Astronomy:ZwCl 8193 BCG

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ZwCl 8193 BCG
File:Image of ZwCl 8193 BCG.png
SDSS image of ZwCl 8193 BCG
Observation data (J2000.0 epoch)
ConstellationHercules
Right ascension 17h 17m 19.20s[1]
Declination+42° 26′ 59.84″[1]
Redshift0.182900[1]
Helio radial velocity54,832 ± 30 km/s[1]
Distance2,648.4 ± 185.4 Mly (812.00 ± 56.84 Mpc)[1]
Group or clusterZwCl 8193
Characteristics
TypeBrClG;AGN blazar[1]
Size~714,500 ly (219.08 kpc) (estimated)[1]
Other designations
2MASX J17171926+4226571, NVSS J171719+422659, LEDA 93954, OCARS 1715+425, OGC 0022, RX J1717.2+4226, WHL J171719.2+422657 BCG[1]

ZwCl 8193 BCG (Short for ZwCl 8193 Brightest Cluster Galaxy) is a massive elliptical galaxy residing as the brightest cluster galaxy of the galaxy cluster, ZwCl 8193.[2] The redshift of the galaxy is (z) 0.182[1] and it was first discovered by astronomers in July 1999, who found the galaxy displays emission lines in its optical spectrum.[3]

Description

ZwCl 8193 BCG is categorized as an elliptical galaxy inside a rich galaxy environment. The galaxy has a disturbed appearance. indicating it is undergoing multiple ongoing galaxy mergers. There is also evidence that there is in the outskirts of the BCG a tidally disrupted galaxy, based on the presence of clumpy bright far-ultraviolet and hydrogen alpha emission that is arranged in a spiral formation. A nuclear bulge is present in the BCG according to optical and 3 ɥm imaging.[4] The total infrared star formation rate is estimated to be 59 Mʘ per year. There is a possible double nucleus.[5]

The BCG contains an active galactic nucleus (AGN), with an estimated radio power of 25.29 W Hz-1.[6] There is a radio source called B3 1715+425 that was originally associated with the BCG, but later reclassified as a tidally stripped radio galaxy or a nearly naked black hole located 8.5 kiloparsecs away from the BCG's central nucleus. The interaction with the BCG likely caused immense tidal forces to a point where the galaxy's outer portion was eventually pulled away, leaving only a small portion of it.[2] The radio luminosity for the BCG itself is 41.61 ± 0.005 erg s-1 at 5 GHz frequencies.[7]

A study published in 2002, reported detections of molecular hydrogen in the BCG. The total molecular mass is estimated to be less than 4.3 × 1010 Mʘ and the molecular line luminosity is approximately 1.1 ± 0.1 × 1041 erg s-1.[8] A carbon oxide line survey also found cold molecular gas in the BCG based on presence of line detections, with the line positions being -14 ± 20 kilometers per seconds and has line widths of 242 ± 65 kilometers per second. The dust mass has been calculated as 3.8 × 107 Mʘ.[9] One of the hydrogen-alpha emission blobs is centered on the BCG.[10] A central supermassive black hole mass of 10.04 ± 0.05 Mʘ has been calculated for the BCG based on its K-band bulge luminosity.[7]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 "NED Search results for ZwCl 8193 BCG (LEDA 93954)". https://ned.ipac.caltech.edu/byname?objname=LEDA+93954&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ 2.0 2.1 Condon, J. J.; Darling, Jeremy; Kovalev, Y. Y.; Petrov, L. (2017-01-10). "A Nearly Naked Supermassive Black Hole". The Astrophysical Journal 834 (2): 184. doi:10.3847/1538-4357/834/2/184. ISSN 0004-637X. Bibcode: 2017ApJ...834..184C. 
  3. ↑ Crawford, C. S.; Allen, S. W.; Ebeling, H.; Edge, A. C.; Fabian, A. C. (1999-07-11). "The ROSAT Brightest Cluster Sample -- III. Optical spectra of the central cluster galaxies". Monthly Notices of the Royal Astronomical Society 306 (4): 857–896. doi:10.1046/j.1365-8711.1999.02583.x. ISSN 0035-8711. Bibcode: 1999MNRAS.306..857C. 
  4. ↑ O'Dea, Kieran P.; Quillen, Alice C.; O'Dea, Christopher P.; Tremblay, Grant R.; Snios, Bradford T.; Baum, Stefi A.; Christiansen, Kevin; Noel-Storr, Jacob et al. (2010-08-02). "HUBBLE SPACE TELESCOPE FAR-ULTRAVIOLET OBSERVATIONS OF BRIGHTEST CLUSTER GALAXIES: THE ROLE OF STAR FORMATION IN COOLING FLOWS AND BCG EVOLUTION". The Astrophysical Journal 719 (2): 1619–1632. doi:10.1088/0004-637x/719/2/1619. ISSN 0004-637X. Bibcode: 2010ApJ...719.1619O. https://doi.org/10.1088/0004-637x/719/2/1619. 
  5. ↑ Tremblay, G. R.; O'Dea, C. P.; Baum, S. A.; Mittal, R.; McDonald, M. A.; Combes, F.; Li, Y.; McNamara, B. R. et al. (2015-06-29). "Far-ultraviolet morphology of star-forming filaments in cool core brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society 451 (4): 3768–3800. doi:10.1093/mnras/stv1151. ISSN 0035-8711. https://academic.oup.com/mnras/article/451/4/3768/1105719. 
  6. ↑ Caccianiga, A.; Marchã, M.J.; Antón, S.; Mack, K.-H.; Neeser, M.J. (February 2002). "The CLASS blazar survey — II. Optical properties". Monthly Notices of the Royal Astronomical Society 329 (4): 877–889. doi:10.1046/j.1365-8711.2002.05062.x. ISSN 0035-8711. Bibcode: 2002MNRAS.329..877C. 
  7. ↑ 7.0 7.1 Mezcua, M.; Hlavacek-Larrondo, J.; Lucey, J. R.; Hogan, M. T.; Edge, A. C.; McNamara, B. R. (February 2018). "The most massive black holes on the Fundamental Plane of black hole accretion" (in en). Monthly Notices of the Royal Astronomical Society 474 (1): 1342–1360. doi:10.1093/mnras/stx2812. ISSN 0035-8711. 
  8. ↑ Edge, A. C.; Wilman, R. J.; Johnstone, R. M.; Crawford, C. S.; Fabian, A. C.; Allen, S. W. (2002-06-21). "A survey of molecular hydrogen in the central galaxies of cooling flows" (in en). Monthly Notices of the Royal Astronomical Society 337 (1): 49–62. doi:10.1046/j.1365-8711.2002.05790.x. Bibcode: 2002MNRAS.337...49E. 
  9. ↑ Salomé, P.; Combes, F. (2003-12-01). "Cold molecular gas in cooling flow clusters of galaxies" (in en). Astronomy & Astrophysics 412 (3): 657–667. doi:10.1051/0004-6361:20031438. ISSN 0004-6361. Bibcode: 2003A&A...412..657S. https://www.aanda.org/articles/aa/pdf/2003/49/aa2615.pdf. 
  10. ↑ Wilman, R. J.; Edge, A. C.; Swinbank, A. M. (2006-08-01). "Integral field spectroscopy of H-alpha emission in cooling flow cluster cores: disturbing the molecular gas reservoir". Monthly Notices of the Royal Astronomical Society 371 (1): 93–107. doi:10.1111/j.1365-2966.2006.10658.x. Bibcode: 2006MNRAS.371...93W. 



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