MCG-02-12-039
From Wikipedia, the free encyclopedia
| MCG-02-12-039 | |
|---|---|
 The galaxy MCG-02-12-039 | |
| Observation data (J2000 epoch) | |
| Constellation | Eridanus |
| Right ascension | 04h 33m 37.83s [1] |
| Declination | −13° 15′ 42.95″[1] |
| Redshift | 0.032806[1] |
| Heliocentric radial velocity | 9835 km/s ± 11[1] |
| Distance | 468.2 ± 32.8 Mly (143.55 ± 10.05 Mpc)[1] |
| Group or cluster | Abell 496 |
| Apparent magnitude (B) | 14.66[1] |
| Characteristics | |
| Type | cD;E+?[1] |
| Size | ~294,000 ly (90.1 kpc) |
| Other designations | |
| 2MASX J04333784-1315430, ABELL 0496:[ZAC2011] BCG, Cul 0431-133, PGC 15524, GIN 189, NVSS J043337-131542[1] | |
MCG-02-12-039 also known as A496 cD, is an elliptical galaxy located in the constellation of Eridanus. The redshift of the galaxy is (z) 0.032[1] and it was first discovered by a group of astronomers in March 1985. It is classified as a Type-cD galaxy and is the brightest cluster galaxy, of the Abell 496 galaxy cluster.[2]
MCG-02-12-039 is the dominant galaxy of Abell 496.[2] It is known to contain a large galactic halo that is found surrounding it with many distant galaxy companions in the background.[3] It has also been described as a weak emission line galaxy based on a study published in December 2008.[4] There is also strong presence of extended optical emission by around 10 arcseconds from the central nucleus, mainly made up of hydrogen-alpha and singly ionized nitrogen.[5] The estimated equivalent age of a single stellar population in the galaxy is around 1.05 ± 0.21 billion years.[6] In the center of the galaxy, there are three dust lanes that are found to be uncurling in an anticlockwise direction, in a spiral pattern.[7]
Evidence found the halo of the galaxy is found to display a blue profile per each increasing radius based on a B-V color profile. However, when observed in visual infrared colors, the profile is shown to be more redder.[8] There is also a presence of an elongated stellar component with gas components also having the same morphology but to a lesser extent. The central nucleus is found to have its parts blueshifted by around 125 kilometer per seconds.[9]
A study published in 2020 has found the presence of gas filaments in the galaxy. When observed, the gas components are described as stretched suggesting there is a common origin. Moreover, a misalignment is shown between stellar and gas kinematics, hinting interstellar gas is found to be externally accreted.[10] The central supermassive black hole of the galaxy is estimated to be around 8.78 M☉.[11]
References
- 1 2 3 4 5 6 7 8 9 "NED Search results for MCG-02-12-039". NASA/IPAC Extragalactic Database. Retrieved 2026-02-21.
- 1 2 Quintana, H.; Melnick, J.; Infante, L.; Thomas, B. (March 1985). "Optical studies of X-ray clusters of galaxies. IV. Velocity dispersions for the cD clusters A496 and A2052". The Astronomical Journal. 90: 410–413. doi:10.1086/113746. ISSN 0004-6256.
- ↑ Vorontsov-Vel'Yaminov, B. A.; Arkhipova, V. P. (1968). "Morphological catalogue of galaxies. Part IV. Catalogue of 5410 galaxies between declinations -9 and -33". Trudy Gosudarstvennogo Astronomicheskogo Instituta. 38: 1–206. ISSN 0371-6791.
- ↑ Loubser, S. I.; Sansom, A. E.; Sánchez-Blázquez, P.; Soechting, I. K.; Bromage, G. E. (December 2008). "Radial kinematics of brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society. 391 (3): 1009–1028. arXiv:0808.1521. doi:10.1111/j.1365-2966.2008.13813.x. ISSN 0035-8711.
- ↑ Fisher, David; Illingworth, Garth; Franx, Marijn (January 1995). "Kinematics of 13 brightest cluster galaxies". The Astrophysical Journal. 438: 539. doi:10.1086/175100. ISSN 0004-637X. Archived from the original on 2023-09-30.
- ↑ Loubser, S. I.; Sánchez-Blázquez, P.; Sansom, A. E.; Soechting, I. K. (2009-09-01). "Stellar populations in the centres of brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society. 398 (1): 133–156. arXiv:0906.0287. doi:10.1111/j.1365-2966.2009.15171.x. ISSN 0035-8711. Archived from the original on 2024-06-20.
- ↑ Hatch, N. A.; Crawford, C. S.; Fabian, A. C. (2007-08-04). "Ionized nebulae surrounding brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society. 380 (1): 33–43. arXiv:0706.0661. doi:10.1111/j.1365-2966.2007.12009.x. ISSN 0035-8711. Archived from the original on 2024-07-28.
- ↑ A., Valentijn, E.; Moorwood, A. F. M. (February 1985). "The stellar content of the A 496 cD galaxy". Astronomy and Astrophysics. 143. ISSN 0004-6361. Archived from the original on 2024-11-13.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ↑ Loubser, S. I.; Soechting, I. K. (2013-03-04). "The detailed nature of active central cluster galaxies". arXiv.org. Retrieved 2026-02-21.
- ↑ Pagotto, Ilaria; Krajnović, Davor; Brok, Mark den; Emsellem, Eric; Brinchmann, Jarle; Weilbacher, Peter M.; Kollatschny, Wolfram; Steinmetz, Matthias (2021-05-01). "Optical emission lines in the most massive galaxies: Morphology, kinematics, and ionisation properties" (PDF). Astronomy & Astrophysics. 649: A63. doi:10.1051/0004-6361/202039443. ISSN 0004-6361.
- ↑ Bettoni, D.; Falomo, R.; Fasano, G.; Govoni, F. (2003-02-14). "The black hole mass of low redshift radiogalaxies". Astronomy & Astrophysics. 399 (3): 869–878. arXiv:astro-ph/0212162. doi:10.1051/0004-6361:20021869. ISSN 0004-6361. Archived from the original on 2024-11-30.
External links
- MCG-02-12-039 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
