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PKS 0458−020

From Wikipedia, the free encyclopedia
Quasar in the constellation Orion
PKS 0458−020
The quasar/blazar PKS 0458−020
Observation data (J2000.0epoch)
ConstellationOrion
Right ascension05h 01m 12.809s
Declination−01° 59′ 14.256″
Redshift2.286000
Heliocentric radial velocity685,326km/s
Distance10.447Gly
Apparent magnitude (V)18.06
Apparent magnitude (B)19.1
Characteristics
TypeBlazar, HPQ, FRSQ
Other designations
4C −02.19, PKS 0458−02, TXS 0458−020,LEDA 2818086, DA 157, OF -098, 4FGL J0501.2−0158, S3 0458−02

PKS 0458−020 also known asPKS 0458−02, is aquasar located in theconstellation ofOrion. It has aredshift of (z) 2.286[1][2] and was first identified as anastronomical radio source during the radio survey conducted byParkes Observatory in 1966.[3] Subsequently the source was shown to displayoptical behavior[4] before being classified as ablazar via an opticalpolarimetry study in 1985.[5] This source also showsradio spectrum appearing to be flat, hence making it aflat-spectrum radio quasar (FRSQ).[6]

Description

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PKS 0458−020 is found variable across theelectromagnetic spectrum and a source ofgamma ray activity.[7][8][9] It is known to show optical flares which was detected byFermi Gamma-ray Space Telescope (Fermi LAT)[10] and by theNordic Optical Telescope in September 2012, where it was reported to be 30 times brighter than its dailyflux of (E > 100MeV) when recorded by Fermi LAT.[11] Anear infrared flare was detected in January 2015.[12]

The radio structure of PKS 0458−020 is extended across a wide scale range. Radio images of the object produced viaVery Large Array (VLA), showed two unique components separated by 1.8arcseconds with aposition angle of -127°. Ajet can seen heading northwest before veering southwest.[1] This jet also appears to have a sharp bend by around 60° based on 15 and 43GHz imaging.[13][14] There is a strong compact radio core straddled by extendedemission which yields a projected angular size of 3.5 arcseconds.[15] A secondary structure is located southwest from the core with a bridge-like structure almost connecting it. There is also some lobe luminosity located on the side of the counterjet with the jet's side having halo emission.[16]

Thesupermassive black hole in PKS 0458−020 is estimated to be 8 x 108 Mʘ based on an Ld value corresponding to the peaking of a disk spectrum with the diskluminosity being Ld ~ 2 x 1046erg s−1.[17]

Twoabsorption line systems located at redshifts (z) 2.039 and (z) 2.04 were detected towards the object with the former having the largest known redshift at radiowavelengths.[18][19]

References

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  1. ^abShen, 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.; Hong, X. -Y.; Liang, S. -G.; Costa, M. E.; Tingay, S. J.; McCulloch, P. M. (1997-11-01)."A 5-GHz Southern Hemisphere VLBI Survey of Compact Radio Sources.I."The Astronomical Journal.114: 1999.arXiv:astro-ph/9709128.Bibcode:1997AJ....114.1999S.doi:10.1086/118621.ISSN 0004-6256.
  2. ^Sapre, A. K.; Mishra, V. D. (1985)."Redshifts of the brightest X-ray QSO's".Astrophysics and Space Science.115 (1):107–118.Bibcode:1985Ap&SS.115..107S.doi:10.1007/bf00653831.ISSN 0004-640X.
  3. ^Shimmins, A.J.; Day, G.A.; 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..837S.doi:10.1071/ph660837.ISSN 0004-9506.
  4. ^Scott, R. L.; Leacock, R. J.; McGimsey, B. Q.; Smith, A. G.; Edwards, P. L.; Hackney, K. R.; Hackney, R. L. (1976-01-01)."Optical behavior of 64 extragalactic radio sources".The Astronomical Journal.81:7–19.Bibcode:1976AJ.....81....7S.doi:10.1086/111846.ISSN 0004-6256.
  5. ^Impey, C. D.; Tapia, S. (October 1988)."New blazars discovered by polarimetry".The Astrophysical Journal.333: 666.Bibcode:1988ApJ...333..666I.doi:10.1086/166775.ISSN 0004-637X.
  6. ^Ciprini, Stefano; Fermi Large Area Telescope Collaboration (2015-08-01)."Fermi LAT detection of renewed GeV activity from the high redshift blazar PKS 0458-02".The Astronomer's Telegram.7952: 1.Bibcode:2015ATel.7952....1C.
  7. ^Antolini, Elisa; Buson, Sara (2014-03-01)."Fermi LAT detection of GeV flares from blazars PKS 0458-02 and B2 1144+40".The Astronomer's Telegram.5951: 1.Bibcode:2014ATel.5951....1A.
  8. ^Dinesh, Adithiya (2023-07-01)."Fermi-LAT detection of renewed gamma-ray activity from the FSRQ S3 0458-02".The Astronomer's Telegram.16110: 1.Bibcode:2023ATel16110....1D.
  9. ^Orienti, M.; D'Ammando, F. (2012-09-01)."Fermi LAT detection of a GeV flare from the high redshift blazar PKS 0458-02".The Astronomer's Telegram.4396: 1.Bibcode:2012ATel.4396....1O.
  10. ^D'Ammando, F.; Orienti, M.; Mountford, C. J. (2012-09-01)."Swift follow-up of the flaring high-redshift blazar PKS 0458-02".The Astronomer's Telegram.4407: 1.Bibcode:2012ATel.4407....1D.
  11. ^Pursimo, Tapio; Ojha, Roopesh; Kiaeerad, Fatemeh (2012-09-01)."Optical activity of the flaring gamma-ray blazar PKS 0458-02".The Astronomer's Telegram.4402: 1.Bibcode:2012ATel.4402....1P.
  12. ^Carrasco, L.; Miramon, J.; Porras, A.; Recillas, E.; Chavushyan, V.; Carraminana, A. (2015-01-01)."A New NIR Flare of the QSO PKS0458-02".The Astronomer's Telegram.6995: 1.Bibcode:2015ATel.6995....1C.
  13. ^Kellermann, K. I.; Vermeulen, R. C.; Zensus, J. A.; Cohen, M. H. (April 1998)."Sub-Milliarcsecond Imaging of Quasars and Active Galactic Nuclei".The Astronomical Journal.115 (4):1295–1318.arXiv:astro-ph/9801010.Bibcode:1998AJ....115.1295K.doi:10.1086/300308.ISSN 0004-6256.
  14. ^Jorstad, Svetlana G.; Marscher, Alan P.; Mattox, John R.; Wehrle, Ann E.; Bloom, Steven D.; Yurchenko, Alexei V. (June 2001)."Multiepoch Very Long Baseline Array Observations of EGRET-detected Quasars and BL Lacertae Objects: Superluminal Motion of Gamma-Ray Bright Blazars".The Astrophysical Journal Supplement Series.134 (2):181–240.arXiv:astro-ph/0101570.Bibcode:2001ApJS..134..181J.doi:10.1086/320858.ISSN 0067-0049.
  15. ^Barthel, Peter D.; Vestergaard, Marianne; Lonsdale, Colin J. (2000-02-01)."Radio imaging of core-dominated high redshift quasars".Astronomy and Astrophysics.354:7–16.arXiv:astro-ph/9911474.Bibcode:2000A&A...354....7B.ISSN 0004-6361.
  16. ^Punsly, Brian (April 1995)."The extended morphology of ultraluminous radio cores".The Astronomical Journal.109: 1555.Bibcode:1995AJ....109.1555P.doi:10.1086/117385.ISSN 0004-6256.
  17. ^Ghisellini, G.; Perri, M.; Costamante, L.; Tagliaferri, G.; Sbarrato, T.; Campitiello, S.; Madejski, G.; Tavecchio, F.; Ghirlanda, G. (July 2019). "ANuSTAR view of powerfulγ-ray loud blazars".Astronomy & Astrophysics.627: A72.arXiv:1906.02955.doi:10.1051/0004-6361/201935750.ISSN 0004-6361.
  18. ^Wolfe, A. M.; Briggs, F. H.; Turnshek, D. A.; Davis, M. M.; Smith, H. E.; Cohen, R. D. (July 1985)."Detection of 21 centimeter absorption at Z = 2.04 in the QSO PKS 0458-02".The Astrophysical Journal.294: L67.Bibcode:1985ApJ...294L..67W.doi:10.1086/184511.ISSN 0004-637X.
  19. ^Tsuboi, Masato; Nakai, Naomasa (1991-12-01)."A Search for the CO J=1-0 Absorption Line at z=2.04 toward the QSO PKS 0458-02".Publications of the Astronomical Society of Japan.43 (6):L65–L68.Bibcode:1991PASJ...43L..65T.doi:10.1093/pasj/43.6.L65.ISSN 0004-6264.

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