3C 254

Last updated

3C 254
3C 254 SDSS image.jpg
The quasar 3C 254. Above the object is the galaxy, 2MASS J11143975+4037350.
Observation data (J2000.0 epoch)
Constellation Ursa Major
Right ascension 11h 14m 38.7241s
Declination +40° 37′ 20.285″
Redshift 0.735926
Heliocentric radial velocity 220,625 km/s
Distance 6.318 Gly
Apparent magnitude  (V)17.42
Apparent magnitude  (B)17.62
Characteristics
Type RL1
Other designations
4C 40.18, DA 298, LEDA 2817631, NRAO 369, QSO J1114+4037, 2E 2426

3C 254 is a radio-loud quasar [1] located in the constellation of Ursa Major. The object has a redshift of (z) 0.734 and is classified as a Fanaroff-Riley class type II source. [2] It was first identified by astronomers as an astronomical radio source in 1965. [3]

Contents

Description

3C 254 contains an asymmetrical radio structure consisting of two radio lobes and a central component. [4] [5] Its radio spectrum is found straight and steep. [6] When imaged by MERLIN (Multi-Element Radio-linked Interferometer Network) at 1539 MHz, the western lobe is made up of two hotspots, a compact primary hotspot and a more diffused secondary hotspot with an approximate peak brightness of 36 mJy. In addition, the western lobe is found to be significantly polarized compared to the eastern lobe, whose emission is less compact and stretching in a south-east direction. [5] A study published in 1982 showed both lobes of 3C 254 are extended. [7] There is also an eastern component found perpendicular towards the axis of the source, interpreted as a side-flow. [8]

The host galaxy of 3C 354 according to imaging by Hubble Space Telescope (HST), has a complex morphology. It is orientated in an east-west direction, showing traces of emission plumes along the position angles of 285° and 45°. [9] Further evidence also showed the object is surrounded by a number of faint objects, suggesting it might belong in a galaxy cluster. [10]

An extended emission-line region has been discovered around 3C 254. Based on observations, the region is extended by 80 kiloparsecs (kpc). [11] [12] Further evidence also showed there are signs of kinematics and intensity in its emission lines, hinting the jet is interacting with a gas cloud. [12] A secondary X-ray emission source was discovered although an optical counterpart wasn't found. [13]

References

  1. ↑ Megn, A. V.; Braude, S. Ya.; Rashkovskij, S. L.; Sharykin, N. K.; Shepelev, V. A.; Inyutin, G. A.; Khristenko, A. D.; Brazhenko, A. I.; Bulatsen, V. G. (1 January 1996). "Interferometer observations of the quasar 3C 254 in the decameter wavelengths range". Kinematika I Fizika Nebesnykh Tel. 12 (6): 3–12. Bibcode:1996KFNT...12f...3M. ISSN   0233-7665.
  2. ↑ Donahue, Megan; Daly, Ruth A.; Horner, Donald J. (20 February 2003). "Constraints on the Cluster Environments and Hot Spot Magnetic Field Strengths of the Radio Sources 3C 280 and 3C 254". The Astrophysical Journal. 584 (2): 643–656. arXiv: astro-ph/0211145 . Bibcode:2003ApJ...584..643D. doi:10.1086/345831. ISSN   0004-637X.
  3. ↑ Schmidt, Maarten (April 1965). "Large Redshifts of Five Quasi-Stellar Sources". The Astrophysical Journal. 141: 1295. Bibcode:1965ApJ...141.1295S. doi:10.1086/148217. ISSN   0004-637X.
  4. ↑ Davis, R. J.; Stannard, D.; Conway, R. G. (1 December 1983). "Interferometric observations of compact components in extragalactic radio sources - II". Monthly Notices of the Royal Astronomical Society. 205 (4): 1267–1278. Bibcode:1983MNRAS.205.1267D. doi: 10.1093/mnras/205.4.1267 . ISSN   0035-8711.
  5. 1 2 Thomasson, P.; Saikia, D. J.; Muxlow, T. W. B. (11 November 2006). "3C 254: MERLIN observations of a highly asymmetric quasar". Monthly Notices of the Royal Astronomical Society. 372 (4): 1607–1613. arXiv: astro-ph/0608481 . Bibcode:2006MNRAS.372.1607T. doi: 10.1111/j.1365-2966.2006.10955.x . ISSN   0035-8711.
  6. ↑ Hooimeyer, J. R. A.; Barthel, P. D.; Schilizzi, R. T.; Miley, G. K. (1 July 1992). "The radio structure of extended quasars. I. A VLBI survey of the nuclear emission". Astronomy and Astrophysics. 261: 18–24. Bibcode:1992A&A...261...18H. ISSN   0004-6361.
  7. ↑ Schilizzi, R. T.; Kapahi, V. K.; Neff, S. G. (1 June 1982). "VLA Observations of Hot Spots in High Luminosity Radio Sources". Journal of Astrophysics and Astronomy. 3 (2): 173–187. Bibcode:1982JApA....3..173S. doi:10.1007/BF02714801. ISSN   0250-6335.
  8. ↑ Liu, R.; Pooley, G.; Riley, J. M. (15 August 1992). "Spectral ageing in a sample of 14 high-luminosity double radio sources". Monthly Notices of the Royal Astronomical Society. 257 (4): 545–571. Bibcode:1992MNRAS.257..545L. doi: 10.1093/mnras/257.4.545 . ISSN   0035-8711.
  9. ↑ 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. (August 1999). "HUBBLE SPACE TELESCOPE Snapshot Survey of 3CR Quasars: The Data" . The Astrophysical Journal Supplement Series. 123 (2): 351–376. Bibcode:1999ApJS..123..351L. doi:10.1086/313239. ISSN   0067-0049.
  10. ↑ Bremer, M. N. (1 January 1997). "3C 254: the alignment effect and unification schemes". Monthly Notices of the Royal Astronomical Society. 284: 126–136. doi: 10.1093/mnras/284.1.126 . hdl: 1887/6700 . ISSN   0035-8711.
  11. ↑ Forbes, D. A.; Crawford, C. S.; Fabian, A. C.; Johnstone, R. M. (1 June 1990). "Extended emission-line gas around the quasars 3C 254 and 3C 309.1 . Very massive cooling flows". Monthly Notices of the Royal Astronomical Society. 244: 680. Bibcode:1990MNRAS.244..680F. ISSN   0035-8711.
  12. 1 2 Crawford, C. S.; Vanderriest, C. (1 March 1997). "Integral field spectroscopy of a jet-cloud interaction in the quasar 3C254". Monthly Notices of the Royal Astronomical Society. 285 (3): 580–592. Bibcode:1997MNRAS.285..580C. doi: 10.1093/mnras/285.3.580 . ISSN   0035-8711.
  13. ↑ Crawford, C. S.; Lehmann, I.; Fabian, A. C.; Bremer, M. N.; Hasinger, G. (1 October 1999). "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.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.