. Herschel's son, John, in his 1864 General Catalogue, described it as a "globular cluster of stars, large, very rich, very much compressed, round, well resolved, clearly consisting of stars".[5] It was not until 1947 that Helen Sawyer Hogg added it and three other objects found by Méchain to the modern Catalogue, the latter having contributed several of the suggested observation objects which Messier had verified and added.[9] The cluster is to be found 2.5° south and slightly west of the star Zeta Ophiuchi.[5]
Properties
M107 is close to the galactic plane and about 20,900 light-years from Earth[3] and 9,800 ly (3,000 pc) from the Galactic Center.[10] Its orbit is partly as far out as the galactic halo, as is between 9,200–12,400 ly (2,820–3,790 pc) from the Galactic Center, the lower figure, the "perigalactic distance" sees it enter and leave the galactic bar.[11] There are 22 known RR Lyrae variable stars in this cluster and a probable SX Phoenicis variable.[12]
See also
References and footnotes
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- ^ Page Module:Citation/CS1/styles.css has no content.Shapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters", Harvard College Observatory Bulletin, 849 (849): 11–14, Bibcode:1927BHarO.849...11S.
- ^ a b Page Module:Citation/CS1/styles.css has no content.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.
- ^ a b c Page Module:Citation/CS1/styles.css has no content.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.
- ^ Page Module:Citation/CS1/styles.css has no content."Messier 107". SEDS Messier Catalog. Retrieved 30 April 2022.
- ^ a b c Page Module:Citation/CS1/styles.css has no content.Mullaney, James (2007), The Herschel Objects and How to Observe Them, Astronomers' Observing Guides, Springer Science & Business Media, p. 94, Bibcode:2007hoho.book.....M, ISBN 978-0387681252.
- ^ From trigonometry: distance × sin( diameter_angle / 2 ) = 39.5 ly. radius
- ^ a b Page Module:Citation/CS1/styles.css has no content.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.
- ^ Page Module:Citation/CS1/styles.css has no content."NGC 6171". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2006-11-16.
{{cite web}}: Invalid|mode=Script error: No such module "Citation mode".(help) - ^ Page Module:Citation/CS1/styles.css has no content.Frommert, Hartmut; Kronberg, Christine (August 30, 2007), "Messier 107", SEDS Messier pages, Students for the Exploration and Development of Space (SEDS), retrieved 2018-12-07.
- ^ Page Module:Citation/CS1/styles.css has no content.Zinn, R. (June 15, 1985), "The globular cluster system of the galaxy. IV - The halo and disk subsystems", Astrophysical Journal, Part 1, 293: 424–444, Bibcode:1985ApJ...293..424Z, doi:10.1086/163249.
- ^ Page Module:Citation/CS1/styles.css has no content.Pichardo, Bárbara; et al. (July 2004), "Models for the Gravitational Field of the Galactic Bar: An Application to Stellar Orbits in the Galactic Plane and Orbits of Some Globular Clusters", The Astrophysical Journal, 609 (1): 144–165, arXiv:astro-ph/0402340, Bibcode:2004ApJ...609..144P, doi:10.1086/421008, S2CID 16356464.
- ^ Page Module:Citation/CS1/styles.css has no content.McCombs, Thayne; et al. (January 2013), "Variable Stars in the Globular Cluster M107: The Discovery of a Probable SX Phoenicis", AAS Meeting #221, vol. 221, American Astronomical Society, p. 250.22, Bibcode:2013AAS...22125022M, 250.22.
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External links
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