QSO B0153+744
| QSO B0153+744 | |
|---|---|
 The quasar QSO B0153+744. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Cassiopeia |
| Right ascension | 01h 57m 34.964s |
| Declination | +74° 42′ 43.230″ |
| Redshift | 2.338000 |
| Heliocentric radial velocity | 700,915 km/s |
| Distance | 10.512 Gly |
| Apparent magnitude (V) | 16.0 |
| Apparent magnitude (B) | 16.0 |
| Characteristics | |
| Type | LPQ, RLQ |
| Other designations | |
| S5 0153+74, NVSS J015735+744241, QSO J0157+1442, RORF 0153+744, 1RXS J015735.2+744246, [HB89] 0153+744 | |
QSO B0153+744 is a quasar[1] located in the constellation of Cassiopeia. It has a redshift of (z) 2.338[2] and has an optical brightness of mR = 17.5 magnitude.[3] It was first discovered as an astronomical radio source in 1988. The radio spectrum of the source appears as flat when seen at centimeter wavelengths but optically thin at millimeter wavelengths.[1] This object is also classified as radio-loud and exhibits low polarization, making it a low polarized quasar (LPQ).[4]
Description
[edit]The radio source of QSO B0153+744 is found to be both one-sided[5] and complex.[6] However, when shown at both frequencies, it is revealed as double source that is embedded inside a halo.[7] In its radio structure, the 15.4 GHz emission is found to be dominated by two main components with a separation gap of 10 milliarcseconds.[5] These two main components are classified as the northern component and southern component respectively. The northern component contains an inverted spectrum whereas the southern component has a steep spectra.[7]
In 1997, these two components of QSO B0153+744 were studied further. This in turn, were confirmed as a jet-core component and a bright secondary component. The former shows core-jet structure made up of four distinctive components, when resolved at 1.3 centimeter (cm) wavelengths whereas the latter is stationary and exhibits a complicated structure. Further evidence shows the spectral index of the bright component's emission is near to one of the steep-spectrum jet components at ranges between 6 cm and 3.6 cm.[2]
A strong one-sided jet is present in QSO B0153+744 with its projected direction changing by an 180° angle.[8][2] There are three other sub-components present (the jet's innermost regions). The two sub-components are shown trailing the jet's direction with a switch of 65° ± 3° at distance r = (0.65 ± 0.05) mas to 88° ± 8° at distance r = (1.35 ± 0.05) mas, while the third sub-component is trailing the jet's outermost regions.[5] Based on the jet's speed and its change of direction, this indicates the radio source of QSO B0153+744 is relatively young.[9]
References
[edit]- ^ a b Hummel, C. A.; Schalinski, C. J.; Krichbaum, T. P.; Witzel, A.; Johnston, K. J. (1988-10-01). "The quasar 0153+74". Astronomy and Astrophysics. 204: 68–72. Bibcode:1988A&A...204...68H. ISSN 0004-6361.
- ^ a b c Hummel, C. A.; Krichbaum, T. P.; Witzel, A.; Wuellner, K. H.; Steffen, W.; Alef, W.; Fey, A. (1997-08-01). "The radio jet of quasar 0153+744". Astronomy and Astrophysics. 324: 857–869. Bibcode:1997A&A...324..857H. ISSN 0004-6361.
- ^ Stickel, M.; Kuehr, H. (1996). "Optical identifications of radio sources from the 1Jy, S4 and S5 catalogues". Astronomy & Astrophysics Supplement Series. 115: 11–40. Bibcode:1996A&AS..115...11S.
- ^ Minev, Milen; Trifonov, Trifon; Ivanov, Valentin D; Ovcharov, Evgeni; Bozhilov, Vladimir; Valcheva, Antoniya; Kostov, Andon; Nedialkov, Petko (2024-06-14). "Results of a long-term optical variability study of 11 quasars and VRI photometry of comparison stars". Monthly Notices of the Royal Astronomical Society. 531 (4): 4746–4761. doi:10.1093/mnras/stae1479. ISSN 0035-8711.
- ^ a b c Pérez-Torres, M. A.; Marcaide, J. M.; Guirado, J. C.; Ros, E. (December 2004). "Absolute kinematics of radio source components in the complete S5 polar cap sample - II. First and second epoch maps at 15 GHz" (PDF). Astronomy & Astrophysics. 428 (3): 847–866. arXiv:astro-ph/0408581. Bibcode:2004A&A...428..847P. doi:10.1051/0004-6361:20040423. ISSN 0004-6361.
- ^ Britzen, S.; Vermeulen, R. C.; Taylor, G. B.; Campbell, R. M.; Pearson, T. J.; Readhead, A. C. S.; Xu, W.; Browne, I. W. A.; Henstock, D. R.; Wilkinson, P. (2007-05-10). "A multi-epoch VLBI survey of the kinematics of CJF sources" (PDF). Astronomy & Astrophysics. 472 (3): 763–771. doi:10.1051/0004-6361:20052677. ISSN 0004-6361.
- ^ a b Pearson, T. J.; Readhead, A. C. S. (May 1988). "The milliarcsecond structure of a complete sample of radio sources. II - First-epoch maps at 5 GHz". The Astrophysical Journal. 328: 114. Bibcode:1988ApJ...328..114P. doi:10.1086/166274. ISSN 0004-637X.
- ^ Ros, E.; Marcaide, J. M.; Guirado, J. C.; Pérez-Torres, M. A. (September 2001). "Absolute kinematics of radio source components in the complete S5 polar cap sample" (PDF). Astronomy & Astrophysics. 376 (3): 1090–1105. doi:10.1051/0004-6361:20010987. ISSN 0004-6361.
- ^ 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.
