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PKS 1424-418

From Wikipedia, the free encyclopedia
Blazar in the constellation Centaurus
PKS 1424-418
The blazar PKS 1424-418
Observation data (J2000.0epoch)
ConstellationCentaurus
Right ascension14h 27m 56.297s
Declination−42° 06′ 19.438″
Redshift1.522000
Heliocentric radial velocity456,824km/s
Distance9.439Gly
Apparent magnitude (V)17.7
Apparent magnitude (B)18.48
Characteristics
TypeBlazar; HPQ, FRSQ
Other designations
LEDA 2827996, PMN J1427-4206, 4FGL J1427.9-4206, WMAP 191, G4Jy 1168

PKS 1424-418 is ablazar[1] located in theconstellation ofCentaurus. It has aredshift of 1.522[2][3] and was first discovered in 1971 by astronomerKeith Peter Tritton who identified the object asultraviolet-excessive.[4] This object is also highlypolarized with a compact radio source.[5] Theradio spectrum of this source appears flat, making it a flat-spectrum radio quasar.[6]

PKS 1424-418 is found optically variable on theelectromagnetic spectrum.[7] It is a strong source ofgamma rays.[8][9] Between 2008 and 2011, PKS 1424-418 showed four phases of bright flares atGeV energies. The flares have a high correlation between the energy ranges with the exception of one flare that occurred at the same time it showed low gamma activity.[10] In April 2013, it underwent a major gamma ray outburst with its peak flux reaching values of F(> 100MeV) > 3 x 10−6 ph cm−2 s−1. According toLarge Area Telescope observations, thisemission originated beyond its broad-line region.[11] Anear-infrared flare was witnessed in PKS 1424–418 in January 2018.[12] In August 2022, it once again displayed an episode of rapid flaring activity in both gamma ray andoptical bands.[13]

PKS 1424-418 contains a radio structure, comprising a strong radio core and a weaker component with aposition angle of 260°.[5] Further observations also showed the core has a size of 0.4 mas with extended emission at both the core's position and northwest.[14] In addition, the core has a flatspectral index of -0.04.[5] Ajet is seen extending west from the core before becoming diffused.[15]

Between May 2009 and September 2019, the gamma ray emission from PKS 1424-418 was found to undergo aquasi-periodic oscillation with a 353-day flux oscillation period.[16][17] A 355-day period with highsignificance level is also confirmed by adoptingtime domain methods.[18] This might be explained byorbital motion of abinary supermassive black hole system with the mass of a primary black hole being M ~ 3.5 x 108 - 5.5 x 109 Mʘ.[19]

References

[edit]
  1. ^Abhir, J.; Joseph, J.; Patel, S. R.; Bose, D. (2021-02-01)."Multi-frequency temporal and spectral variability study of blazar PKS 1424-418".Monthly Notices of the Royal Astronomical Society.501 (2):2504–2511.arXiv:2009.08220.Bibcode:2021MNRAS.501.2504A.doi:10.1093/mnras/staa3639.ISSN 0035-8711.
  2. ^Yang, Jianping; Cao, Gang; Zhou, Bing; Qin, Longhua (2021-01-26)."Quasi-periodic Oscillation of Blazar PKS 1424–418 in γ-Ray Band".Publications of the Astronomical Society of the Pacific.133 (1020): 024101.Bibcode:2021PASP..133b4101Y.doi:10.1088/1538-3873/abd152.ISSN 0004-6280.
  3. ^White, Graeme L.; Jauncey, David L.; Wright, Alan E.; Batty, Michael J.; Savage, Ann; Peterson, Bruce A.; Gulkis, Sam (April 1988)."Redshifts of southern radio sources. VII".The Astrophysical Journal.327: 561.Bibcode:1988ApJ...327..561W.doi:10.1086/166216.ISSN 0004-637X.
  4. ^Tritton, K. P. (1971-12-01)."Spectroscopy and Photography of Southern Hemisphere Quasar Identifications".Monthly Notices of the Royal Astronomical Society.155 (1):1P –2P.doi:10.1093/mnras/155.1.1p.ISSN 0035-8711.
  5. ^abcShen, 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. (April 1998)."A 5 GHz Southern Hemisphere VLBI Survey of Compact Radio Sources. II".The Astronomical Journal.115 (4):1357–1370.arXiv:astro-ph/9803104.Bibcode:1998AJ....115.1357S.doi:10.1086/300284.
  6. ^Ciprini, Stefano; Cutini, Sara (2013-01-01)."Swift detection of increased X-ray activity from gamma-ray flaring blazar PKS 1424-41".The Astronomer's Telegram.4770: 1.Bibcode:2013ATel.4770....1C.
  7. ^Shun, Zhang; Tingfeng, Yi; Zhiyuan, Pu; Na, Wang; Zhihui, Chen; Junping, Chen; Li, Ma (2023-07-15)."Study on Optical Variability of Blazar PKS 1424-41 in Multiband".Astronomical Techniques and Instruments.20 (4):275–282.doi:10.14005/j.cnki.issn1672-7673.20230428.003.ISSN 2097-3675.
  8. ^Verrecchia, F.; Pittori, C.; Piano, G.; Tavani, M.; Panebianco, G.; Bulgarelli, A.; Fioretti, V.; Parmiggiani, N.; Addis, A.; Baroncelli, L.; Di Piano, A.; Lucarelli, F.; Vercellone, S.; Cardillo, M.; Ursi, A. (2022-12-01)."AGILE detection of increasing gamma-ray activity of blazar PKS 1424-418".The Astronomer's Telegram.15818: 1.Bibcode:2022ATel15818....1V.
  9. ^D'Ammando, F.; Orienti, M.; Longo, F.; Jankowsky, F.; Schwemmer, S.; Wagn, S. (2013-01-01)."Detection of a strong optical and gamma-ray flare from blazar PKS 1424-41".The Astronomer's Telegram.4714: 1.Bibcode:2013ATel.4714....1D.
  10. ^Buson, S.; Longo, F.; Larsson, S.; Cutini, S.; Finke, J.; Ciprini, S.; Ojha, R.; D’Ammando, F.; Donato, D.; Thompson, D. J.; Desiante, R.; Bastieri, D.; Wagner, S.; Hauser, M.; Fuhrmann, L. (2014-09-01)."Unusual flaring activity in the blazar PKS 1424−418 during 2008−2011".Astronomy & Astrophysics.569: A40.arXiv:1407.0299.Bibcode:2014A&A...569A..40B.doi:10.1051/0004-6361/201423367.ISSN 0004-6361.
  11. ^Tavecchio, F.; Pacciani, L.; Donnarumma, I.; Stamerra, A.; Isler, J.; MacPherson, E.; Urry, C. M. (2013-07-22)."The far emission region of the γ-ray blazar PKS B1424–418".Monthly Notices of the Royal Astronomical Society: Letters.435 (1):L24 –L28.arXiv:1306.0734.doi:10.1093/mnrasl/slt087.ISSN 1745-3933.
  12. ^Nesci, R.; Ojha, R.; Kadler, M. (2018-01-01)."Exceptional NIR flare in gamma-ray loud FSRQ PKS B1424-418".The Astronomer's Telegram.11235: 1.Bibcode:2018ATel11235....1N.
  13. ^Kadler, Matthias; Stevens, Jamie; Ojha, Roopesh; Edwards, Philip G.; Roesch, Florian (2022-08-01)."ATCA finds a long-term radio outburst of PKS1424-418 coincident with optical/gamma-ray flaring activity".The Astronomer's Telegram.15536: 1.Bibcode:2022ATel15536....1K.
  14. ^Dodson, R.; Fomalont, E. B.; Wiik, K.; Horiuchi, S.; Hirabayashi, H.; Edwards, P. G.; Murata, Y.; Asaki, Y.; Moellenbrock, G. A.; Scott, W. K.; Taylor, A. R.; Gurvits, L. I.; Paragi, Z.; Frey, S.; Shen, Z.-Q. (April 2008)."The VSOP 5 GHz Active Galactic Nucleus Survey. V. Imaging Results for the Remaining 140 Sources".The Astrophysical Journal Supplement Series.175 (2):314–355.arXiv:0710.5707.Bibcode:2008ApJS..175..314D.doi:10.1086/525025.ISSN 0067-0049.
  15. ^Marshall, H. L.; Schwartz, D. A.; Lovell, J. E. J.; Murphy, D. W.; Worrall, D. M.; Birkinshaw, M.; Gelbord, J. M.; Perlman, E. S.; Jauncey, D. L. (January 2005)."AChandra Survey of Quasar Jets: First Results".The Astrophysical Journal Supplement Series.156 (1):13–33.arXiv:astro-ph/0409566.Bibcode:2005ApJS..156...13M.doi:10.1086/425578.ISSN 0067-0049.
  16. ^Bhatta, Gopal; Dhital, Niraj (March 2020)."The Nature of γ-Ray Variability in Blazars".The Astrophysical Journal.891 (2): 120.arXiv:1911.08198.Bibcode:2020ApJ...891..120B.doi:10.3847/1538-4357/ab7455.ISSN 0004-637X.
  17. ^Bhatta, Gopal; Dhital, Niraj (March 2020)."The Nature of γ-Ray Variability in Blazars".The Astronomical Journal.891 (2): 120.arXiv:1911.08198.Bibcode:2020ApJ...891..120B.doi:10.3847/1538-4357/ab7455.
  18. ^Chen, Junping; Yu, Jinjie; Huang, Weitian; Ding, Nan (2024-02-08)."Transient quasi-periodic oscillations in the gamma-ray light curves of bright blazars".Monthly Notices of the Royal Astronomical Society.528 (4):6807–6822.arXiv:2401.10658.doi:10.1093/mnras/stae416.ISSN 0035-8711.
  19. ^Yang, Jianping; Cao, Gang; Zhou, Bing; Qin, Longhua (2021-01-26)."Quasi-periodic Oscillation of Blazar PKS 1424–418 in γ-Ray Band".Publications of the Astronomical Society of the Pacific.133 (1020): 024101.Bibcode:2021PASP..133b4101Y.doi:10.1088/1538-3873/abd152.ISSN 0004-6280.

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