ESO 541-13
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| ESO 541-13 | |
|---|---|
 DESI Legacy Surveys image of ESO 541-13 | |
| Observation data (J2000 epoch) | |
| Constellation | Cetus |
| Right ascension | 01h 02m 41.74s[1] |
| Declination | −21° 52′ 55.33″[1] |
| Redshift | 0.056949[1] |
| Heliocentric radial velocity | 17,073 km/s ± 28[1] |
| Distance | 821.5 ± 57.5 Mly (251.88 ± 17.64 Mpc) |
| Group or cluster | Abell 133 |
| magnitude (J) | 11.64[1] |
| Characteristics | |
| Type | cD;E+3 pec[1] |
| Size | ~840,000 ly (257.53 kpc) (estimated)[1] |
| Other designations | |
| 2MASX J01024177-2152557, ESO 541-G013, G4Jy 0113, PGC 3727, MCG -04-03-044[1] | |
ESO 541-13 is a supergiant type-cD galaxy located in the constellation of Cetus. The redshift of the galaxy is (z) 0.056[1] and it was first discovered as a radio source in 1984, that is found to contain a steep radio spectrum, with the galaxy itself being coincident with the center of the radio component.[2] It is the brightest cluster galaxy of the galaxy cluster, Abell 133.[3]
ESO 541-13 is a Type-cD galaxy dominating the center of Abell 133. It is also a radio galaxy, with its source found mainly compact and is separated into four different components of which two of them are associated with the galaxy itself.[4][5] The source is also classified as having a steep spectrum and has an amorphous appearance. An extension feature is also found south of the radio lobe feature of the source.[6] There are also detections of radio emission that is mainly confined within the nucleus region by only a few arcseconds.[7]
Observations made with Chandra X-ray Observatory found there is a tongue of emission described as extending outwards from the galaxy towards the northwest direction where it is found to overlap together with a radio relic, although partly. Evidence also showed the emission is also of thermal type, originating from cool interstellar gas. This is found likely to be produced through Kelvin-Helmholtz instabilities between the cold gas of the galaxy and also the hot intracluster medium.[4] The central supermassive black hole of the galaxy is estimated to be 3.0 × 109 M☉.[8]
Evidence found the galaxy has hydrogen-alpha emission described as extended. The stellar population of the galaxy is mainly made up of two types; stars with an upper limit of around 20 billion years old and very young stars that are less than 100 million years old, with them contributing the light at 20%.[9]
References
- 1 2 3 4 5 6 7 8 9 "NED Search results for ESO 541-13". NASA/IPAC Extragalactic Database. Retrieved 2026-03-01.
- ↑ Slee, O. B.; Reynolds, J. E. (1984). "Steep-spectrum radio sources in clusters of galaxies - the southern sample". Publications of the Astronomical Society of Australia. 5 (4): 516–529. Bibcode:1984PASA....5..516S. doi:10.1017/S1323358000017501. ISSN 0066-9997.
- ↑ Clarke, Tracy; Giacintucci, Simona; Randall, Scott; Osinga, Erik; Van Weeren, Reinout; Cotton, William; Peters, Wendy (January 2025). "Intricate Threads of Abell 133: Unraveling the Complex Thermal Gas and AGN-Induced Outburst in a Cool-Core Cluster". American Astronomical Society Meeting Abstracts #245. 245: 472.02. Bibcode:2025AAS...24547202C.
- 1 2 Fujita, Yutaka; Sarazin, Craig L.; Kempner, Joshua C.; Rudnick, L.; Slee, O. B.; Roy, A. L.; Andernach, H.; Ehle, M. (August 2002). "Chandra Observations of the Disruption of the Cool Core in A133". The Astrophysical Journal. 575 (2): 764–778. arXiv:astro-ph/0204188. Bibcode:2002ApJ...575..764F. doi:10.1086/341352. ISSN 0004-637X.
- ↑ Reuter, H.-P.; Andernach, H. (February 1990). "A Radio Survey of Clusters of Galaxies. VII - 11.1 CM Maps of 20 Abell Clustesr and 6.3 CM Maps of Selected Fields". Astronomy and Astrophysics Supplement Series. 82 (2): 279–317. Bibcode:1990A&AS...82..279R. ISSN 0365-0138.
- ↑ Burns, Jack O.; Rhee, George; Owen, Frazer N.; Pinkney, Jason (March 1994). "Clumped X-Ray Emission around Radio Galaxies in Abell Clusters". The Astrophysical Journal. 423: 94. Bibcode:1994ApJ...423...94B. doi:10.1086/173792. ISSN 0004-637X.
- ↑ Hu, E. M.; Cowie, L. L.; Wang, Z. (December 1985). "Long-slit spectroscopy of gas in the cores of X-ray luminous clusters". The Astrophysical Journal Supplement Series. 59: 447–498. Bibcode:1985ApJS...59..447H. doi:10.1086/191081. ISSN 0067-0049.
- ↑ McNamara, B. R.; Rohanizadegan, Mina; Nulsen, P. E. J. (January 2011). "Are Radio Active Galactic Nuclei Powered by Accretion or Black Hole Spin?". The Astrophysical Journal. 727 (1): 39. arXiv:1007.1227. Bibcode:2011ApJ...727...39M. doi:10.1088/0004-637X/727/1/39. ISSN 0004-637X.
- ↑ Loubser, S. I. (March 2014). "Stellar populations in central cluster galaxies: the influence of cooling flows". Monthly Notices of the Royal Astronomical Society. 439 (1): 416–431. arXiv:1401.1822. doi:10.1093/mnras/stu020. ISSN 0035-8711.
External links
- ESO 541-13 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
