4C 34.07

Last updated
4C 34.07
Image of quasar 4C 34.07.png
Pan-STARRS image of 4C 34.07
Observation data (J2000.0 epoch)
Constellation Triangulum
Right ascension 02h 26m 10.33s [1]
Declination +34° 21′ 30.28″ [1]
Redshift 2.910000 [1]
Heliocentric radial velocity 872,396 km/s [1]
Distance 11.6 Gly
Apparent magnitude  (B)21.3
Characteristics
Type GPS/CSS b [1]
Other designations
B2 0223+34, LEDA 2820338, NVSS J022610+342130, 5C 06.291, 6C B022309.9+340807, S4 0223+34, IERS B0223+341, ICRF J022610.3+342130 [1]

4C 34.07 is a quasar [2] located in the constellation of Triangulum. First documented as a radio source in 1967, [3] the object displays a flat radio spectrum and was later identified with a stellar object through another study published in 1981. [4] [5] The redshift of the quasar at that time was unknown until the 7C survey confirmed its redshift as (z) 2.910. [6] [1]

Contents

Description

4C 34.07 is classified as a strong compact steep spectrum (CSS) source. [7] [8] When observed it is surrounded by a large extended halo structure which contributes 20% of the flux at the frequencies of 1.67 GHz. Evidence also showed the quasar has significant flux density variations indicating the source has interstellar scintillations. It is also found the spectrum of the source at low frequencies displays steepening with the maximum value of between 300-500 MHz. [9]

Radio imaging made with MERLIN, would find the source is a triple asymmetric. When imaged with Very Long Baseline Interferometry (VLBI) at 18 centimeters, it is found to display radio emission on compact scales with small faint knot features located towards the direction of a southwest radio lobe. [10] Another observation by VLBI in 2008, showed the source has a bright radio core dominating it, a radio lobe extending west with another weaker radio lobe in north direction and hot spot that is partially resolved, being located between the position of both western lobe and core. [11] Studies published in 2013, would find the lobes of the source are polarized, with a depolarized northern component in the frequency range between 23.2 and 15 GHz. However, the polarization percentage is relatively constant, in the middle of 15 and 8.0 GHz. [12]

New VLBI observations in 2013 at 5 GHz, found there is an eastern compact region in the quasar. When observed, the region is shown displaying a complicated morphology made up two dominant bright knots located in at the tips of both northern and eastern structures, separating from each other by 79 parsecs. At the southern direction of the source, several blob features are evident which points in the direction of its western lobe. A central compact component is found, hosting 16 MJy of the flux density and has a distance of 68 milliarcseconds from another component with its position angle positioned at 43°. [13] 327 GHz VLBI imaging, would show the structure mainly being dominated by component positioned between two features described as both extended. A south component interpreted as the jet, is seen ending in a direction of a possible hot spot feature in the west. [14]

References

  1. 1 2 3 4 5 6 7 "NED Search results for 4C 34.07". NASA/IPAC Extragalactic Database. Retrieved 2025-09-16.
  2. ↑ Rossetti, A.; Mantovani, F.; Dallacasa, D.; Fanti, C.; Fanti, R. (2005-05-01). "Multi-frequency VLBA observations of compact sources from the Peacock and Wall catalogue" (PDF). Astronomy & Astrophysics. 434 (2): 449–458. arXiv: astro-ph/0501407 . Bibcode:2005A&A...434..449R. doi:10.1051/0004-6361:20041661. ISSN   0004-6361.
  3. ↑ Olsen, E. T. (August 1967). "Accurate positions of selected 4C sources". The Astronomical Journal. 72: 738. Bibcode:1967AJ.....72..738O. doi:10.1086/110302. ISSN   0004-6256. Archived from the original on 2022-04-23.
  4. ↑ L., Fanaroff, B.; M., Blake, G. (1972-04-01). "Observations of Radio Sources with Flat Spectra". Monthly Notices of the Royal Astronomical Society. 157 (1). doi:10.1093/mnra (inactive 16 September 2025). ISSN   0035-8711. Archived from the original (PDF) on 2024-04-23.{{cite journal}}: CS1 maint: DOI inactive as of September 2025 (link) CS1 maint: multiple names: authors list (link)
  5. ↑ Peacock, J. A.; Perryman, M. A. C.; Longair, M. S.; Gunn, J. E.; Westphal, J. A. (1981-03-01). "Investigation of the optical fields of flat-spectrum radio sources to faint limiting magnitudes" (PDF). Monthly Notices of the Royal Astronomical Society. 194 (3): 601–612. doi: 10.1093/mnras/194.3.601 . ISSN   0035-8711.
  6. ↑ Willott, Chris J.; Rawlings, Steve; Blundell, Katherine M.; Lacy, Mark (November 1998). "The radio luminosity function of radio-loud quasars from the 7C Redshift Survey". Monthly Notices of the Royal Astronomical Society. 300 (3): 625–648. arXiv: astro-ph/9807026 . Bibcode:1998MNRAS.300..625W. doi: 10.1046/j.1365-8711.1998.01946.x (inactive 16 September 2025). ISSN   0035-8711.{{cite journal}}: CS1 maint: DOI inactive as of September 2025 (link)
  7. ↑ R., Fanti; C., Fanti; T., Schilizzi, R.; E., Spencer, R.; Rendong, Nan; P., Parma; van Breugel, W. J. M.; T., Venturi (May 1990). "On the nature of compact steep spectrum radio sources". Astronomy and Astrophysics. 231: 333. Bibcode:1990A&A...231..333F. ISSN   0004-6361. Archived from the original on 2024-03-27.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  8. ↑ Fomalont, E. B.; Frey, S.; Paragi, Z.; Gurvits, L. I.; Scott, W. K.; Taylor, A. R.; Edwards, P. G.; Hirabayashi, H. (November 2000). "The VSOP 5 GHz Continuum Survey: The Prelaunch VLBA Observations". The Astrophysical Journal Supplement Series. 131 (1): 95–183. Bibcode:2000ApJS..131...95F. doi:10.1086/317368. ISSN   0067-0049. Archived from the original on 2025-02-19.
  9. ↑ Tyul’bashev, S. A.; Chernikov, P. A. (May 2000). "Physical conditions in steep-spectrum radio sources". Astronomy Reports. 44 (5): 286–297. Bibcode:2000ARep...44..286T. doi:10.1134/1.163852. ISSN   1063-7729. Archived from the original on 2025-02-19.
  10. ↑ D., Dallacasa; C., Fanti; R., Fanti; T., Schilizzi, R.; E., Spencer, R. (March 1995). "A sample of small size compact steep-spectrum radio sources. I. VLBI images at 18 cm". Astronomy and Astrophysics. 295: 27. Bibcode:1995A&A...295...27D. ISSN   0004-6361. Archived from the original on 2024-03-27.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  11. ↑ Lenc, E.; Garrett, M. A.; Wucknitz, O.; Anderson, J. M.; Tingay, S. J. (2008-01-20). "A Deep, High-Resolution Survey of the Low-Frequency Radio Sky". The Astrophysical Journal. 673 (1): 78–95. arXiv: 0710.1946 . Bibcode:2008ApJ...673...78L. doi:10.1086/524295. ISSN   0004-637X.
  12. ↑ Mantovani, F.; Rossetti, A.; Junor, W.; Saikia, D. J.; Salter, C. J. (2013-07-01). "Radio polarimetry of compact steep spectrum sources at sub-arcsecond resolution". Astronomy & Astrophysics. 555: A4. arXiv: 1305.1644 . Bibcode:2013A&A...555A...4M. doi:10.1051/0004-6361/201220769. ISSN   0004-6361.
  13. ↑ Dallacasa, D.; Orienti, M.; Fanti, C.; Fanti, R.; Stanghellini, C. (2013-05-21). "A sample of small-sized compact steep-spectrum radio sources: VLBI images and VLA polarization at 5 GHz". Monthly Notices of the Royal Astronomical Society. 433 (1): 147–161. arXiv: 1304.6261 . doi: 10.1093/mnras/stt710 . ISSN   0035-8711.
  14. ↑ Dallacasa, D; Orienti, M; Fanti, C; Fanti, R (2021-04-13). "VLBI images at 327 MHz of compact steep spectrum and GHz-peaked spectrum sources from the 3C and PW samples". Monthly Notices of the Royal Astronomical Society. 504 (2): 2312–2324. arXiv: 2104.12804 . doi: 10.1093/mnras/stab1014 . 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.