4C 03.24

Last updated
4C 03.24
Observation data (J2000.0 epoch)
Constellation Virgo
Right ascension 12h 45m 38.32s [1]
Declination +03° 23′ 20.89″ [1]
Redshift 3.569900 [1]
Heliocentric radial velocity 1,070229 km/s [1]
Distance 11.546 Gly
Characteristics
Type Radio galaxy
Notable featuresGiant emission Lyman-alpha nebula surrounding the galaxy
Other designations
LEDA 2818474, PKS 1243+036, MRC 1243+036, USS 1243+036, NVSS J124538+032319, 1243+03 [1]

4C 03.24 is a radio galaxy located in the constellation of Virgo. Its redshift is (z) 3.56 [1] and it was first identified as a discrete radio source located in the northern sky by astronomers in 1979. [2] The radio spectrum of this source is found to be ultra-steep, making it an ultra-steep spectrum source (USS) based on deep R-band CCD imaging and was later identified with an R magnitude 22.5 galaxy. [3] [4]

Description

4C 03.24 is classified as a Type 2 Fanaroff-Riley Class radio galaxy. [4] Its size is estimated to be greater than 1.7 kiloparsecs with a star-formation rate of 142 Mʘ yr-1. The star-formation luminosity of the galaxy is 1.23+2.08
−1.13×1012 Lʘ based on Atacama Large Millimeter Array (ALMA) observations. [5]

The source of 4C 03.24, best described as a double, has a northern radio lobe containing a compact component with a tail extension extending towards the north. The southern radio lobe of the galaxy shows a compact feature near its nucleus and a bent jet going south from the northern component. This jet is also slightly extended to the west. Between the lobes, there is a faint radio emission region containing a core-jet structure which is orientated at –24°. [4] [6] Imaging by the Hubble Space Telescope also discovered a small component beyond its northern hotspot. [7] There is a radio core clearly detected at 4.7 GHz and 8.3 GHz frequencies, located 0.5 arcseconds from an X-ray source. [8]

The galaxy is surrounded by a giant irregular Lyman-alpha emission nebula with a projected size of 5.3" x 0.9". [4] [9] [10] When imaged with the Subaru Telescope and FOCAS spectrometer, the nebula is found to have an extremely complicated structure. The first component shown displays an asymmetric blue profile. The second component found extended, is located on both sides of the nucleus with an outer-halo extending at a systematic velocity. The third component is found blueshifted with a velocity of –1000 km/s. There is another blueshifted component on the northwest side; the opposite side of the nucleus, with a wide velocity width of 1900 km/s at full width at half maximum. Further evidence also showed the nebula is extended by 30 kiloparsecs, suggesting it was caused by circumgalactic matter being ionized by the AGN's anisotropic hard radiation. Alternatively, it might be created by superwind outflows, given the galaxy showed elongated core-like or bubble structures protruding in opposite directions. [9] Observations also suggested the jet is interacting with the interstellar gas within the inner region based on Lyman-alpha imaging. [11]

A detection of a weak X-ray emission halo has been discovered around 4C 03.24. Based on results, the X-ray luminosity of the halo is 3 x 1044 erg/s and is found to be four times fainter compared to two other high-redshift radio galaxies, 4C 41.17 and 4C 60.07, which were observed previously. [12] Companion systems have also been discovered in 4C 03.24 by both James Webb Space Telescope and ALMA in 2025 who found three [C III] emitters. [13]

References

  1. 1 2 3 4 5 6 "NED search results for 4C 03.24". NASA/IPAC Extragalactic Database. Retrieved 2025-06-08.
  2. ↑ Braude, S. Ia; Megn, A. V.; Sokolov, K. P.; Tkachenko, A. P.; Sharykin, N. K. (August 1979). "Decametric survey of discrete sources in the northern sky: V. Source catalogue in the range of declinations 0° to +10°". Astrophysics and Space Science. 64 (1): 73–126. Bibcode:1979Ap&SS..64...73B. doi:10.1007/BF00640035. ISSN   0004-640X.
  3. ↑ Roettgering, H. J. A.; Miley, G. K.; Chambers, K. C.; Macchetto, F. (November 1995). "CCD imaging of ultra-steep-spectrum radio sources". Astronomy and Astrophysics Supplement Series. 114: 51. ISSN   0365-0138.
  4. 1 2 3 4 van Ojik, R.; Roettgering, H. J. A.; Carilli, C. L.; Miley, G. K.; Bremer, M. N.; Macchetto, F. (September 1996). "A powerful radio galaxy at z=3.6 in a giant rotating Lyman α halo". Astronomy and Astrophysics. 313: 25–44. arXiv: astro-ph/9608099 . Bibcode:1996A&A...313...25V. ISSN   0004-6361.
  5. ↑ Falkendal, Theresa; Breuck, Carlos De; Lehnert, Matthew D.; Drouart, Guillaume; Vernet, Joël; Emonts, Bjorn; Lee, Minju; Nesvadba, Nicole P. H.; Seymour, Nick; Béthermin, Matthieu; Kolwa, Sthabile; Gullberg, Bitten; Wylezalek, Dominika (2019-01-01). "Massive galaxies on the road to quenching: ALMA observations of powerful high redshift radio galaxies" (PDF). Astronomy & Astrophysics. 621: A27. arXiv: 1809.09427 . Bibcode:2019A&A...621A..27F. doi:10.1051/0004-6361/201732485. ISSN   0004-6361.
  6. ↑ Ojik, R. van; Röttgering, H. J. A.; Carilli, C. L.; Miley, G. K.; Bremer, M. N.; Macchetto (1996-08-16), A radio galaxy at z=3.6 in a giant rotating Lyman α halo, arXiv: astro-ph/9608099 , arXiv:astro-ph/9608099
  7. ↑ Pentericci, L.; Rottgering, H. J. A.; Miley, G. K.; McCarthy, P.; Spinrad, H.; Breugel, W. J. M. van; Macchetto, F. (1998-09-05), HST images and properties of the most distant radio galaxies, arXiv: astro-ph/9809056 , arXiv:astro-ph/9809056
  8. ↑ Wu, Jianfeng; Ghisellini, Gabriele; Hodges-Kluck, Edmund; Gallo, Elena; Ciardi, Benedetta; Haardt, Francesco; Sbarrato, Tullia; Tavecchio, Fabrizio (2017-02-20). "CMB-induced radio quenching of high-redshift jetted AGNs with highly magnetic hotspots". Monthly Notices of the Royal Astronomical Society. 468 (1): 109–121. arXiv: 1702.04725 . doi: 10.1093/mnras/stx416 . ISSN   0035-8711.
  9. 1 2 Ohyama, Y.; Taniguchi, Y. (June 2004). "Subaru Spectroscopy of the Giant Lyα Nebula around 1243+036". Recycling Intergalactic and Interstellar Matter. 217: 344. Bibcode:2004IAUS..217..344O. ISSN   1743-9221.
  10. ↑ Nesvadba, N. P. H.; Breuck, C. De; Lehnert, M. D.; Best, P. N.; Collet, C. (2017-03-01). "The SINFONI survey of powerful radio galaxies at z ~ 2: Jet-driven AGN feedback during the Quasar Era" (PDF). Astronomy & Astrophysics. 599: A123. arXiv: 1610.02057 . Bibcode:2017A&A...599A.123N. doi:10.1051/0004-6361/201528040. ISSN   0004-6361.
  11. ↑ Cimatti, A.; Freudling, W.; Rottgering, H. J. A.; Ivison, R. J.; Mazzei, P. (January 1998). "Dust in high-z radio-loud AGN". Astronomy and Astrophysics. 329: 399–408. arXiv: astro-ph/9708204 . Bibcode:1998A&A...329..399C. ISSN   0004-6361.
  12. ↑ Smail, Ian; Blundell, Katherine M.; Lehmer, B. D.; Alexander, D. M. (2012-11-16). "INVERSE COMPTON X-RAY HALOS AROUND HIGH-zRADIO GALAXIES: A FEEDBACK MECHANISM POWERED BY FAR-INFRARED STARBURSTS OR THE COSMIC MICROWAVE BACKGROUND?". The Astrophysical Journal. 760 (2): 132. arXiv: 1210.4548 . Bibcode:2012ApJ...760..132S. doi:10.1088/0004-637x/760/2/132. ISSN   0004-637X.
  13. ↑ Wang, Wuji; Breuck, Carlos De; Wylezalek, Dominika; Vernet, Joël; Lehnert, Matthew D.; Stern, Daniel; Rupke, David S. N.; Nesvadba, Nicole P. H.; Vayner, Andrey; Zakamska, Nadia L.; Lin, Lingrui; Kukreti, Pranav; Oliveira, Bruno Dall’Agnol de; Groth, Julian T. (2025-04-01). "JWST + ALMA ubiquitously discover companion systems within ≲18 kpc around four z ≈ 3.5 luminous radio-loud AGN" (PDF). Astronomy & Astrophysics. 696: A88. arXiv: 2502.20442 . Bibcode:2025A&A...696A..88W. doi:10.1051/0004-6361/202553668. ISSN   0004-6361.
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