QSO B0133+476
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| QSO B0133+476 | |
|---|---|
 The blazar QSO B0133+476. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Andromeda |
| Right ascension | 01h 36m 58.5948s |
| Declination | +47° 51′ 29.100″ |
| Redshift | 0.859000 |
| Heliocentric radial velocity | 257,522 km/s |
| Distance | 6.916 Gly |
| Apparent magnitude (V) | 19.50 |
| Characteristics | |
| Type | HPQ; Blazar, FSRQ |
| Other designations | |
| Mis V1436, OHIO C 457, DA 55, NVSS J013658+475129, S5 0133+47, WMAP 80, QSO J0136+4751, [MGL2009] BZQ J0136+4751, [HB93] 0133+476 | |
QSO B0133+476, alternatively known as DA 55, is a blazar[1] located in the constellation of Andromeda. Its redshift is (z) 0.859[2][3] and it was first discovered as an astronomical radio source by astronomers who conducted a survey at 1.4 GHz in 1970.[4] This object has also been referred to as an optically violent variable (OVV) quasar due to its variability,[5] a BL Lac object[6] and a highly polarized quasar (HPQ).[7]
QSO B0133+476 is in a constant active state.[8][9] It is known to exhibit several outbursts showing longer outburst time scales at longer wavelengths and a recorded amplitude outburst reaching near 15 to 31 GHz, during observations spanning roughly one decade. Its pre-outburst spectrum, found relatively flat between 2.7 and 31.4 GHz, started rising and became inverted during an outburst in between 1973 and 1974. Between 1978 and 1980 it had another outburst with the peak of the spectrum reaching 8 GHz in 1979.5 and 2.7 GHz by 1980.3. When compared to the 1973-1974 outburst, the spectrum was much flatter which it subsequently broadened.[2]
A flare was detected from QSO B0133+476 in the middle of July 2002, with a brightness increase to 14.3 magnitude.[3][10] It was followed by another flare detected from November 2024 during which the flux density rose steadily to 16.1 magnitude between January 20 and 21 2025.[11] Near-infrared activity was detected towards the end of 2008, in 2011 and again in February 2013.[12][13][14]
The source of QSO B0133+476 is classified as double. Based on polarization images presented by Very Long Baseline Interometry, it has a compact radio structure, mainly comprising an elongated strong radio core, a faint weak secondary component that is located 3.7 milliarcseconds (mas) from the core and signs of an extended diffused structure in the west direction.[15] Observations also showed most of the radio emission is contained within the core,[16] which in turn has a flat spectrum and a rest-frame rotation measure of -1420 ± 56 rad m−2.[17] When imaged by the Very Long Baseline Array (VLBA) at 1.7, 4.8 and 8.4 GHz frequencies, the source instead shows a core-jet morphology with its emission being dominated by a bright component and a jet resolving into a wiggled tail-like structure.[18]
References
- ↑ Blinov, D.; Myserlis, I.; Angelakis, E.; King, O.; Pavlidou, V. (February 2013). "Optical and gamma-ray brightening of blazar OC 457". The Astronomer's Telegram. 4779: 1. Bibcode:2013ATel.4779....1B.
- 1 2 O'Dea, Christopher P.; Dent, William A.; Kinzel, Wayne M.; Balonek, Thomas J. (December 1986). "Multifrequency radio observations of the variable quasars 0133+476, 0235+164, 1749+096, and 2131-021". The Astronomical Journal. 92: 1262–1271. Bibcode:1986AJ.....92.1262O. doi:10.1086/114260. ISSN 0004-6256.
- 1 2 Yoshida, S.; Ohkura, N.; Nakashima, Y.; Greaves, J.; Bouma, R. J. (February 2008). "QSO 0133+476". Central Bureau Electronic Telegrams (1249): 1. Bibcode:2008CBET.1249....1Y.
- ↑ Andrew, B. H.; Kraus, J. D. (January 1970). "Radio Sources with Flat Spectra". The Astrophysical Journal. 159: L45 – L50. Bibcode:1970ApJ...159L..45A. doi:10.1086/180475. ISSN 0004-637X.
- ↑ "MisV1436: Discovery of Optically Violently Variable Quasar QSO B0133+47". MISAO Project. Retrieved 2025-04-12.
- ↑ Balonek, T. J.; O'Dea, C. P.; Dent, W. A.; Kinzel, W. M. (September 1984). "Multifrequency Radio Observations of Four BL Lacertae Objects". Bulletin of the American Astronomical Society. 16: 952. Bibcode:1984BAAS...16..952B.
- ↑ Hovatta, T.; Lehto, H. J.; Tornikoski, M. (2008-07-17). "Wavelet analysis of a large sample of AGN at high radio frequencies" (PDF). Astronomy & Astrophysics. 488 (3): 897–903. arXiv:0807.1796. Bibcode:2008A&A...488..897H. doi:10.1051/0004-6361:200810200. ISSN 0004-6361.
- ↑ "The blazar S4 0133+47: new flash with R~15.4 magnitude". The Astronomer's Telegram. Retrieved 2025-04-12.
- ↑ "The blazar S4 0133+47 in a flaring state with R~16.1 magnitude". The Astronomer's Telegram. Retrieved 2025-04-12.
- ↑ Carramiñana, A.; Carrasco, L. (November 2009). "Optical and near infrared studies of γ-ray bright WMAP sources" (PDF). A Long Walk Through Astronomy: A Celebration of Luis Carrasco's 60th Birthday - Revista Mexicana de Astronomía y Astrofísica. 37: 132–137. Bibcode:2009RMxAC..37..132C.
- ↑ "The blazar S4 0133+47: the brightest flare since 2023 September and still growing up". The Astronomer's Telegram. Retrieved 2025-04-12.
- ↑ Carraminana, Alberto; Carrasco, Luis; Porras, Alicia; Recillas, Elsa (2010). "Extensive near infrared monitoring of millimeter-wave / Gamma-ray bright blazars". arXiv:1001.0204 [astro-ph.HE].
- ↑ Carrasco, L.; Carraminana, A.; Escobedo, G.; Porras, A.; Recillas, E.; Mayya, Y. D.; Valdes, J. R. (February 2011). "NIR Flaring of the Blazar BZQ J0136+4751". The Astronomer's Telegram. 3157: 1. Bibcode:2011ATel.3157....1C.
- ↑ Carrasco, L.; Valdes, J. R.; Recillas, E.; Porras, A.; Carraminana, A. (February 2013). "NIR Flare of the quasar HB890133+476". The Astronomer's Telegram. 4791: 1. Bibcode:2013ATel.4791....1C.
- ↑ Cawthorne, T. V.; Wardle, J. F. C.; Roberts, D. H.; Gabuzda, D. C.; Brown, L. F. (October 1993). "Milliarcsecond Polarization Structure of 24 Objects from the Pearson-Readhead Sample of Bright Extragalactic Radio Sources. I. The Images". The Astrophysical Journal. 416: 496. Bibcode:1993ApJ...416..496C. doi:10.1086/173253. ISSN 0004-637X.
- ↑ Scott, W. K.; Fomalont, E. B.; Horiuchi, S.; Lovell, J. E. J.; Moellenbrock, G. A.; Dodson, R. G.; Edwards, P. G.; Coldwell, G. V.; Fodor, S.; Frey, S.; Gurvits, L. I.; Hirabayashi, H.; Lister, M. L.; Mosoni, L.; Murata, Y. (November 2004). "The VSOP 5 GHz Active Galactic Nucleus Survey. III. Imaging Results for the First 102 Sources". The Astrophysical Journal Supplement Series. 155 (1): 33–72. arXiv:astro-ph/0407041. Bibcode:2004ApJS..155...33S. doi:10.1086/424819. hdl:1959.3/404. ISSN 0067-0049.
- ↑ 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.
- ↑ Rossetti, A.; Mantovani, F.; Dallacasa, D.; Fanti, C.; Fanti, R. (2005-05-01). "Multi-frequency VLBA observations of compact sources from the Peacock and Wall catalogue" (PDF). Astronomy & Astrophysics. 434 (2): 449–458. arXiv:astro-ph/0501407. Bibcode:2005A&A...434..449R. doi:10.1051/0004-6361:20041661. ISSN 0004-6361.
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