Astronomy:ESO 541-13

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ESO 541-13
DESI Legacy Surveys image of ESO 541-13
Observation data (J2000 epoch)
ConstellationCetus
Right ascension 01h 02m 41.74s[1]
Declination−21° 52′ 55.33″[1]
Redshift0.056949[1]
Helio radial velocity17,073 km/s ± 28[1]
Distance821.5 ± 57.5 Mly (251.88 ± 17.64 Mpc)
Group or clusterAbell 133
Characteristics
TypecD;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]

Description

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 x 109 Mʘ.[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. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "NED Search results for ESO 541-13". https://ned.ipac.caltech.edu/byname?objname=LEDA+3727&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Slee, O. B.; Reynolds, J. E. (1984). "Steep-spectrum radio sources in clusters of galaxies - the southern sample." (in en). Publications of the Astronomical Society of Australia 5 (4): 516–529. doi:10.1017/S1323358000017501. ISSN 0066-9997. Bibcode: 1984PASA....5..516S. https://articles.adsabs.harvard.edu/full/1984PASA....5..516S. 
  3. ↑ 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" (in en). American Astronomical Society Meeting Abstracts #245 245: 472.02. Bibcode: 2025AAS...24547202C. https://ui.adsabs.harvard.edu/abs/2025AAS...24547202C/abstract. 
  4. ↑ 4.0 4.1 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" (in en). The Astrophysical Journal 575 (2): 764–778. doi:10.1086/341352. ISSN 0004-637X. Bibcode: 2002ApJ...575..764F. 
  5. ↑ 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" (in en). Astronomy and Astrophysics Supplement Series 82 (2): 279–317. ISSN 0365-0138. Bibcode: 1990A&AS...82..279R. https://articles.adsabs.harvard.edu//full/1990A%26AS...82..279R/0000281.000.html. 
  6. ↑ Burns, Jack O.; Rhee, George; Owen, Frazer N.; Pinkney, Jason (March 1994). "Clumped X-Ray Emission around Radio Galaxies in Abell Clusters" (in en). The Astrophysical Journal 423: 94. doi:10.1086/173792. ISSN 0004-637X. Bibcode: 1994ApJ...423...94B. https://articles.adsabs.harvard.edu//full/1994ApJ...423...94B/0000113.000.html. 
  7. ↑ Hu, E. M.; Cowie, L. L.; Wang, Z. (December 1985). "Long-slit spectroscopy of gas in the cores of X-ray luminous clusters." (in en). The Astrophysical Journal Supplement Series 59: 447–498. doi:10.1086/191081. ISSN 0067-0049. Bibcode: 1985ApJS...59..447H. https://articles.adsabs.harvard.edu//full/1985ApJS...59..447H/0000474.000.html. 
  8. ↑ McNamara, B. R.; Rohanizadegan, Mina; Nulsen, P. E. J. (January 2011). "Are Radio Active Galactic Nuclei Powered by Accretion or Black Hole Spin?" (in en). The Astrophysical Journal 727 (1): 39. doi:10.1088/0004-637X/727/1/39. ISSN 0004-637X. Bibcode: 2011ApJ...727...39M. 
  9. ↑ Loubser, S. I. (March 2014). "Stellar populations in central cluster galaxies: the influence of cooling flows" (in en). Monthly Notices of the Royal Astronomical Society 439 (1): 416–431. doi:10.1093/mnras/stu020. ISSN 0035-8711. 



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