3C 334

Nowadays, 3C 334 is a topic that arouses the interest of many people around the world. Over time, 3C 334 has acquired great relevance in various fields, from politics to science, including culture and society in general. Its impact has been so significant that it has generated debates, controversies and deep reflections among experts and ordinary citizens alike. In this article, we will analyze the role that 3C 334 currently plays and explore its implications in different contexts.

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]
Heliocentric 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. ^ a b c d e f "NASA/IPAC Extragalactic Database results for 3C 334". ned.ipac.caltech.edu. Retrieved 2025-03-16.
  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" (PDF). Astronomy & Astrophysics. 428 (2): 401–408. arXiv:astro-ph/0407307. Bibcode:2004A&A...428..401V. doi:10.1051/0004-6361:20040303. ISSN 0004-6361.
  3. ^ Marecki, A. (2012-09-01). "Are 3C 249.1 and 3C 334 restarted quasars?". Astronomy & Astrophysics. 545: A132. arXiv:1209.1284. Bibcode:2012A&A...545A.132M. doi:10.1051/0004-6361/201220010. ISSN 0004-6361.
  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. Bibcode:1965ApJ...142.1674B. doi:10.1086/148459. ISSN 0004-637X.
  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. Bibcode:1992ApJ...393...81H. doi:10.1086/171486. ISSN 0004-637X.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  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. arXiv:astro-ph/9912306. Bibcode:2000MNRAS.315..433C. doi:10.1046/j.1365-8711.2000.03290.x. ISSN 0035-8711.
  7. ^ a b 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. Bibcode:1994AJ....108..766B. doi:10.1086/117112. ISSN 0004-6256.
  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. Bibcode:2004MNRAS.351..845G. doi:10.1111/j.1365-2966.2004.07824.x. ISSN 0035-8711.
  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. Bibcode:1994A&AS..105...91B. ISSN 0365-0138.
  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" (PDF). Astronomy & Astrophysics. 371 (1): 97–106. arXiv:astro-ph/0103232. Bibcode:2001A&A...371...97M. doi:10.1051/0004-6361:20010359. ISSN 0004-6361.
  11. ^ Guibin, Jia; Xuefen, Cen; Huiyu, Ma; Wang, Jiancheng (1997). "Variability in blazars". Astronomy & Astrophysics Supplement Series. 128: 315–324.
  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. Bibcode:1998ApJ...501...69D. doi:10.1086/305817. ISSN 0004-637X.
  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. arXiv:astro-ph/9803210. Bibcode:1998A&A...334..799V. ISSN 0004-6361.
  14. ^ Setti, G.; Brunetti, G.; Comastri, A. (2002). "Extended X-ray Emission from FRIIs and RL Quasars". Symposium - International Astronomical Union. 199: 227–230. arXiv:astro-ph/0002225. 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. arXiv:astro-ph/9904371. Bibcode:1999MNRAS.308.1159C. doi:10.1046/j.1365-8711.1999.02804.x. ISSN 0035-8711.
  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. Bibcode:1996A&A...313..423H. doi:10.1086/192178. ISSN 0067-0049.

3C 334 on SIMBAD