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ZwCl 8193 BCG

From Wikipedia, the free encyclopedia
Brightest cluster galaxy of ZwCl 8193 in the constellation Hercules
ZwCl 8193 BCG
SDSS image of ZwCl 8193 BCG
Observation data (J2000.0 epoch)
Constellation Hercules
Right ascension 17h 17m 19.20s[1]
Declination +42°26′59.84′′[1]
Redshift 0.182900[1]
Heliocentric radial velocity 54,832 ± 30 km/s [1]
Distance 2,648.4±185.4Mly (812.00±56.84Mpc)[1]
Group or cluster ZwCl 8193
magnitude(J)13.24[1]
Characteristics
Type BrClG;AGN blazar[1]
Size~714,500ly (219.08kpc) (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 ×ばつ 1010 Mʘ and the molecular line luminosity is approximately 1.1 ± 0.1 ×ばつ 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 ×ばつ 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. 1 2 3 4 5 6 7 8 9 10 "NED Search results for ZwCl 8193 BCG (LEDA 93954)". NASA/IPAC Extragalactic Database. Retrieved 2026年05月14日.
  2. 1 2 Condon, J. J.; Darling, Jeremy; Kovalev, Y. Y.; Petrov, L. (2017年01月10日). "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年07月11日). "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年08月02日). "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年06月29日). "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. 1 2 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年06月21日). "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年12月01日). "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年08月01日). "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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