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ZwCl 8193 BCG

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ZwCl 8193 BCG
SDSS image of ZwCl 8193 BCG
Observation data (J2000.0 epoch)
ConstellationHercules
Right ascension17h 17m 19.20s[1]
Declination+42° 26′ 59.84″[1]
Redshift0.182900[1]
Heliocentric radial velocity54,832 ± 30 km/s[1]
Distance2,648.4 ± 185.4 Mly (812.00 ± 56.84 Mpc)[1]
Group or clusterZwCl 8193
magnitude (J)13.24[1]
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

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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

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  1. ^ a b c d e f g h i j "NED Search results for ZwCl 8193 BCG (LEDA 93954)". NASA/IPAC Extragalactic Database. Retrieved 2026-05-14.
  2. ^ a b 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. arXiv:1606.04067. Bibcode:2017ApJ...834..184C. doi:10.3847/1538-4357/834/2/184. ISSN 0004-637X.
  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. arXiv:astro-ph/9903057. Bibcode:1999MNRAS.306..857C. doi:10.1046/j.1365-8711.1999.02583.x. ISSN 0035-8711.
  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; Edge, Alastair C.; Donahue, Megan; Voit, G. Mark (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. arXiv:1006.3796. Bibcode:2010ApJ...719.1619O. doi:10.1088/0004-637x/719/2/1619. ISSN 0004-637X.
  5. ^ Tremblay, G. R.; O'Dea, C. P.; Baum, S. A.; Mittal, R.; McDonald, M. A.; Combes, F.; Li, Y.; McNamara, B. R.; Bremer, M. N.; Clarke, T. E.; Donahue, M.; Edge, A. C.; Fabian, A. C.; Hamer, S. L.; Hogan, M. T. (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. arXiv:1505.03533. doi:10.1093/mnras/stv1151. ISSN 0035-8711.
  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. Bibcode:2002MNRAS.329..877C. doi:10.1046/j.1365-8711.2002.05062.x. ISSN 0035-8711.
  7. ^ a b 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". Monthly Notices of the Royal Astronomical Society. 474 (1): 1342–1360. arXiv:1710.10268. 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". Monthly Notices of the Royal Astronomical Society. 337 (1): 49–62. arXiv:astro-ph/0206379. Bibcode:2002MNRAS.337...49E. doi:10.1046/j.1365-8711.2002.05790.x.
  9. ^ Salomé, P.; Combes, F. (2003-12-01). "Cold molecular gas in cooling flow clusters of galaxies" (PDF). Astronomy & Astrophysics. 412 (3): 657–667. arXiv:astro-ph/0309304. Bibcode:2003A&A...412..657S. doi:10.1051/0004-6361:20031438. ISSN 0004-6361.
  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. arXiv:astro-ph/0606305. Bibcode:2006MNRAS.371...93W. doi:10.1111/j.1365-2966.2006.10658.x.
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