QSO B1611+343
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| QSO B1611+343 | |
|---|---|
 The blazar QSO B1611+343. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Corona Borealis |
| Right ascension | 16h 13m 41.0642s |
| Declination | +34° 12′ 47.909″ |
| Redshift | 1.398040 |
| Heliocentric radial velocity | 419,122 km/s |
| Distance | 8.809 Gly |
| Apparent magnitude (V) | 17.46 |
| Apparent magnitude (B) | 17.98 |
| Characteristics | |
| Type | FSRQ, blazar |
| Other designations | |
| DA 406, WMAP 23, QSO J1613+3412, LHE 403, 6C 161147+342017, SDSS J161341.06+341247.8, OHIO S 319, INTREF 677, PGC 4062791 | |
QSO B1611+343 also known as DA 406, is a blazar located in the northern constellation of Corona Borealis. Its redshift is (z) 1.4 and it is classified as an optically violent variable quasar or an OVV quasar although lowly polarized.[1][2] Its radio spectrum is flat, making it a flat-spectrum source with a spectral index of -0.04.[3][4]
QSO B1611+343 is variable on the electromagnetic spectrum, showing a low-frequency radio outburst in 1987 and temporal significant variations.[5][6] In the 1983–1991 period it displayed optical fluxes ranging from 0.27 to 0.7 mJy with a short-term flickering period recorded on time scales between February 28, 1995 and 8 April 1996.[2][7] A near-infrared flare was detected in June 2012 by astronomers during the monitoring of gamma ray sources by the Fermi Gamma-ray Space Telescope.[8] The light curves of the object showed it to be moderately variable at 2.7, 4.9 and 8.0 GHz frequencies, exhibiting a major flux surging below 880 MHz.[9]
QSO B1611+343 is described as a powerful core-dominated source. When imaged by the Very Large Array, it is found to have a triple morphology with its southern extension being consistent with the position angle of a bright component located in the south.[10][1] Results of the snapshot observations at 92 centimeters by Very Long Baseline Interferometry (VLBI) showed the source is fully resolved with a diffused component containing 37% of the flux density.[11] On milliarcsecond scales at 2.32 GHz observed by VLBI, the radio core is found to be elongated and exposed, measuring 3 milliarcseconds in diameter.[12] This core also has the highest rotation measure, starting at −519±55 rad m–2 before declining to −44±55 rad m−2 upon reaching 10 parsecs within it.[13]
The jet of QSO B1611+343 in multi-epoch observations is moving in a southerly direction, subsequently terminating at a bright diffused component located 2.9 milliarcseconds from the core.[14] When imaged in high resolution observations by VLBI, it bends eastwards by 3 milliarcseconds, displaying superluminal motion.[4][15] Based on observations it contains at least four components; all of them moving at apparent speeds of 6.7±1.6, 3.8±1.4, 7.6±1.3 and 11.5±2.3 h−1 c.[1] Polarized weak flux was also discovered southwards from one of the components, likely associated with a stationary oblique shock, causing the jet to change its trajectory.[16]
The supermassive black hole in QSO B1611+343 has a mass of 9.69 ± 0.02, estimated from a singly ionized magnesium line. Based on studies, its accretion rate should be approximately M0.9 = 5.3 M☉ yr−1 and Log M0.9982 = 3.7 M☉ yr−1.[17]
References
- 1 2 3 Piner, B. Glenn; Kingham, Kerry A. (1997-04-20). "VLBI Observations of the Gamma-Ray Blazar 1611+343". The Astrophysical Journal. 479 (2): 684–693. Bibcode:1997ApJ...479..684P. doi:10.1086/303919. ISSN 0004-637X.
- 1 2 Villata, M.; Raiteri, C. M.; Ghisellini, G.; de Francesco, G.; Bosio, S.; Latini, G.; Bucciarelli, B.; Chiaberge, M.; Chiumiento, G.; Cora, A.; Lanteri, L.; Lattanzi, M. G.; Massone, G.; Peila, A.; Racioppi, F. (January 1997). "Optical photometric monitoring of γ-ray loud blazars. I. Observations from November 1994 to November 1995" (PDF). Astronomy and Astrophysics Supplement Series. 121: 119–138. doi:10.1051/aas:1997313. ISSN 0365-0138.
- ↑ M., Neumann; W., Reich; E., Fuerst; W., Brinkmann; P., Reich; J., Siebert; R., Wielebinski; J., Truemper (August 1994). "Multifrequency observations of ROSAT selected radio sources". Astronomy and Astrophysics Supplement Series. 106. ISSN 0365-0138. Archived from the original on 2022-06-10. Retrieved 2025-04-13.
- 1 2 An, Tao; Hong, Xiao-Yu; Wang, Wei-Hua; Jiang, Dong-Rong; Chen, Yong-Jun (August 2001). "VLBI Observations of the Blazar 1611+343 at 5 GHz" (PDF). Chinese Journal of Astronomy and Astrophysics. 1 (4): 305–312. Bibcode:2001ChJAA...1..305A. doi:10.1088/1009-9271/1/4/305. ISSN 1009-9271.
- ↑ Altschuler, D. R.; Dennison, B. K.; Mitchell, K. J.; O'Dell, S. L.; Broderick, J. J.; Condon, J. J.; Payne, H. E. (1987). "The Low Frequency Variability of Extragalactic Radio Sources". Observational Evidence of Activity in Galaxies. 121: 211. Bibcode:1987IAUS..121..211A. ISSN 1743-9221.
- ↑ O'Dell, S. L.; Broderick, J. J.; Dennison, B.; Mitchell, K. J.; Altschuler, D. R.; Condon, J. J.; Payne, H. E. (March 1983). "Temporal Variations of Extragalactic Radio Sources between 0.3 and 1.4 GHz". Bulletin of the American Astronomical Society. 15: 659. Bibcode:1983BAAS...15..659O.
- ↑ Villata, M.; Raiteri, C. M.; Ghisellini, G.; Francesco, G. De; Bosio, S.; Latini, G.; Bucciarelli, B.; Chiaberge, M.; Chiumiento, G.; Cora, A.; Lanteri, L.; Lattanzi, M. G.; Massone, G.; Peila, A.; Racioppi, F. (1997-01-01). "Optical photometric monitoring of γ-ray loud blazars. - I. Observations from November 1994 to November 1995" (PDF). Astronomy and Astrophysics Supplement Series. 121 (1): 119–138. doi:10.1051/aas:1997313. ISSN 0365-0138.
- ↑ Carrasco, L.; Escobedo, G.; Porras, A.; Recillas, E.; Mayya, D. Y.; Carraminana, A. (June 2012). "NIR brightening of the QSO HB891611+343". The Astronomer's Telegram. 4203: 1. Bibcode:2012ATel.4203....1C.
- ↑ Altschuler, D. R.; Broderick, J. J.; Condon, J. J.; Dennison, B.; Mitchell, K. J.; O'Dell, S. L.; Payne, H. E. (December 1984). "Multifrequency light-curves of low-frequency variable radio sources". The Astronomical Journal. 89: 1784–1798. Bibcode:1984AJ.....89.1784A. doi:10.1086/113687. ISSN 0004-6256.
- ↑ Murphy, D. W.; Browne, I. W. A.; Perley, R. A. (September 1993). "VLA observations of a complete sample of core-dominated radio sources". Monthly Notices of the Royal Astronomical Society. 264 (2): 298–318. doi:10.1093/mnras/264.2.298. ISSN 0035-8711.
- ↑ R., Altschuler, D.; I., Gurvits, L.; W., Alef; B., Dennison; D., Graham; S., Trotter, A.; E., Carson, J. (December 1995). "The centi-arcsecond structure of 16 low-frequency variable sources at 92 cm". Astronomy and Astrophysics Supplement Series. 114. ISSN 0365-0138. Archived from the original on 2024-03-27. Retrieved 2025-04-13.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ↑ Fey, Alan L.; Clegg, Andrew W.; Fiedler, Ralph L. (September 1996). "VLBI Observations of Eight Extreme Scattering Event Sources: Milliarcsecond-Scale Structure". The Astrophysical Journal. 468: 543. Bibcode:1996ApJ...468..543F. doi:10.1086/177713. ISSN 0004-637X.
- ↑ Zavala, R. T.; Taylor, G. B. (2003-05-20). "A View through Faraday's Fog: Parsec-Scale Rotation Measures in Active Galactic Nuclei". The Astrophysical Journal. 589 (1): 126–146. arXiv:astro-ph/0302367. Bibcode:2003ApJ...589..126Z. doi:10.1086/374619. ISSN 0004-637X.
- ↑ Jorstad, Svetlana G.; Marscher, Alan P.; Mattox, John R.; Wehrle, Ann E.; Bloom, Steven D.; Yurchenko, Alexei V. (June 2001). "Multiepoch Very Long Baseline Array Observations of EGRET-detected Quasars and BL Lacertae Objects: Superluminal Motion of Gamma-Ray Bright Blazars". The Astrophysical Journal Supplement Series. 134 (2): 181–240. arXiv:astro-ph/0101570. Bibcode:2001ApJS..134..181J. doi:10.1086/320858. ISSN 0067-0049.
- ↑ "Superluminal Motion in the Gamma Ray Blazar 1611+343 | PDF". Scribd. Retrieved 2025-04-13.
- ↑ Lister, Matthew L.; Marscher, Alan P.; Gear, W. K. (1998-09-10). "Submilliarcsecond Polarimetric Imaging of Blazar Jets at 43 GHz". The Astrophysical Journal. 504 (2): 702–719. Bibcode:1998ApJ...504..702L. doi:10.1086/306112. ISSN 0004-637X.
- ↑ Campitiello, Samuele; Ghisellini, Gabriele; Sbarrato, Tullia; Calderone, Giorgio (2018). "How to constrain mass and spin of supermassive black holes through their disk emission". Astronomy & Astrophysics. 612: A59. arXiv:1702.00011. Bibcode:2018A&A...612A..59C. doi:10.1051/0004-6361/201731897. ISSN 0004-6361.
