NGC 6316

In this article, we will approach NGC 6316 from different angles, with the aim of providing a broad and detailed view on this topic. NGC 6316 is a topic of great relevance today, since it impacts various aspects of society, the economy, politics, culture and people's daily lives. Through rigorous and in-depth analysis, we will explore the different facets of NGC 6316, examining its implications, challenges and opportunities. Through this article, we aim to offer the reader a comprehensive and enriching perspective that allows them to better understand the importance and scope of NGC 6316 in the contemporary world.

NGC 6316
NGC 6316 as seen through the Hubble Space Telescope
Observation data (J2000 epoch)
ClassIII[1]
ConstellationOphiuchus
Right ascension17h 16m 37.42s[2]
Declination−28° 08′ 24.0″[2]
Distance36.86 ± 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 age13.1 ± 0.5 Gyr[3]
Notable featuresRelatively metal-rich globular cluster
Other designationsGCl 57, VDBH 219[2]
See also: Globular cluster, List of globular clusters

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]

See also

References

  1. ^ a b Hartmut Frommert. "NGC 6316 - Hartmut Frommert - SEDS". SEDS. Retrieved 6 February 2017.
  2. ^ a b c d "NGC 6136". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 6 February 2017.
  3. ^ 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.
  4. ^ a b William E. Harris. "Catalog of Parameters for Milky Way Globular Clusters". Retrieved 3 February 2017.
  5. ^ 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.
  6. ^ Seligman, Courtney. "NGC 6316 (= GCL 57)". cseligman. Retrieved 4 October 2015.
  7. ^ 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.
  • Media related to NGC 6316 at Wikimedia Commons


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