PKS 2134+004
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| PKS 2134+004 | |
|---|---|
 The quasar PKS 2134+004. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Aquarius |
| Right ascension | 21h 36m 38.5863s |
| Declination | +00° 41′ 54.213″ |
| Redshift | 1.941251 |
| Heliocentric radial velocity | 581,972 km/s |
| Distance | 9.945 Gly |
| Apparent magnitude (V) | 17.08 |
| Apparent magnitude (B) | 17.30 |
| Characteristics | |
| Type | Opt. var, LPQ, FSRQ |
| Other designations | |
| PHL 61, OHIO X 057, LEDA 2830964, PKS 2134+008, QSO J2136+0041, DA 553, VSOP J2136+0041 | |
PKS 2134+004 is a distant radio-loud quasar[1] located in the constellation of Aquarius with an approximate magnitude of 18.[2] Its redshift is (z) 1.944 and it is classified as a compact source.[3][4] It was discovered in a survey by A.J. Shimmins in 1968.[5] This object contains a radio spectrum appearing as flat, making it a flat-spectrum radio quasar.[3] The spectrum of the source shows an absorption feature.[6]
PKS 2134+004 is described as a high frequency peaker (HFP) with a core-jet morphology.[7][8][9] It consists of a radio core located in the easternmost region and a jet that is pointing north with a bending angle towards the west, when imaged by the Very Long Baseline Array (VLBA).[7] Based on polarimetric observations by VLBA, the core is found brighter and stronger at 15 GHz with a flat spectral index approximately measured as 0.0 ± 0.1.[10][11] The core also has a polarization level of 0.5% and a Faraday rotation of 1100 rad m−2.[10]
Very Long Baseline Interferometry (VLBI) showed PKS 2134+004 has three components; mainly a compact strong core and two other components having an approximate separation of both 4.0 milliarcseconds at position angle of -152° and 2.5 milliarcseconds at position angle of -122°.[12] Radio emission can be seen surrounding the core on arcsecond scales with a faint bridge reaching the western component.[13][14][15]
PKS 2134+004 displays small variations, usually occurring on time-scales of several years. The radio spectrum of the source is peaked, with its flux density reaching around 8 Jy at 5 GHz frequencies.[16] Light curves of the object showed it be to extremely variable at optical wavelengths and on a millimetre radio light curve, exhibiting two bright radio outbursts that were detected in 1937 and 1949, with its B magnitude reaching a maximum of 14.8.[17][18] Increased gamma ray activity was detected by the Large Area Telescope (LAT) in December 2018.[3][19]
The host of PKS 2134+004 is a massive, luminous elliptical galaxy. Based on studies, it has a color index that is found redder by 0.5 magnitude compared to its nucleus.[20]
References
- ↑ Wolter, A.; Celotti, A. (2001-05-01). "An X-ray selected sample of radio-loud quasars". Astronomy and Astrophysics. 371 (2): 527–537. arXiv:astro-ph/0103394. Bibcode:2001A&A...371..527W. doi:10.1051/0004-6361:20010415. ISSN 0004-6361.
- ↑ Mutoh, M.; Inoue, M.; Kameno, S.; Asada, K. (2003-01-01). "Rotation Measure and Opacity Asymmetry in 2134+004". Publications of the Astronomical Society of Australia. 20 (1): 144–146. Bibcode:2003PASA...20..144M. doi:10.1071/AS03014. ISSN 1323-3580.
- 1 2 3 Ciprini, Stefano; Buson, Sara (2018-12-01). "Fermi-LAT detection of a new gamma-ray source associated with the high-redshift FSRQ PKS 2134+004 (OX 057)". The Astronomer's Telegram. 12273: 1. Bibcode:2018ATel12273....1C.
- ↑ Pacholczyk, A. G.; Swihart, T. L. (1973-01-01). "Polarization of Radio Sources.IV. The Compact Source PKS 2134+004". The Astrophysical Journal. 179: 21–28. Bibcode:1973ApJ...179...21P. doi:10.1086/151843. ISSN 0004-637X.
- ↑ Shimmins, A. J. (1968-01-01). "The Spectra of Radio Galaxies and Quasi-Stellar Objects". Astrophysical Letters. 2: 157. Bibcode:1968ApL.....2..157S. ISSN 0004-6388.
- ↑ Levshakov, S. A.; Varshalovich, D. A. (1986-12-01). "On the Spectrum of the Quasar PHL:61". Soviet Astronomy Letters. 12: 347. Bibcode:1986SvAL...12..347L.
- 1 2 Orienti, M.; Dallacasa, D.; Tinti, S.; Stanghellini, C. (2006-04-19). "VLBA images of high frequency peakers" (PDF). Astronomy & Astrophysics. 450 (3): 959–970. arXiv:astro-ph/0602158. Bibcode:2006A&A...450..959O. doi:10.1051/0004-6361:20054656. ISSN 0004-6361.
- ↑ Stanghellini, C.; Dallacasa, D.; O'Dea, C. P.; Baum, S. A.; Fanti, R.; Fanti, C. (October 2001). "VLBA observations of GHz-Peaked-Spectrum radio sources at 15 GHz" (PDF). Astronomy & Astrophysics. 377 (2): 377–388. arXiv:astro-ph/0108185. Bibcode:2001A&A...377..377S. doi:10.1051/0004-6361:20011101. ISSN 0004-6361.
- ↑ Edwards, P. G.; Tingay, S. J. (2004-09-01). "New candidate GHz peaked spectrum and compact steep spectrum sources". Astronomy and Astrophysics. 424: 91–106. arXiv:astro-ph/0407010. Bibcode:2004A&A...424...91E. doi:10.1051/0004-6361:20035749. ISSN 0004-6361.
- 1 2 Taylor, Gregory B. (2000-04-10). "Magnetic Fields in Quasar Cores. II". The Astrophysical Journal. 533 (1): 95–105. arXiv:astro-ph/9911414. Bibcode:2000ApJ...533...95T. doi:10.1086/308666. ISSN 0004-637X.
- ↑ Fomalont, E. B.; Frey, S.; Paragi, Z.; Gurvits, L. I.; Scott, W. K.; Taylor, A. R.; Edwards, P. G.; Hirabayashi, H. (November 2000). "The VSOP 5 GHz Continuum Survey: The Prelaunch VLBA Observations". The Astrophysical Journal Supplement Series. 131 (1): 95–183. Bibcode:2000ApJS..131...95F. doi:10.1086/317368. ISSN 0067-0049.
- ↑ 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.; Jiang, D.R. (1997). "A 5-GHz Southern Hemisphere VLBI Survey of Compact Radio Sources - I". The Astronomical Journal. 144 (5): 1999. arXiv:astro-ph/9709128. Bibcode:1997AJ....114.1999S. doi:10.1086/118621.
- ↑ Stanghellini, C.; O'Dea, C. P.; Dallacasa, D.; Cassaro, P.; Baum, S. A.; Fanti, R.; Fanti, C. (2005-11-15). "Extended emission around GPS radio sources" (PDF). Astronomy & Astrophysics. 443 (3): 891–902. arXiv:astro-ph/0507499. Bibcode:2005A&A...443..891S. doi:10.1051/0004-6361:20042226. ISSN 0004-6361.
- ↑ Stanghellini, Carlo (2003-01-01). "Radio Properties of GPS and CSS Sources: Galaxies versus Quasars". Publications of the Astronomical Society of Australia. 20 (1): 118–122. Bibcode:2003PASA...20..118S. doi:10.1071/AS02055. ISSN 1323-3580.
- ↑ Lister, M. L.; Kellermann, K. I.; Pauliny-Toth, I. I. K. (2002-06-01). The Diverse Properties of GPS Sources. eprint: arXiv:astro-ph/0207175: Max-Planck-Institut für Radioastronomie. Bibcode:2002evn..conf..135L.
{{cite book}}: CS1 maint: location (link) - ↑ Pauliny-Toth, I. I. K.; Alberdi, A.; Zensus, J. A.; Cohen, M. H. (1989). "Structural Variations in the Quasar 2134+004". Reviews in Modern Astronomy 2. Vol. 2. pp. 177–179. Bibcode:1989RvMA....2..177P. doi:10.1007/978-3-642-75183-7_16. ISBN 978-3-642-75185-1.
- ↑ Gottlieb, E. W.; Liller, W. (May 1978). "The historical light curve of PKS 2134 + 004 - A highly luminous QSO". Astrophysical Journal, Part 2 - Letters to the Editor. 222: L1. Bibcode:1978ApJ...222L...1G. doi:10.1086/182678. ISSN 0004-637X.
- ↑ Schramm, K. -J.; Borgeest, U.; Kuehl, D.; Linde, J. V.; Linnert, M. D. (1994-05-01). "The Hamburg Quasar Monitoring program (HQM) at Calar Alto. II. Lightcurves of weakly variable objects". Astronomy and Astrophysics Supplement Series. 104: 473–480. arXiv:astro-ph/9403049. Bibcode:1994A&AS..104..473S. ISSN 0365-0138.
- ↑ Nesci, Roberto (2018-12-01). "Optical follow-up of PKS2134-004". The Astronomer's Telegram. 12278: 1. Bibcode:2018ATel12278....1N.
- ↑ Aretxaga, Itziar; Terlevich, Roberto J.; Boyle, B. J. (1998-05-21). "Multicolour imaging of z = 2 QSO hosts". Monthly Notices of the Royal Astronomical Society. 296 (3): 643–652. arXiv:astro-ph/9711130. Bibcode:1998MNRAS.296..643A. doi:10.1046/j.1365-8711.1998.01398.x. ISSN 0035-8711.
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