OH 471
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| OH 471 | |
|---|---|
 The quasar/blazar OH 471. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Auriga |
| Right ascension | 06h 46m 32.0260s |
| Declination | +44° 51′ 16.590″ |
| Redshift | 3.396000 |
| Heliocentric radial velocity | 1,018,295 km/s |
| Distance | 11.442 Gly |
| Apparent magnitude (V) | 18.49 |
| Apparent magnitude (B) | 19.57 |
| Characteristics | |
| Type | Opt. 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]
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 M☉ and a luminosity of 6.8 × 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 2 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. Bibcode:1975ApJ...195..269C. doi:10.1086/153326. ISSN 0004-637X.
- ↑ Oke, J. B. (April 1974). "Photoelectric Spectrophotometry of OQ 172 and OH 471". The Astrophysical Journal. 189: L47. Bibcode:1974ApJ...189L..47O. doi:10.1086/181461. hdl:2060/19740019233. ISSN 0004-637X.
- ↑ 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. Bibcode:1992AJ....103.1451S. doi:10.1086/116159. ISSN 0004-6256.
- ↑ "The Edge of Night - TIME". 2008-12-14. Archived from the original on 14 December 2008. Retrieved 2025-03-30.
- ↑ 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. arXiv:astro-ph/9812089. Bibcode:1999ApJS..122....1B. doi:10.1086/313204. ISSN 0067-0049.
- 1 2 Guo, S.; An, T.; Liu, Y.; Sotnikova, Y.; Volvach, A.; Mufakharov, T.; Chen, L.; Cui, L.; Wang, A.; Xu, Z.; Zhang, Y.; Xu, W.; Kovalev, Y. A.; Kovalev, Y. Y.; Kharinov, M. (2024-05-01). "Magnetically driven relativistic jet in the high-redshift blazar OH 471". Astronomy & Astrophysics. 685: L11. arXiv:2404.16343. Bibcode:2024A&A...685L..11G. doi:10.1051/0004-6361/202449934. ISSN 0004-6361.
- 1 2 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" (PDF). Astronomy & Astrophysics. 435 (3): 839–856. Bibcode:2005A&A...435..839T. doi:10.1051/0004-6361:20041886. ISSN 0004-6361.
- ↑ Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Gonzalez, J. Becerra; Bellazzini, R.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonino, R.; Bottacini, E.; Bregeon, J.; Bruel, P. (February 2017). "Gamma-Ray Blazars within the First 2 Billion Years". The Astrophysical Journal Letters. 837 (1): L5. arXiv:1702.04006. Bibcode:2017ApJ...837L...5A. doi:10.3847/2041-8213/aa5fff. ISSN 2041-8205.
- ↑ 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. arXiv:1202.2193. Bibcode:2011MNRAS.415.3049O. doi:10.1111/j.1365-2966.2011.18915.x. ISSN 0035-8711.
- ↑ Nesterov, N. S.; Volvach, A. E.; Pogrebenko, S. V. (2002-10-01). "WSRT observations of the quasar OH 471". Astronomy Letters. 28 (10): 656–659. Bibcode:2002AstL...28..656N. doi:10.1134/1.1512222. ISSN 1562-6873.
- ↑ Nesterov, N. S.; Volvach, A. E. (2002-11-01). "Studies of the quasar OH 471". Astronomy Letters. 28 (11): 721–726. Bibcode:2002AstL...28..721N. doi:10.1134/1.1518710. ISSN 1562-6873.
- ↑ 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. Bibcode:1995ApJS...99..297X. doi:10.1086/192189. ISSN 0067-0049.
- ↑ 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. Bibcode:1992A&A...260...82G. ISSN 0004-6361.
- ↑ Lister, M. L.; Cohen, M. H.; Homan, D. C.; Kadler, M.; Kellermann, K. I.; Kovalev, Y. Y.; Ros, E.; Savolainen, T.; Zensus, J. A. (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. arXiv:0909.5100. Bibcode:2009AJ....138.1874L. doi:10.1088/0004-6256/138/6/1874. ISSN 0004-6256.
- ↑ Lobanov, A. P.; Gómez, J. L.; Bruni, G.; Kovalev, Y. Y.; Anderson, J.; Bach, U.; Kraus, A.; Zensus, J. A.; Lisakov, M. M.; Sokolovsky, K. V.; Voytsik, P. A. (November 2015). "RadioAstron space VLBI imaging of polarized radio emission in the high-redshift quasar 0642+449 at 1.6 GHz" (PDF). Astronomy & Astrophysics. 583: A100. arXiv:1504.04273. Bibcode:2015A&A...583A.100L. doi:10.1051/0004-6361/201526335. ISSN 0004-6361.
- ↑ 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. arXiv:1607.04706. Bibcode:2016AJ....152..151X. doi:10.3847/0004-6256/152/5/151. ISSN 0004-6256.
- ↑ Dodson, R.; Fomalont, E. B.; Wiik, K.; Horiuchi, S.; Hirabayashi, H.; Edwards, P. G.; Murata, Y.; Asaki, Y.; Moellenbrock, G. A.; Scott, W. K.; Taylor, A. R.; Gurvits, L. I.; Paragi, Z.; Frey, S.; Shen, Z.-Q. (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. arXiv:0710.5707. Bibcode:2008ApJS..175..314D. doi:10.1086/525025. ISSN 0067-0049.
