| NGC 2158 | |
|---|---|
 | |
| Observation data (J2000 epoch) | |
| Right ascension | 06h 07m 25s[1] |
| Declination | +24° 05.8′[1] |
| Distance | 11,000+ ly[2] (3600±400 pc) |
| Apparent magnitude (V) | 8.6[1] |
| Apparent dimensions (V) | 5 arcmin[2] |
| Physical characteristics | |
| Mass | 3067 ±69.84 M☉ |
| Radius | 8 ly |
| Estimated age | ~2 billion yrs[2] |
| Other designations | OCL 468, Lund 206, Melotte 40 |
| Associations | |
| Constellation | Gemini |
| Galaxy | Milky Way |
NGC 2158, also known as OCL 468, Lund 206 or Melotte 40, it is an open cluster of stars located around 11,000 light years (3600 ±400 pc) from Earth in the constellation of Gemini. It is of intermediate age being around 2 billion years old. The cluster is populous with stars containing some 3000 ±69 stars within a radius of about 8 light years.[2]
It is, in angle, immediately southwest of open cluster Messier 35. The two clusters are unrelated, as the subject is around 9,000 light years further away.[2]
History
Once thought to be a globular cluster, it is now known to be a metal-poor open cluster that is a member of the old thin disk population. It was first classed as such by Trumpler but later Sharpely would open cluster due to its diffuse core.[3] NGC 2158 has been studied numerous times. A study from Arp & Cuffey (1962) was the first study of NGC 2158 obtaining photographic photometry for about 900 stars and determine the cluster to be an intermediate between regular star clusters and globular clusters. Later, the photometry of more than 2000 stars would be obtained by Karchenko, Andruk & Schilbach (1997).[2][4]
Properties
NGC 2158 has unusual properties for an open cluster (OC). Its rich stellar content (only with suitable equipment can spaces between the stars be seen) and brightness initially makes it appear as a globular cluster (GC). It also has a red giant population similar to GCs. However it is not and is rather an intermediate object between globular clusters and regular star clusters.[4]
The cluster has anomalously low amount of metals making it metal-poor. It has been estimated that NGC 2158 is around 2 billion years old. This would make the cluster of intermediate-age.[2]
Contents
NGC 2158 is a populous cluster with many low to intermediate mass stars. NGC 2158 has three mass regimes: high mass stars, low mass stars and very low mass stars. Data used from the third edition of the Gaia Data Release (DR3) revealed that there are 3067 ±69.84 stars totaling to a mass of 3216.4 ±59.50 solar masses.[5] There is a red giant population.[4] The cluster also has a M-dwarf discontinuity.[6] It also contains a cataclysmic variable (CV) star (the fourth known to exist in a open cluster) and five Delta Scuti variables (δ Scuti).[7]
Due to the distance of NGC 2158, most binary systems that survived inside the dense environment are unable to be resolved. Instead, these systems appear as point-like sources with the exception of wide binary systems which can be resolved as two distinct sources.[6]
Additional images
References
- ^ a b c "SIMBAD Astronomical Database". Results for NGC 2158. Retrieved 2010-08-31.
- ^ a b c d e f g Carraro, Giovanni; Girardi, Leo; Marigo, Paola (2002). "The intermediate-age open cluster NGC 2158". Monthly Notices of the Royal Astronomical Society. 332 (3): 705. arXiv:astro-ph/0202018. Bibcode:2002MNRAS.332..705C. doi:10.1046/j.1365-8711.2002.05326.x. S2CID 15054623.
- ^ Ahmed, Nasser M.; Tadross, A. L. (2025-06-20). "Precision analysis of NGC 2158 with Gaia DR3". Scientific Reports. 15 (1): 20189. doi:10.1038/s41598-025-06119-1. ISSN 2045-2322.
- ^ a b c Arp, H.; Cuffey, J. (1962-07-01). "The star cluster NGC 2158". The Astrophysical Journal. 136: 51. doi:10.1086/147350. ISSN 0004-637X. Archived from the original on 2022-04-04.
- ^ Ahmed, Nasser M.; Tadross, A. L. (2025-06-20). "Precision analysis of NGC 2158 with Gaia DR3". Scientific Reports. 15 (1): 20189. doi:10.1038/s41598-025-06119-1. ISSN 2045-2322.
- ^ a b Marchuk, A. V.; Muratore, F.; Milone, A. P.; Legnardi, M. V.; D'Antona, F.; Cordoni, G.; Mastrobuono-Battisti, A.; Bortolan, E.; Dell'Agli, F. (2026-02-25), A deep HST view of the open cluster NGC2158: binaries, mass functions, and M-dwarf discontinuity, arXiv, doi:10.48550/arXiv.2602.21882, arXiv:2602.21882, retrieved 2026-03-06
- ^ Mochejska, B. J.; Stanek, K. Z.; Sasselov, D. D.; Szentgyorgyi, A. H.; Westover, M.; Winn, J. N. (2004-07-01). "Planets in Stellar Clusters Extensive Search. II. Discovery of 57 Variables in the Cluster NGC 2158 with Millimagnitude Image Subtraction Photometry". The Astronomical Journal. 128 (1): 312–322. doi:10.1086/420992. ISSN 0004-6256.
External links
Media related to NGC 2158 at Wikimedia Commons- NGC 2158 (SEDS)
- NGC 2158 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
- NASA Astronomy Picture of the Day: Open Star Clusters M35 and NGC 2158 (2003 December 15)
| Stars |
| ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||||
| Star clusters |
| ||||||||||||
| |||||||||||||
| Galaxies |
| ||||||||||||
| |||||||||||||
 | This star cluster–related article is a stub. You can help Wikipedia by adding missing information. |
