Astronomy:OH 471

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OH 471
The quasar/blazar OH 471.
Observation data (J2000.0 epoch)
ConstellationAuriga
Right ascension 06h 46m 32.0260s
Declination+44° 51′ 16.590″
Redshift3.396000
Helio radial velocity1,018,295 km/s
Distance11.442 Gly
Apparent magnitude (V)18.49
Apparent magnitude (B)19.57
Characteristics
TypeOpt. var; LPQ, FSRQ
Other designations
2E 1729, QSO B0642+449, NVSS J064632+445116, KODIAQ JJ064632+445116, S4 0642+449

OH 471 (OHIO H 471) is a distant powerful quasar located in the northern constellation of Auriga. First discovered in 1974 from a photoelectric spectrophotometry, the object has a redshift of (z) 3.40.[1] [2][3] This high redshift makes it one of the most distant objects observed, giving it a nickname of "the blaze marking the edge of the universe."[4] It is found to be significantly variable thus classifying it as a blazar.[5][6]

Description

OH 471 is a low polarized quasar but also a high frequency peaker (HFP).[7] It is a radio-loud gamma ray blazar with a central supermassive black hole mass of 9.1 Mʘ and a luminosity of 6.8 x 1028 W Hz-1.[8][9] In its spectrum, it shows an inverted and steep spectra, reaching a peak at 18.6 GHz.[7]

In additional, OH 471 also displayed two major flares, visible at higher frequencies of 15 and 8 GHz, in March 2003 and October 2008. Reduced activity was observed in the object with its flux density decreasing following 2009.[6] During 1985 to 1996, the object exhibited an increase in its radio flux with its factor showing a slight increase by 1.6.[10]

Observations by Very Long Baseline Interferometry found the object has a core-jet morphology.[11][12] Based on radio images, the source is compact. Its non-linear structure described as a jet, is found to be extended by 8 milliarcseconds to the east direction. The jet also appears as twisted with a bending angle of 50°.[13] Superluminal motion was also implied as the inner jet component displayed an estimated core separation of 0.76 ± 0.11c.[14] A nuclear region was detected, containing most of the flux density. There is a resolved radio core extending along a position angle of 81°, which is further broken up into two individual circular nuclear components with a separation of 0.76 mas.[15][16] A fainter component can be seen west from the core.[17]

Digicon and image-tube spectroscopy of the spectrum of OH 471, found there are 89 absorption lines. Four absorption-line redshift systems are identified. Based on results, they are located at redshifts (z) 3.122, 3.191, 3.246 and 3.343.[1]

References

  1. ↑ 1.0 1.1 Carswell, R. F.; Strittmatter, P. A.; Williams, R. E.; Beaver, E. A.; Harms, R. (1975-01-01). "The spectrum of OH 471 (0642+44).". The Astrophysical Journal 195: 269–277. doi:10.1086/153326. ISSN 0004-637X. Bibcode: 1975ApJ...195..269C. https://articles.adsabs.harvard.edu/pdf/1975ApJ...195..269C. 
  2. ↑ Oke, J. B. (April 1974). "Photoelectric Spectrophotometry of OQ 172 and OH 471". The Astrophysical Journal 189: L47. doi:10.1086/181461. ISSN 0004-637X. Bibcode: 1974ApJ...189L..47O. https://adsabs.harvard.edu/full/1974ApJ...189L..47O. 
  3. ↑ Schneider, Donald P.; van Gorkom, J. H.; Schmidt, Maarten; Gunn, James E. (May 1992). "Radio properties of optically selected high-redshift quasars. I - VLA observations of 22 quasars at 6 CM". The Astronomical Journal 103: 1451. doi:10.1086/116159. ISSN 0004-6256. Bibcode: 1992AJ....103.1451S. https://articles.adsabs.harvard.edu/pdf/1992AJ....103.1451S. 
  4. ↑ "The Edge of Night - TIME". 2008-12-14. http://www.time.com/time/magazine/article/0,9171,945213,00.html. 
  5. ↑ Bloom, Steven D.; Marscher, Alan P.; Moore, E. M.; Gear, Walter; Terasranta, Harri; Valtaoja, Esko; Aller, Hugh D.; Aller, Margo F. (May 1999). "Multiwaveband Observations of Quasars with Flat Radio Spectra and Strong Millimeter-Wave Emission". The Astrophysical Journal Supplement Series 122 (1): 1–27. doi:10.1086/313204. ISSN 0067-0049. Bibcode: 1999ApJS..122....1B. https://iopscience.iop.org/article/10.1086/313204/fulltext/. 
  6. ↑ 6.0 6.1 Guo, S.; An, T.; Liu, Y.; Sotnikova, Y.; Volvach, A.; Mufakharov, T.; Chen, L.; Cui, L. et al. (2024-05-01). "Magnetically driven relativistic jet in the high-redshift blazar OH 471" (in en). Astronomy & Astrophysics 685: L11. doi:10.1051/0004-6361/202449934. ISSN 0004-6361. Bibcode: 2024A&A...685L..11G. https://www.aanda.org/articles/aa/full_html/2024/05/aa49934-24/aa49934-24.html. 
  7. ↑ 7.0 7.1 Torniainen, I.; Tornikoski, M.; Teräsranta, H.; Aller, M. F.; Aller, H. D. (2005-05-13). "Long term variability of gigahertz-peaked spectrum sources and candidates". Astronomy & Astrophysics 435 (3): 839–856. doi:10.1051/0004-6361:20041886. ISSN 0004-6361. Bibcode: 2005A&A...435..839T. https://www.aanda.org/articles/aa/pdf/2005/21/aa1886-04.pdf. 
  8. ↑ Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Gonzalez, J. Becerra; Bellazzini, R. et al. (February 2017). "Gamma-Ray Blazars within the First 2 Billion Years" (in en). The Astrophysical Journal Letters 837 (1): L5. doi:10.3847/2041-8213/aa5fff. ISSN 2041-8205. Bibcode: 2017ApJ...837L...5A. 
  9. ↑ O’Sullivan, S. P.; Gabuzda, D. C.; Gurvits, L. I. (2011-06-13). "Multifrequency polarization properties of 10 quasars on decaparsec scales at z > 3". Monthly Notices of the Royal Astronomical Society 415 (4): 3049–3064. doi:10.1111/j.1365-2966.2011.18915.x. ISSN 0035-8711. Bibcode: 2011MNRAS.415.3049O. 
  10. ↑ Nesterov, N. S.; Volvach, A. E.; Pogrebenko, S. V. (2002-10-01). "WSRT observations of the quasar OH 471" (in en). Astronomy Letters 28 (10): 656–659. doi:10.1134/1.1512222. ISSN 1562-6873. Bibcode: 2002AstL...28..656N. https://adsabs.harvard.edu/full/2002AstL...28..656N. 
  11. ↑ Nesterov, N. S.; Volvach, A. E. (2002-11-01). "Studies of the quasar OH 471" (in en). Astronomy Letters 28 (11): 721–726. doi:10.1134/1.1518710. ISSN 1562-6873. Bibcode: 2002AstL...28..721N. https://adsabs.harvard.edu/full/2002AstL...28..721N. 
  12. ↑ Xu, W.; Readhead, A. C. S.; Pearson, T. J.; Polatidis, A. G.; Wilkinson, P. N. (1995-08-01). "The First Caltech--Jodrell Bank VLBI Survey. III. VLBI and MERLIN Observations at 5 GHz and VLA Observations at 1.4 GHz". The Astrophysical Journal Supplement Series 99: 297. doi:10.1086/192189. ISSN 0067-0049. Bibcode: 1995ApJS...99..297X. https://articles.adsabs.harvard.edu/pdf/1995ApJS...99..297X. 
  13. ↑ Gurvits, L. I.; Kardashev, N. S.; Popov, M. V.; Schilizzi, R. T.; Barthel, P. D.; Pauliny-Toth, I. I. K.; Kellermann, K. I. (1992-07-01). "The compact radio structure of the high redshift quasars 0642+449, 1402+044, 1614+051". Astronomy and Astrophysics 260: 82–88. ISSN 0004-6361. Bibcode: 1992A&A...260...82G. https://articles.adsabs.harvard.edu/pdf/1992A%26A...260...82G. 
  14. ↑ Lister, M. L.; Cohen, M. H.; Homan, D. C.; Kadler, M.; Kellermann, K. I.; Kovalev, Y. Y.; Ros, E.; Savolainen, T. et al. (2009-12-01). "MOJAVE: Monitoring of Jets in Active Galactic Nuclei with VLBA Experiments. VI. Kinematics Analysis of a Complete Sample of Blazar Jets". The Astronomical Journal 138 (6): 1874–1892. doi:10.1088/0004-6256/138/6/1874. ISSN 0004-6256. Bibcode: 2009AJ....138.1874L. https://iopscience.iop.org/article/10.1088/0004-6256/138/6/1874/pdf. 
  15. ↑ Lobanov, A. P.; Gómez, J. L.; Bruni, G.; Kovalev, Y. Y.; Anderson, J.; Bach, U.; Kraus, A.; Zensus, J. A. et al. (November 2015). "RadioAstron space VLBI imaging of polarized radio emission in the high-redshift quasar 0642+449 at 1.6 GHz". Astronomy & Astrophysics 583: A100. doi:10.1051/0004-6361/201526335. ISSN 0004-6361. Bibcode: 2015A&A...583A.100L. https://www.aanda.org/articles/aa/pdf/2015/11/aa26335-15.pdf. 
  16. ↑ Xu, Ming H.; Heinkelmann, Robert; Anderson, James M.; Mora-Diaz, Julian; Schuh, Harald; Wang, Guang L. (2016-10-31). "The Source Structure of 0642+449 Detected from the Cont14 Observations". The Astronomical Journal 152 (5): 151. doi:10.3847/0004-6256/152/5/151. ISSN 0004-6256. Bibcode: 2016AJ....152..151X. 
  17. ↑ Dodson, R.; Fomalont, E. B.; Wiik, K.; Horiuchi, S.; Hirabayashi, H.; Edwards, P. G.; Murata, Y.; Asaki, Y. et al. (April 2008). "The VSOP 5 GHz Active Galactic Nucleus Survey. V. Imaging Results for the Remaining 140 Sources". The Astrophysical Journal Supplement Series 175 (2): 314–355. doi:10.1086/525025. ISSN 0067-0049. Bibcode: 2008ApJS..175..314D. https://iopscience.iop.org/article/10.1086/525025/fulltext/. 

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