Summary
NGC 6496 is a globular cluster which is in the direction of the Milky Way's galactic bulge based on observations collected with the WFPC2 on board the Hubble Space Telescope. NGC 6496 was originally believed[who?] to be a member of the disc system of the Galactic Center, but scientists questioned this classification. It was instead suggested[who?] that NGC 6496, together with two other clusters, NGC 6624 and NGC 6637, could be halo clusters with strongly inclined orbits. NGC 6496 lies in the Southern sky at RA=17:59:03.68 and Dec=-44:15:57.4.[6]
| NGC 6496 | |
|---|---|
 Processed Hubble Space Telescope image of the globular cluster | |
| Observation data | |
| Class | XII[1] |
| Constellation | Scorpius |
| Right ascension | 17h 59m 03.68s[2] |
| Declination | −44° 15′ 57.4″[2] |
| Distance | 36.9 kly (11.3 kpc)[3] |
| Apparent dimensions (V) | 5.6' |
| Physical characteristics | |
| Mass | 8.2×104[4] M☉ |
| Metallicity | = –0.70[5] dex |
| Estimated age | 12.42 Gyr[5] |
![{\displaystyle {\begin{smallmatrix}\left[{\ce {Fe}}/{\ce {H}}\right]\end{smallmatrix}}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/4c0821bd80891e071c08e7c7ee8e022baedf522c)
The first CMD presented of NGC 6496 had photometry reaching 2 mag below the horizontal branch, disclosing for the first time the usual red arm of the metal-rich clusters. The extinction towards NGC 6496 is uncertain, with estimates ranging between and .[7]
The cluster has a relatively metal-rich composition of [Fe/H] = –0.46 dex and is of an open, uncrowded nature. Few attempts were made to find variable stars in NGC 6496. In one of the studies, thirteen variable stars were detected by Dr. Moe Abbas and Dr. Andrew Layden from Bowling Green State University.[8]
Gallery edit
![NGC 6496 hosts a selection of long-period variables and short-period eclipsing binaries.[9]](http://upload.wikimedia.org/wikipedia/commons/thumb/a/a4/A_heavy-metal_home.jpg/120px-A_heavy-metal_home.jpg)
References edit
- ^ 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 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.
- ^ 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.
- ^ Marks, Michael; Kroupa, Pavel (August 2010), "Initial conditions for globular clusters and assembly of the old globular cluster population of the Milky Way", Monthly Notices of the Royal Astronomical Society, 406 (3): 2000–2012, arXiv:1004.2255, Bibcode:2010MNRAS.406.2000M, doi:10.1111/j.1365-2966.2010.16813.x, S2CID 118652005. Mass is from MPD on Table 1.
- ^ a b 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.
- ^ Richtler, T; Grebel, E (1994). "The cases of the "disk" globular clusters NGC 6496, NGC 6624, and NGC 6637". Astronomy and Astrophysics. 290: 412–420. Bibcode:1994A&A...290..412R.
- ^ Armandroff, Taft E. (1988). "Color-magnitude diagrams for six metal-rich, low-latitude globular clusters". The Astronomical Journal. 96: 588. Bibcode:1988AJ.....96..588A. doi:10.1086/114833.
- ^ Abbas, Moe; et al. (February 2015), "Variable Stars in Metal-Rich Globular Clusters. IV. Long-Period Variables in NGC 6496", The Astronomical Journal, 149 (2): 40, arXiv:1410.3305, Bibcode:2015AJ....149...40A, doi:10.1088/0004-6256/149/2/40, S2CID 118503316.
- ^ "A heavy-metal home". Retrieved 30 May 2016.
External links edit
Media related to NGC 6496 at Wikimedia Commons
