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3C 179

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3C 179
Pan-STARRS image of 3C 179
Observation data (J2000.0 epoch)
ConstellationCamelopardalis
Right ascension07h 28m 10.89s[1]
Declination+67° 48′ 47.03″[1]
Redshift0.841600[1]
Heliocentric radial velocity252,305 km/s[1]
Distance7.035 Gly
Absolute magnitude (V)18.0
Characteristics
TypeSy 1.2, LPQ SSRQ[1]
Other designations
4C +67.14, NVSS J072811+674847, 8C 0723+679, LEDA 2817576, DA 233, NRAO 0263, 2XMM J072810.7+674847, TXS 0723+679, OCARS 0723+679[1]

3C 179 is a powerful Fanaroff-Riley Type II quasar[2][3] located in the northern constellation of Camelopardalis. Its redshift is (z) 0.841[1] and it was first discovered as an astronomical radio source in 1966.[4] It classfied as a radio-loud object[5] and is noted for being the first known double-lobed source to display superluminal motion.[6][7]

Description

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3C 179 is has a compact radio structure. When imaged with Very Large Array (VLA), it has two radio lobes, with its western lobe displaying a different morphology and expanding in southwards direction, through a radio emission region. The eastern lobe on the other hand, is found to split into two main features.[2] There is a strong and bright core dominating the central region of the quasar.[7][8] It is suggested the core might be marginally elongated in east to west direction.[9] Very Long Baseline Interferometry (VLBI) observations have found the two components detected on milliarcseconds, are moving at relative velocities.[6] A bright knot of emission can be seen dotting 0.8 arcseconds along the 270° position angle from the core.[10]

MERLIN imaging revealed 3C 179 has a jet. This jet found one-sided, has a knotty appearance and shows a 'splash' knot feature making it somehow disrupted. It is then further spit into two other jet sections which in turn, goes off in two different directions.[7][11] When imaged, the bright deflated branch of the jet is described as either decollimated or expanding towards the path of a terminal hotspot region. The weaker branch of the jet however, is found moving southwest before fading away into the extended part of the lobe.[7] According to VLA, the entire jet is shown curving northwards.[2]

The core of 3C 179 is described having detections of superluminal motion. Based on observations made by VLBI, it has a double inner structure at the position angle of -92°. Evidence has shown the components are separating apart from each other by 1.07 milliarcseconds, later changing to 1.24 milliarcseconds. The eastern component was also observed and is found increasing in flux density by 15 percent.[12]

References

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  1. ^ a b c d e f g "NED search results for 3C 179". NASA/IPAC Extragalactic Database. Retrieved 2025-07-04.
  2. ^ a b c Fernini, Ilias (2014-05-15). "VERY LARGE ARRAY IMAGES AT 8.4 GHz OF 40 FANAROFF-RILEY II 3CR RADIO SOURCES WITH 0.1 < z < 2.0". The Astrophysical Journal Supplement Series. 212 (2): 19. Bibcode:2014ApJS..212...19F. doi:10.1088/0067-0049/212/2/19. ISSN 0067-0049.
  3. ^ Shone, D. L.; Porcas, R. W.; Zensus, J. A. (April 1985). "Combined MERLIN/VLA observations of the superluminal quasar 3C179". Nature. 314 (6012): 603–604. Bibcode:1985Natur.314..603S. doi:10.1038/314603a0. ISSN 0028-0836.
  4. ^ Pauliny-Toth, I. I. K.; Wade, C. M.; Heeschen, D. S. (May 1966). "Positions and Flux Densities of Radio Sources". The Astrophysical Journal Supplement Series. 13: 65. Bibcode:1966ApJS...13...65P. doi:10.1086/190137. ISSN 0067-0049.
  5. ^ Sambruna, Rita M.; Gliozzi, Mario; Tavecchio, F.; Maraschi, L.; Foschini, Luigi (November 2006). "The Jet-Disk Connection in AGNs: Chandra and XMM-Newton Observations of Three Powerful Radio-Loud Quasars". The Astrophysical Journal. 652 (1): 146–156. arXiv:astro-ph/0606659. Bibcode:2006ApJ...652..146S. doi:10.1086/507420. ISSN 0004-637X.
  6. ^ a b Porcas, R. W. (November 1981). "Superluminal quasar 3C179 with double radio lobes". Nature. 294 (5836): 47–49. Bibcode:1981Natur.294...47P. doi:10.1038/294047a0. ISSN 0028-0836.
  7. ^ a b c d Akujor, C. E. (June 1992). "3C 179 : a high fidelity image of the double-lobed superluminal quasar at 5 GHz". Astronomy and Astrophysics. 259: L61 – L64. ISSN 0004-6361.
  8. ^ Pearson, T. J.; Readhead, A. C. S. (May 1988). "The milliarcsecond structure of a complete sample of radio sources. II - First-epoch maps at 5 GHz". The Astrophysical Journal. 328: 114. Bibcode:1988ApJ...328..114P. doi:10.1086/166274. ISSN 0004-637X.
  9. ^ Pilbratt, G.; Booth, R. S.; Porcas, R. W. (February 1987). "EVN and MERLIN observations of five superluminal radio sources". Astronomy and Astrophysics. 173: 12–22. Bibcode:1987A&A...173...12P. ISSN 0004-6361.
  10. ^ Lehnert, Matthew D.; Miley, George K.; Sparks, William B.; Baum, Stefi A.; Biretta, John; Golombek, Daniel; de Koff, Sigrid; Macchetto, Ferdinando D.; McCarthy, Patrick J. (April 1999). "HST Snapshot Survey of 3CR Quasars: The Data". arXiv e-prints: astro–ph/9904106. arXiv:astro-ph/9904106. Bibcode:1999astro.ph..4106L.
  11. ^ Reddy, Karthik; Georganopoulos, Markos; Meyer, Eileen T. (2021-03-17). "X-Ray-to-radio Offset Inference from Low-count X-Ray Jets". The Astrophysical Journal Supplement Series. 253 (2): 37. arXiv:2101.02024. Bibcode:2021ApJS..253...37R. doi:10.3847/1538-4365/abd8d7. ISSN 0067-0049.
  12. ^ Porcas, R. (1982). "Superluminal expansion in 3C 179". Extragalactic Radio Sources. 97: 361. Bibcode:1982IAUS...97..361P. ISSN 1743-9221.
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