Astronomy:PKS 2134+004

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PKS 2134+004
The quasar PKS 2134+004.
Observation data (J2000.0 epoch)
ConstellationAquarius
Right ascension 21h 36m 38.5863s
Declination+00° 41′ 54.213″
Redshift1.941251
Helio radial velocity581,972 km/s
Distance9.945 Gly
Apparent magnitude (V)17.08
Apparent magnitude (B)17.30
Characteristics
TypeOpt. 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]

Description

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

  1. ↑ Wolter, A.; Celotti, A. (2001-05-01). "An X-ray selected sample of radio-loud quasars". Astronomy and Astrophysics 371 (2): 527–537. doi:10.1051/0004-6361:20010415. ISSN 0004-6361. Bibcode: 2001A&A...371..527W. 
  2. ↑ 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. doi:10.1071/AS03014. ISSN 1323-3580. Bibcode: 2003PASA...20..144M. https://ui.adsabs.harvard.edu/abs/2003PASA...20..144M/abstract. 
  3. ↑ 3.0 3.1 3.2 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. https://ui.adsabs.harvard.edu/abs/2018ATel12273....1C/abstract. 
  4. ↑ 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. doi:10.1086/151843. ISSN 0004-637X. Bibcode: 1973ApJ...179...21P. https://ui.adsabs.harvard.edu/abs/1973ApJ...179...21P/abstract. 
  5. ↑ Shimmins, A. J. (1968-01-01). "The Spectra of Radio Galaxies and Quasi-Stellar Objects". Astrophysical Letters 2: 157. ISSN 0004-6388. Bibcode: 1968ApL.....2..157S. https://articles.adsabs.harvard.edu/pdf/1968ApL.....2..157S. 
  6. ↑ 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. https://articles.adsabs.harvard.edu/pdf/1986SvAL...12..347L. 
  7. ↑ 7.0 7.1 Orienti, M.; Dallacasa, D.; Tinti, S.; Stanghellini, C. (2006-04-19). "VLBA images of high frequency peakers". Astronomy & Astrophysics 450 (3): 959–970. doi:10.1051/0004-6361:20054656. ISSN 0004-6361. Bibcode: 2006A&A...450..959O. https://www.aanda.org/articles/aa/pdf/2006/18/aa4656-05.pdf. 
  8. ↑ 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". Astronomy & Astrophysics 377 (2): 377–388. doi:10.1051/0004-6361:20011101. ISSN 0004-6361. Bibcode: 2001A&A...377..377S. https://www.aanda.org/articles/aa/pdf/2001/38/aa1554.pdf. 
  9. ↑ 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. doi:10.1051/0004-6361:20035749. ISSN 0004-6361. Bibcode: 2004A&A...424...91E. 
  10. ↑ 10.0 10.1 Taylor, Gregory B. (2000-04-10). "Magnetic Fields in Quasar Cores. II.". The Astrophysical Journal 533 (1): 95–105. doi:10.1086/308666. ISSN 0004-637X. Bibcode: 2000ApJ...533...95T. https://iopscience.iop.org/article/10.1086/308666/fulltext/. 
  11. ↑ 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. doi:10.1086/317368. ISSN 0067-0049. Bibcode: 2000ApJS..131...95F. https://iopscience.iop.org/article/10.1086/317368/fulltext/. 
  12. ↑ Shen, Z.Q.; Wan, T.S.; Moran, J.M.; Jauncey, D.L.; Reynolds, J.E.; Tzioumis, A.K.; Gough, R.G.; Ferris, R.H. et al. (1997). "A 5-GHz Southern Hemisphere VLBI Survey of Compact Radio Sources - I". The Astronomical Journal 144 (5): 1999. doi:10.1086/118621. Bibcode: 1997AJ....114.1999S. https://articles.adsabs.harvard.edu/pdf/1997AJ....114.1999S. 
  13. ↑ 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". Astronomy & Astrophysics 443 (3): 891–902. doi:10.1051/0004-6361:20042226. ISSN 0004-6361. Bibcode: 2005A&A...443..891S. https://www.aanda.org/articles/aa/pdf/2005/45/aa2226-04.pdf. 
  14. ↑ 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. doi:10.1071/AS02055. ISSN 1323-3580. Bibcode: 2003PASA...20..118S. https://articles.adsabs.harvard.edu/pdf/2003PASA...20..118S. 
  15. ↑ 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. https://articles.adsabs.harvard.edu/pdf/2002evn..conf..135L. 
  16. ↑ 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. 2. pp. 177–179. doi:10.1007/978-3-642-75183-7_16. ISBN 978-3-642-75185-1. Bibcode: 1989RvMA....2..177P. https://articles.adsabs.harvard.edu//full/1989RvMA....2..177P/0000177.000.html. 
  17. ↑ 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. doi:10.1086/182678. ISSN 0004-637X. Bibcode: 1978ApJ...222L...1G. https://doi.org/10.1086/182678. 
  18. ↑ 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. ISSN 0365-0138. Bibcode: 1994A&AS..104..473S. https://articles.adsabs.harvard.edu/pdf/1994A%26AS..104..473S. 
  19. ↑ Nesci, Roberto (2018-12-01). "Optical follow-up of PKS2134-004". The Astronomer's Telegram 12278: 1. Bibcode: 2018ATel12278....1N. https://ui.adsabs.harvard.edu/abs/2018ATel12278....1N/abstract. 
  20. ↑ 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. doi:10.1046/j.1365-8711.1998.01398.x. ISSN 0035-8711. Bibcode: 1998MNRAS.296..643A. 



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