Astronomy:3C 334

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3C 334
The quasar 3C 334.
Observation data (J2000.0 epoch)
ConstellationHercules
Right ascension +16h 20m 21.819s[1]
Declination+17° 36′ 23.951″[1]
Redshift0.555167[1]
Helio radial velocity166,435 km/s[1]
Distance5.255 Gly
Apparent magnitude (V)16.41
Apparent magnitude (B)16.53
Characteristics
TypeQSO[1]
Other designations
NRAO 500, QSO B1618+1743, LEDA 2817681, 4C 17.68, OHIO S 131, PKS 1618+177, 2E 3648

3C 334 is a powerful radio-loud quasar located in the constellation of Hercules, about 5.2 billion light years away from Earth.[1] It has a redshift of (z) 0.555.[2][3] First discovered as an astronomical radio source in 1965,[4] the object is classified as a lobe-dominated quasar showing signs of superluminal motion.[5]

Description

3C 334 is found to be located inside a dense cluster environment.[6] It has a sharp bounded northern radio lobe with a plume extension in the south while the southern radio lobe on the other hand, is weakly brightened with a much faint lobe emission.[7] There is also a trail of radio emission found leading towards a diffused hotspot, possibly interpreted as a counter-jet. A southern jet can be seen going straight before curving eastwards to a hotspot region, based on Multi-Element Radio Linked Interferometer Network and Very Large Array observation imaging.[8] Low brightness emission is also present between the object's lobes and the radio core.[9] There is a knot described as elongated, connecting to the hotspot via a weak emission bridge.[7]

The host galaxy of the object has an elongated appearance. Based on observations, the host has twisted isotopes with an arc-like structure to the south direction evidently detected by its oxygen atom (O II) emission.[10]

The object shows a variation period of 15 years indicating blazar behavior.[11] In February 1997, it was found to be in a stable state but however its brightness faded by 0.05 magnitude after 2.5 hours.[12] According to high resolution centimeter-millimeter observations, its core is found to have substantial variability, exhibiting core flux density values of 5 GHz which was measured during the past 20 years.[13] Extended X-ray emission was also found emitting from the object with its 60ɥm luminosity measured as 1046 erg s-1.[14] The pressure of the emission from within its emission-line region has a value exceeding 6 x 105 cm-3 Kelvin.[15] Emission line imaging also showed the object having a bar-shaped nebula that is located at position angle of 150°.[16]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 "NASA/IPAC Extragalactic Database results for 3C 334". https://ned.ipac.caltech.edu/byname?objname=3C+334&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Varano, S.; Chiaberge, M.; Macchetto, F. D.; Capetti, A. (2004-11-26). "The nuclear radio-optical properties of intermediate-redshift FR II radio galaxies and quasars". Astronomy & Astrophysics 428 (2): 401–408. doi:10.1051/0004-6361:20040303. ISSN 0004-6361. Bibcode: 2004A&A...428..401V. https://www.aanda.org/articles/aa/pdf/2004/47/aa0303-04.pdf. 
  3. ↑ Marecki, A. (2012-09-01). "Are 3C 249.1 and 3C 334 restarted quasars?" (in en). Astronomy & Astrophysics 545: A132. doi:10.1051/0004-6361/201220010. ISSN 0004-6361. Bibcode: 2012A&A...545A.132M. https://www.aanda.org/articles/aa/full_html/2012/09/aa20010-12/aa20010-12.html. 
  4. ↑ Burbidge, E. Margaret (1965). "Redshifts of the Quasi-Stellar Radio Sources 3c 334, 3c 345, 3c 380, and a Discussion of the Possible Redshift of 3c 446.". The Astrophysical Journal 142: 1674. doi:10.1086/148459. ISSN 0004-637X. Bibcode: 1965ApJ...142.1674B. https://articles.adsabs.harvard.edu//full/1965ApJ...142.1674B/0001674.000.html. 
  5. ↑ Hough, D. H.; Readhead, A. C. S.; Wood, D. A., Jr.; Feldmeier, J. J. (1992). "Three-epoch VLBI observations of the nucleus in the lobe-dominated quasar 3C 334". The Astrophysical Journal 393: 81. doi:10.1086/171486. ISSN 0004-637X. Bibcode: 1992ApJ...393...81H. https://adsabs.harvard.edu/full/1992ApJ...393...81H. 
  6. ↑ Crawford, C. S.; Vanderriest, C. (2000-07-01). "Optical integral field spectroscopy of the extended line emission around six radio-loud quasars". Monthly Notices of the Royal Astronomical Society 315 (3): 433–449. doi:10.1046/j.1365-8711.2000.03290.x. ISSN 0035-8711. Bibcode: 2000MNRAS.315..433C. 
  7. ↑ 7.0 7.1 Bridle, Alan H.; Hough, David H.; Lonsdale, Colin J.; Burns, Jack O.; Laing, Robert A. (1994-09-01). "Deep VLA Imaging of Twelve Extended 3CR Quasars". The Astronomical Journal 108: 766. doi:10.1086/117112. ISSN 0004-6256. Bibcode: 1994AJ....108..766B. https://articles.adsabs.harvard.edu/pdf/1994AJ....108..766B. 
  8. ↑ Gilbert, G. M.; Riley, J. M.; Hardcastle, M. J.; Croston, J. H.; Pooley, G. G.; Alexander, P. (2004). "High-resolution observations of a complete sample of 27 FR II radio galaxies and quasars with 0.3 <z< 0.6". Monthly Notices of the Royal Astronomical Society 351 (3): 845–890. doi:10.1111/j.1365-2966.2004.07824.x. ISSN 0035-8711. Bibcode: 2004MNRAS.351..845G. 
  9. ↑ Bogers, W. J.; Hes, R.; Barthel, P. D.; Zensus, J. A. (1994-05-01). "High resolution radio observations of intermediate redshift quasars and radio galaxies". Astronomy and Astrophysics Supplement Series 105: 91–113. ISSN 0365-0138. Bibcode: 1994A&AS..105...91B. https://articles.adsabs.harvard.edu//full/1994A%26AS..105...91B/0000098.000.html. 
  10. ↑ Márquez, I.; Petitjean, P.; Théodore, B.; Bremer, M.; Monnet, G.; Beuzit, J.-L. (2001-05-01). "Adaptive optics imaging of low and intermediate redshift quasars" (in en). Astronomy & Astrophysics 371 (1): 97–106. doi:10.1051/0004-6361:20010359. ISSN 0004-6361. Bibcode: 2001A&A...371...97M. https://www.aanda.org/articles/aa/pdf/2001/19/aa1059.pdf. 
  11. ↑ Guibin, Jia; Xuefen, Cen; Huiyu, Ma; Wang, Jiancheng (1997). "Variability in blazars". Astronomy & Astrophysics Supplement Series 128: 315–324. https://aas.aanda.org/articles/aas/full/1998/05/dst6383/node4.html#SECTION00040000000000000000. 
  12. ↑ de Diego, J. A.; Dultzin-Hacyan, D.; Ramirez, A.; Benitez, E. (1998). "A Comparative Study of the Microvariability Properties in Radio-loud and Radio-quiet Quasars". The Astrophysical Journal 501 (1): 69–81. doi:10.1086/305817. ISSN 0004-637X. Bibcode: 1998ApJ...501...69D. https://iopscience.iop.org/article/10.1086/305817/fulltext/37520.text.html. 
  13. ↑ van Bemmel, Ilse M.; Barthel, Peter D.; Yun, Min S. (1998-06-01). "Nature of 60mu M emission in 3C 47, 3C 207 and 3C 334". Astronomy and Astrophysics 334: 799–804. ISSN 0004-6361. Bibcode: 1998A&A...334..799V. https://articles.adsabs.harvard.edu/pdf/1998A%26A...334..799V. 
  14. ↑ Setti, G.; Brunetti, G.; Comastri, A. (2002). "Extended X-ray Emission from FRIIs and RL Quasars". Symposium - International Astronomical Union 199: 227–230. doi:10.1017/s0074180900168986. ISSN 0074-1809. 
  15. ↑ Crawford, C. S.; Lehmann, I.; Fabian, A. C.; Bremer, M. N.; Hasinger, G. (1999-10-01). "Detection of X-ray emission from the host clusters of 3CR quasars". Monthly Notices of the Royal Astronomical Society 308 (4): 1159–1172. doi:10.1046/j.1365-8711.1999.02804.x. ISSN 0035-8711. Bibcode: 1999MNRAS.308.1159C. https://articles.adsabs.harvard.edu/pdf/1999MNRAS.308.1159C. 
  16. ↑ McCarthy, Patrick J.; Spinrad, Hyron; van Breugel, Wil (1996). "Emission-Line Imaging of 3CR Radio Galaxies. I. Imaging Data". The Astrophysical Journal Supplement Series 99: 27. doi:10.1086/192178. ISSN 0067-0049. Bibcode: 1996A&A...313..423H. https://articles.adsabs.harvard.edu//full/1996A%26A...313..423H/0000428.000.html. 

3C 334 on SIMBAD



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