PKS 2145+067
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| PKS 2145+067 | |
|---|---|
_image.png) SDSS image of PKS 2145+067 | |
| Observation data (J2000.0 epoch) | |
| Constellation | Pegasus |
| Right ascension | 21h 48m 05.45s[1] |
| Declination | +06° 57′ 38.60″[1] |
| Redshift | 1.003000[1] |
| Heliocentric radial velocity | 300,692 km/s[1] |
| Distance | 7.527 Gly |
| Apparent magnitude (V) | 16.47 |
| Apparent magnitude (B) | 16.85 |
| Characteristics | |
| Type | Opt.var.; LPQ FSRQ[1] |
| Other designations | |
| 4C +06.69, PKS 2145+06, 2MASS J21480545+0657386, LEDA 2818722, PMN J2148+0657, NVSS J214805+065739, DA 562, OX +076.1, PAPER J327.74+07.03, WMAP 037, RX J2148.0+0657, JVAS J2148+0657[1] | |
PKS 2145+067 is a radio-loud quasar[2] located in the constellation of Pegasus. It has a redshift of (z) 1.003[1] and it was first discovered by astronomers conducting the Parkes Survey at Parkes Observatory in 1966, designated as PKS 2145+06.[3] The radio spectrum of the object is flat, making it a flat-spectrum source, but it is classified as a weakly polarized quasar.[4][5][6]
PKS 2145+067 is classified as a blazar mainly due to its variability on the electromagnetic spectrum, displaying four flares when observed at eight frequency bands between 4.8 and 230 GHz frequencies, and radio flux variations that reaching 2 Jy within 2 hours.[7][8][9] In additional to its flaring activity, it also had weak intensity fluctuations resulting from interstellar scintillation in daily averages of 2695 and 8086 MHz.[10] The X-ray flux of the quasar is known to vary, from 3.3 × 10−12 erg cm−2 s−1 at 0.1 and 2.0 KeV in May 1991 to 3.8 × 10−12 erg cm−2 s−1 in 1994.[2]
The radio structure of PKS 2145+067 is compact. When observed with Very Long Baseline Interferometry (VLBI), the radio core is shown as weakly elongated with no signs of a significant structure.[11] At 5 GHz, it has a strong elongated component towards the south-east direction and another component found diffused with a position angle of 140°. These two components are found embedded in a diffused halo.[6][12] VLBI Observations at 93 centimeters showed the source has some possible structural features that are located 48 and 200 milliarcseconds from the core and a single component roughly containing 30% of its flux density.[13] Geodetic VLBI imaging revealed the object's core has a size of 0.25 milliarcseconds in extent and a brightness temperature of 1.4 × 1012 Kelvin, with extended radio emission orientating at 140°.[14]
The jet of PKS 2145+067 is known to be compact. When observed by Flávio Benevenuto da Silva Junior and Anderson Caproni, the jet was made up of 11 components which are moving at superluminal velocities with speeds between 10c and 18c. The position angles of these components are all estimated between the ranges of 0.03 and 11.29 degrees.[15]
PKS 2145+067 is classified as a Lyman-limit quasar with a detected Lyman-limit system located at the redshift of (z) 0.7913, accompanying several metal-rich absorption lines in various states of low and high ionization.[2][16] X-ray observations by the Advanced Satellite for Cosmology and Astrophysics (ASCA) also showed the quasar has a 0.6-10 KeV spectrum of 1.3 × 10−11 erg cm−2 s-1, best fitted by a power-law model.[2] The host galaxy of PKS 2145+067 is marginally resolved by near-infrared H-band imaging.[17]
References
- 1 2 3 4 5 6 7 "NED search results for PKS 2145+067". NASA/IPAC Extragalactic Database. Retrieved 2025-06-29.
- 1 2 3 4 Yamasaki, Noriko Y.; Ishikawa, Teru; Ohashi, Takaya (October 2000). "ASCA Observation of the Lyman-Limit Quasar PKS 2145+067". Publications of the Astronomical Society of Japan. 52 (5): 763–767. arXiv:astro-ph/0006224. doi:10.1093/pasj/52.5.763. ISSN 0004-6264.
- ↑ Day, G. A.; Shimmins, A. J.; Ekers, R. D.; Cole, D. J. (1966). "The Parkes Catalogue Of Radio Sources Declination Zone 0° To ?20°". Australian Journal of Physics. 19 (6): 837. Bibcode:1966AuJPh..19...35D. doi:10.1071/ph660837. ISSN 0004-9506.
- ↑ Tappe, A.; Black, J. H. (2004-09-01). "High-resolution spectroscopy of flat-spectrum quasars - I. Redshifted emission and absorption in PKS 2145+067". Astronomy & Astrophysics. 423 (3): 943–954. doi:10.1051/0004-6361:20035861. ISSN 0004-6361.
- ↑ Drinkwater, M. J.; Webster, R. L.; Francis, P. J.; Condon, J. J.; Ellison, S. L.; Jauncey, D. L.; Lovell, J.; Peterson, B. A.; Savage, A. (1997-01-01). "The Parkes half-jansky flat-spectrum sample". Monthly Notices of the Royal Astronomical Society. 284 (1): 85–125. arXiv:astro-ph/9609019. Bibcode:1997MNRAS.284...85D. doi:10.1093/mnras/284.1.85. ISSN 0035-8711.
- 1 2 Shen, Z.-Q.; Wan, T.-S.; Moran, J. M.; Jauncey, D. L.; Reynolds, J. E.; Tzioumis, A. K.; Gough, R. G.; Ferris, R. H.; Sinclair, M. W. (1997-09-14), "A 5-GHZ Southern Hemishere VLBI Survey of Compact Radio Sources.I.", The Astronomical Journal, 114: 1999, arXiv:astro-ph/9709128, Bibcode:1997AJ....114.1999S, doi:10.1086/118621
- ↑ Plavin, Alexander; Kovalev, Yuri Y; Kovalev, Yuri A; Troitsky, Sergey (2021-07-08). "Radio astronomy locates the neutrino origin in bright blazars". Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021). Trieste, Italy: Sissa Medialab. p. 967. doi:10.22323/1.395.0967.
- ↑ Hovatta, T.; Nieppola, E.; Tornikoski, M.; Valtaoja, E.; Aller, M. F.; Aller, H. D. (2008-05-09), "Long-term radio variability of AGN: Flare characteristics", Astronomy & Astrophysics, 485 (1): 51–61, arXiv:0805.1283, Bibcode:2008A&A...485...51H, doi:10.1051/0004-6361:200809806
- ↑ Volvach, A. E.; Bychkova, V. S.; Kardashev, N. S.; Larionov, M. G.; Vlasyuk, V. V.; Spiridonova, O. I. (May 2009). "Fast brightness variations of blazars in the radio and optical". Astronomy Reports. 53 (5): 401–409. Bibcode:2009ARep...53..401V. doi:10.1134/S1063772909050035. ISSN 0004-6299.
- ↑ Condon, J. J.; Backer, D. C. (April 1975). "Interstellar scintillation of extragalactic radio sources". The Astrophysical Journal. 197: 31–38. Bibcode:1975ApJ...197...31C. doi:10.1086/153485. ISSN 0004-637X.
- ↑ Rantakyrö, F. T.; Backer, D. C.; Booth, R. S.; Carlstrom, J. E.; Emerson, D. T.; Grewing, M.; Hirabayashi, H.; Hodges, M. W.; Inoue, M.; Kobayashi, H.; Krichbaum, T. P.; Kus, A. J.; Moran, J. M.; Morimoto, M.; Padin, S. (1998-09-01). "50 μas resolution VLBI images of AGN's at λ3 mm" (PDF). Astronomy and Astrophysics Supplement Series. 131 (3): 451–467. Bibcode:1998A&AS..131..451R. doi:10.1051/aas:1998282. ISSN 0365-0138.
- ↑ Wehrle, Ann E.; Cohen, Marshall H.; Unwin, Stephen C.; Aller, Hugh D.; Aller, Margo F.; Nicolson, George (June 1992). "The Milliarcsecond Structure of Highly Variable Radio Sources". The Astrophysical Journal. 391: 589. Bibcode:1992ApJ...391..589W. doi:10.1086/171373. ISSN 0004-637X.
- ↑ Altschuler, D. R.; Gurvits, L. I.; Alef, W.; Dennison, B.; Graham, D.; Trotter, A. S.; Carson, J. E. (December 1995). "The centi-arcsecond structure of 16 low-frequency variable sources at 92 cm". Astronomy and Astrophysics Supplement Series. 114: 197. ISSN 0365-0138.
- ↑ Airapetyan, E. A.; Matveenko, L. I. (January 1997). "The fine structure of compact radio sources from geodetic data". Astronomy Letters. 23 (1): 64–70. ISSN 0320-0108.
- ↑ Benevenuto da Silva Junior, Flávio; Caproni, Anderson (2023). "Kinematic study of the relativistic jets of the blazars AO 0235+164 and PKS 2145+067" (PDF). Boletim da Sociedade Astronômica Brasileira. 1 (34): 219–220.
- ↑ Bergeron, Jacqueline; Petitjean, Patrick; Sargent, W. L. W.; Bahcall, John N.; Boksenberg, Alec; Hartig, George F.; Jannuzi, Buell T.; Kirhakos, Sofia; Savage, Blair D.; Schneider, Donald P.; Turnshek, David A.; Weymann, Ray J.; Wolfe, Arthur M. (November 1994). "The Hubble Space Telescope Quasar Absorption Line Key Project. VI. Properties of the Metal-rich Systems". The Astrophysical Journal. 436: 33. Bibcode:1994ApJ...436...33B. doi:10.1086/174878. ISSN 0004-637X.
- ↑ Kotilainen, Jari K.; Falomo, Renato; Scarpa, Riccardo (April 1998). "Near-infrared imaging of the host galaxies of flat spectrum radio quasars". Astronomy and Astrophysics. 332: 503–513. arXiv:astro-ph/9711065. Bibcode:1998A&A...332..503K. ISSN 0004-6361.
