3C 356

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3C 356
Radio galaxy 3C 356.jpg
The radio galaxy 3C 356.
Observation data (J2000.0 epoch)
Constellation Draco
Right ascension 17h 24m 19.041s
Declination +50° 57′ 40.14″
Redshift 1.079000
Heliocentric radial velocity 323,476 km/s
Distance 7.817 Gly
Apparent magnitude  (V)21.5
Apparent magnitude  (B)21.5
Characteristics
Type NLRG
Other designations
LHE 425, 4C 51.36, OHIO T 538, NRAO 526, NVSS J172420+505714, WB 1723+5100, LEDA 2817697

3C 356 is a distant radio galaxy [1] [2] located in the constellation of Draco, hosted by a merging pair of elliptical galaxies located at redshift (z) 1.079 [3] with two radio cores having a separation gap of 5 arcseconds. [4] [5] It was first discovered as an astronomical radio source by P. Veron from a 3C revised catalogue in 1966 [6] and such, shows an alignment effect at both wavelengths. [7] The X-ray source luminosity for this galaxy is estimated to be 2.5 x 1044 erg s−1. [2]

Contents

Description

3C 356 contains a double compact source with a 170° position angle. The source is found weakly depolarized in south-east direction closer to the central region. There is a presence of a northern object displaying a more ionized emission line spectrum likely the source's origin. In additional, the northern component is more compact but has an extension directly south by 3 arcseconds. [8] According to Hubble Space Telescope (HST) imaging of a northwest component, this shows a high surface brightness conelike structure with a much fainter extension. [9]

The radio structure of 3C 356 is complex. Its radio core position is unresolved with a diffused region peaking 5 arcseconds away at a position angle of 150° and a radio axis of 162°. [10] There are two radio lobes in 3C 356 are located 15 arcseconds and 30 arcseconds in both directions. [3] According to Very Large Array radio mapping, both northwestern and southeastern lobes are shown enlarged and overlaid polarized. In the southeastern lobe, there are three compact structures of equal brightness. The northwestern lobe on the other hand, contains a defined hot spot and more extended emission. [11]

According to deep near-infrared imaging taken via Subaru Telescope, 3C 356 is found connected with a poor cluster of galaxies. [12] A stellar mass of 4 x 1011 Mʘ has also been calculated for the spectral energy distribution of the galaxy as well, with the supermassive black hole mass being 8.74 ± 0.42 Mʘ. [13]

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References

  1. ↑ information@eso.org. "Radio galaxy 3C 356". www.esahubble.org. Retrieved 2024-12-01.
  2. 1 2 Crawford, C. S.; Fabian, A. C. (July 1996). "A ROSAT HRI observation of 3C 356: further evidence for a distant intracluster medium". Monthly Notices of the Royal Astronomical Society. 281 (1): L5 –L8. Bibcode:1996MNRAS.281L...5C. doi: 10.1093/mnras/281.1.l5 . ISSN   0035-8711.
  3. 1 2 Hilbert, B.; Chiaberge, M.; Kotyla, J. P.; Tremblay, G. R.; Stanghellini, C.; Sparks, W. B.; Baum, S.; Capetti, A.; Macchetto, F. D.; Miley, G. K.; O’Dea, C. P.; Perlman, E. S.; Quillen, A. (2016-07-01). "Powerful Activity in the Bright Ages. I. A Visible/IR Survey of High Redshift 3C Radio Galaxies and Quasars". The Astrophysical Journal Supplement Series. 225 (1): 12. arXiv: 1605.03196 . Bibcode:2016ApJS..225...12H. doi: 10.3847/0067-0049/225/1/12 . ISSN   0067-0049.
  4. ↑ Best, P. N.; Longair, M. S.; Rottgering, H. J. A. (1996-05-01). "Evolution of the aligned structures in z 1 radio galaxies". Monthly Notices of the Royal Astronomical Society. 280 (1): L9 –L12. doi: 10.1093/mnras/280.1.l9 . hdl: 1887/6693 . ISSN   0035-8711.
  5. ↑ Jackson, N.; Rawlings, S. (1997-03-21). "[O III] 500.7 spectroscopy of 3C galaxies and quasars at redshift z > 1". Monthly Notices of the Royal Astronomical Society. 286 (1): 241–256. Bibcode:1997MNRAS.286..241J. doi: 10.1093/mnras/286.1.241 . ISSN   0035-8711.
  6. ↑ Véron, P. (June 1966). "Optical Positions for Radio Sources in the 3C Revised Catalogue". The Astrophysical Journal. 144: 861. Bibcode:1966ApJ...144..861V. doi:10.1086/148682. ISSN   0004-637X.
  7. ↑ Cimatti, Andrea; Dey, Arjun; Breugel, Wil van; Hurt, Todd; Antonucci, Robert (1997-02-20). "Keck Spectropolarimetry of Two High-zRadio Galaxies: Discerning the Components of the Alignment Effect". The Astrophysical Journal. 476 (2): 677–684. Bibcode:1997ApJ...476..677C. doi:10.1086/303660. ISSN   0004-637X.
  8. ↑ Crawford, C. S.; Fabian, A. C. (January 1993). "A ROSAT observation of the powerful distant radio galaxy 3C 356". Monthly Notices of the Royal Astronomical Society. 260 (1): L15 –L19. doi: 10.1093/mnras/260.1.l15 . ISSN   0035-8711.
  9. ↑ Martel, André R.; Baum, Stefi A.; Sparks, William B.; Wyckoff, Eric; Biretta, John A.; Golombek, Daniel; Macchetto, Ferdinando D.; de Koff, Sigrid; McCarthy, Patrick J.; Miley, George K. (May 1999). "Hubble Space Telescope Snapshot Survey of 3CR Radio Source Counterparts. II. Radio Galaxies with z > 0.5". The Astrophysical Journal Supplement Series. 122 (1): 81–108. Bibcode:1999ApJS..122...81M. doi:10.1086/313205. ISSN   0067-0049.
  10. ↑ Eisenhardt, Peter; Chokshi, Arati (March 1990). "Infrared images of distant 3C radio galaxies". The Astrophysical Journal. 351: L9. Bibcode:1990ApJ...351L...9E. doi:10.1086/185667. ISSN   0004-637X.
  11. ↑ Fernini, Ilias; Burns, Jack O.; Bridle, Alan H.; Perley, Rick A. (May 1993). "Very Large Array imaging of five Fanaroff-Riley II 3CR radio galaxies". The Astronomical Journal. 105: 1690. Bibcode:1993AJ....105.1690F. doi:10.1086/116547. ISSN   0004-6256.
  12. ↑ Simpson, C.; Rawlings, S. (2002-08-11). "The radio galaxy 3C 356 and clues to the trigger mechanisms for powerful radio sources". Monthly Notices of the Royal Astronomical Society. 334 (3): 511–522. arXiv: astro-ph/0203446 . Bibcode:2002MNRAS.334..511S. doi: 10.1046/j.1365-8711.2002.05453.x . ISSN   0035-8711.
  13. ↑ Fernandes, C. A. C.; Jarvis, M. J.; Martínez-Sansigre, A.; Rawlings, S.; Afonso, J.; Hardcastle, M. J.; Lacy, M.; Stevens, J. A.; Vardoulaki, E. (2014-12-22). "Black hole masses, accretion rates and hot- and cold-mode accretion in radio galaxies at z ∼ 1". Monthly Notices of the Royal Astronomical Society. 447 (2): 1184–1203. arXiv: 1411.7388 . doi: 10.1093/mnras/stu2517 . ISSN   1365-2966.
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