| NGC 6316 | |
|---|---|
 NGC 6316 as seen through the Hubble Space Telescope | |
| Observation data (J2000 epoch) | |
| Class | III[1] |
| Constellation | Ophiuchus |
| Right ascension | 17h 16m 37.42s[2] |
| Declination | −28° 08′ 24.0″[2] |
| Distance | 36.86 ± 0.98 kly (11.3 ± 0.3 kpc)[3] |
| Apparent magnitude (V) | 9.03[2] |
| Apparent dimensions (V) | 4.9′ × 4.9′[1] |
| Physical characteristics | |
| Metallicity | = -0.45[4] -0.87[5] -0.90[3] dex |
| Estimated age | 13.1 ± 0.5 Gyr[3] |
| Notable features | Relatively metal-rich globular cluster |
| Other designations | GCl 57, VDBH 219[2] |
![{\displaystyle {\begin{smallmatrix}\left[{\ce {Fe}}/{\ce {H}}\right]\end{smallmatrix}}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/4c0821bd80891e071c08e7c7ee8e022baedf522c)
NGC 6316 is a globular cluster located in the constellation Ophiuchus. Its Shapley-Sawyer Concentration Class is III, meaning that it has a "strong inner core of stars" and was discovered by the German-born British astronomer William Herschel on 24 May 1784.[6] It is at a distance of about 37,000 light years away from the Earth.[3] NGC 6316 has a metallicity of -0.45,[4] although new studies suggest this cluster to be more metal Poor, with a metallicity of -0.87 [5] and -0.9;[3] this means that its ratio of hydrogen/helium to other elements is only 35% that of the Sun, but still enough to be considered a "metal-rich" globular cluster.[7]
- ^ a b Hartmut Frommert. "NGC 6316 - Hartmut Frommert - SEDS". SEDS. Retrieved 6 February 2017.
- ^ a b c d "NGC 6136". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 6 February 2017.
- ^ a b c d e Deras, Dan; Cadelano, Mario; Ferraro, Francesco R.; Lanzoni, Barbara; Pallanca, Cristina (2023). "Digging into the Galactic Bulge: Stellar Population and Structure of the Poorly Studied Cluster NGC 6316". The Astrophysical Journal. 942 (2): 104. arXiv:2212.03649. Bibcode:2023ApJ...942..104D. doi:10.3847/1538-4357/aca9ce. S2CID 254366515.
- ^ a b William E. Harris. "Catalog of Parameters for Milky Way Globular Clusters". Retrieved 3 February 2017.
- ^ a b Conroy, Charlie; Villaume, alexa; van Dokkum, Pieter G.; Lind, karin (February 2018). "Metal-rich, Metal-poor: Updated Stellar Population Models for Old Stellar Systems". The Astrophysical Journal. 854 (2): 139. arXiv:1801.10185. Bibcode:2018ApJ...854..139C. doi:10.3847/1538-4357/aaab49.
- ^ Seligman, Courtney. "NGC 6316 (= GCL 57)". cseligman. Retrieved 4 October 2015.
- ^ Layden, Andrew C.; Bowes, Benjamin T.; Welch, Douglas L.; Webb, Tracy M. A. (2003). "Variable Stars in Metal-Rich Globular Clusters. II. NGC 6316". The Astronomical Journal. 126 (1): 255–264. arXiv:astro-ph/0304077. Bibcode:2003AJ....126..255L. doi:10.1086/375651. S2CID 8720908.