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PKS 1144-379

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PKS 1144-379
PKS 1144-379 seen by DESI Legacy Surveys
Observation data (J2000.0 epoch)
ConstellationCentaurus
Right ascension11h 47m 01.37s
Declination-38d 12m 11.02s
Redshift1.049000
Heliocentric radial velocity314,482 km/s
Distance7.709 Gly (light travel time distance)
Apparent magnitude (V)0.266
Apparent magnitude (B)0.352
Surface brightness16.2
Characteristics
TypeOpt. var; FSRQ, BL Lac
Notable featuresQuasar with high variability
Other designations
WMAP 169, PGC 2826879, IRAS F11445-3755, NVSS J114701-381211, RFC J1147-3812, IRCF J114701.3-381211, MRC 1144-379, PG 1144-379, SUMSS J114701-381210

PKS 1144-379 also known as PKS B1144-379, is a quasar located in the constellation of Centaurus. At the redshift of 1.048,[1] the object is located nearly 8 billion light-years from Earth.[2]

Characteristics[edit]

PKS 1144-379 is classified as a flat-spectrum radio quasar (FSRQ), brighter than S4.8 GHz=65 mJy.[3][4] It has an active galactic nucleus with high optical polarization.[5][6] As monitored at 13 cm and 6 cm by researchers over three years, which they found it as a star-like object, PKS 1144-379 has been identified as BL lac object[7] of Mv ≈16.2, due to its variability in optical, infrared, and radio wavelengths.[8][1] Such BL Lac objects like PKS 1144-379 are rare active galactic nuclei class, characterized by all frequencies, and absence of emission lines.[9]

PKS 1144-379 is also radio variable as observed in the Parkes 2700 MHz survey by researchers working at Parkes Observatory.[10] The quasar is dominated by its bright compact radio core, but according to maps that is made with a high dynamic range, it shows an extended structure. PKS 1144-379 also has a luminosity above both FR I/FR II limit ~ 1032 erg s−1 Hz−1 at 5 GHz[11] and such also classfied as a blazar,[12][13] a type of active galaxy that is producing radiation, observed at wavelengths from radio to gamma rays.[14]

Observation of PKS 1144-379[edit]

PKS 1144-379 is known to be variable for its long and short-term flux density variability at centimeter wavelengths. Some of the first observations of PKS 1144−379 showed variability at frequencies of 5 GHz. The flux density is shown to increase from 0.9 Jy to 1.6 Jy between December 1970 and February, 1971.[15][16] In September of the same year, it had increased again to 2.22 Jy.[17] Between May and August 1994, the flux density of PKS 1144−379 at 4.8GHz dropped by 17%, and subsequently 9% at 8.6 GHz.[18]

In June 1996, PKS 1144-379 underwent optical variation again. Over the next 2.5 days, the survey data shows the quasar had a 33% change at 4.8 GHz. Subsequent data showed more variations in PKS 1144–379 with maximum of 8.6 GHz with over three hours of irregular change of 20%. This is strongly correlated with 10% change at 4.8 GHz.[19] From the results studying the variability behavior of PKS 1144–379, researchers found the optical variation is 1.92 mag. This is smaller than those, ~ 3.5 mag in its infrared region.[20]

Using the Ceduna 30-m radio telescope at a frequency of 6.7 GHz and very long baseline interferometry (VLBI) data at 8.6 GHz at the University of Tasmania in Australia, researchers investigated the evolution of PKS 1144–379. They found the variability time-scales associated with two flares detected in PKS 1144-379 between November 2005 and August 2008 were found to derive from long-term variations in total flux density as monitored by Ceduna between 2003 and 2011. Moreover, a kinematic study of the parsec-scale jet of PKS 1144-379 was also performed through VLBI data obtained between 1997 and 2018, which they observe quasi-periodic flarings of ~3-4 yr. Over the 20-yr interval, they found the average jet position angle was ~150°.[21] The core component of PKS 1144-379 is found to be compacted, which its angular size varied between the ranges of 5.65-15.90 Чas estimating to be 0.05-0.13 pc.[22]

Researchers assumed the variations observed in PKS 1144–379, are due to scintillation. The variations are 6.2 ×1012 K at 4.9 GHz with approximately 10% of total flux density found in the scintillating component. Given the results, PKS 1144-379 has a high modulation index in the range of 5–18%[22] combined with the 1.2 day characteristic timescale (corresponding to a peak-to-peak period of 7.7 days), making it the most extreme bright scintillators identified in history.[23] According to observations by Fermi, PKS 1144-379 has a column dissipation radius of 64.5 x 1015 cm (430) RS with an accretion disc luminosity of 1045 erg s−1 3 x (0.04) LEdd. The jet power as the form of radiation for the quasar has a log probability of 44.92 log Pr with Poynting flux of 44.49 log PB while the bulk motion of electrons and protons is found to be have 44.34 log Pe and 46.41 log Pp. From the results, PKS 1144-379 has an estimated black hole mass of 108–109 M⊙, whom researchers noted.[24]

References[edit]

  1. ^ a b Stickel, M.; Fried, J. W.; Kuehr, H. (1989-10-01). "Optical spectroscopy of 1 Jy BL Lacertae objects and flat spectrum radio sources". Astronomy and Astrophysics Supplement Series. 80: 103–114. Bibcode:1989A&AS...80..103S. ISSN 0365-0138.
  2. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-06-08.
  3. ^ Healey, Stephen E.; Romani, Roger W.; Taylor, Gregory B.; Sadler, Elaine M.; Ricci, Roberto; Murphy, Tara; Ulvestad, James S.; Winn, Joshua N. (2007-07-01). "CRATES: An All-Sky Survey of Flat-Spectrum Radio Sources". The Astrophysical Journal Supplement Series. 171 (1): 61–71. arXiv:astro-ph/0702346. Bibcode:2007ApJS..171...61H. doi:10.1086/513742. ISSN 0067-0049.
  4. ^ Korsmeier, Michael; Pinetti, Elena; Negro, Michela; Regis, Marco; Fornengo, Nicolao (2022-07-01). "Flat spectrum radio quasars and BL Lacs dominate the anisotropy of the unresolved gamma-ray background". The Astrophysical Journal. 933 (2): 221. arXiv:2201.02634. Bibcode:2022ApJ...933..221K. doi:10.3847/1538-4357/ac6c85. ISSN 0004-637X.
  5. ^ Véron-Cetty, M. -P.; Véron, P. (2006-08-01). "A catalogue of quasars and active nuclei: 12th edition". Astronomy and Astrophysics. 455 (2): 773–777. Bibcode:2006A&A...455..773V. doi:10.1051/0004-6361:20065177. ISSN 0004-6361.
  6. ^ Scarpa, R.; Falomo, R. (1997-09-01). "Are high polarization quasars and BL Lacertae objects really different? A study of the optical spectral properties". Astronomy and Astrophysics. 325: 109–123. Bibcode:1997A&A...325..109S. ISSN 0004-6361.
  7. ^ "A Sample-Oriented Catalogue of BL Lacertae Objects". ned.ipac.caltech.edu. Retrieved 2024-06-08.
  8. ^ Nicolson, G. D.; Glass, I. S.; Feast, M. W.; Andrews, P. J. (1979-10-01). "The BL Lac object PKS 1144-379". Monthly Notices of the Royal Astronomical Society. 189: 29P–31P. Bibcode:1979MNRAS.189P..29N. doi:10.1093/mnras/189.1.29P. ISSN 0035-8711.
  9. ^ Giommi, P.; Ansari, S. G.; Micol, A. (1995). "1995A&AS..109..267G Page 267". Astronomy and Astrophysics Supplement Series. 109: 267. Bibcode:1995A&AS..109..267G. Retrieved 2024-06-08.
  10. ^ Peterson, B. A.; Bolton, J. G. (1973). "1973ApL....13..187P Page 187". Astrophysical Letters. 13: 187. Bibcode:1973ApL....13..187P. Retrieved 2024-06-08.
  11. ^ "The Emission Line Spectrum of Active Galactic Nuclei and the Unifying Scheme - Veron-Cetty & Veron". ned.ipac.caltech.edu. Retrieved 2024-06-08.
  12. ^ Urry, C. Megan; Padovani, Paolo (1995-09-01). "Unified Schemes for Radio-Loud Active Galactic Nuclei". Publications of the Astronomical Society of the Pacific. 107: 803. arXiv:astro-ph/9506063. Bibcode:1995PASP..107..803U. doi:10.1086/133630. ISSN 0004-6280.
  13. ^ Safna, P. Z.; Stalin, C. S.; Rakshit, Suvendu; Mathew, Blesson (2020-09-22). "Long term optical and infrared variability characteristics of Fermi Blazars". Monthly Notices of the Royal Astronomical Society. 498 (3): 3578–3591. arXiv:2008.12072. doi:10.1093/mnras/staa2622. ISSN 0035-8711.
  14. ^ Itoh, Ryosuke; Nalewajko, Krzysztof; Fukazawa, Yasushi; Uemura, Makoto; Tanaka, Yasuyuki T.; Kawabata, Koji S.; Madejski, Greg M.; Schinzel, Frank K.; Kanda, Yuka; Shiki, Kensei; Akitaya, Hiroshi; Kawabata, Miho; Moritani, Yuki; Nakaoka, Tatsuya; Ohsugi, Takashi (December 2016). "Systematic Study of Gamma-Ray-Bright Blazars With Optical Polarization and Gamma-Ray Variability". The Astrophysical Journal. 833 (1): 77. arXiv:1610.04313. Bibcode:2016ApJ...833...77I. doi:10.3847/1538-4357/833/1/77. ISSN 0004-637X.
  15. ^ Shimmins, A. J.; Bolton, J. G. (1972-01-01). "Accurate Flux Densities at 5009 MHz of 1007 Radio Sources". Australian Journal of Physics Astrophysical Supplement. 23: 1. Bibcode:1972AuJPA..23....1S.
  16. ^ Bolton, J. G.; Shimmins, A. J. (1973-01-01). "The Parkes 2700 MHz Survey (Fifth Part): Catalogue for the Declination zone -35o to -45o". Australian Journal of Physics Astrophysical Supplement. 30: 1. Bibcode:1973AuJPA..30....1B.
  17. ^ Gardner, F. F.; Whiteoak, J. B.; Morris, D. (1975-01-01). "The Linear Polarization of Radio Sources I: Observations at Wavelengths of 6, 11, 18 and 21 cm". Australian Journal of Physics Astrophysical Supplement. 35: 1. Bibcode:1975AuJPA..35....1G.
  18. ^ Kedziora-Chudczer, L. L.; Jauncey, D. L.; Wieringa, M. H.; Tzioumis, A. K.; Reynolds, J. E. (2001-08-01). "The ATCA intraday variability survey of extragalactic radio sources". Monthly Notices of the Royal Astronomical Society. 325 (4): 1411–1430. arXiv:astro-ph/0103506. Bibcode:2001MNRAS.325.1411K. doi:10.1046/j.1365-8711.2001.04516.x. ISSN 0035-8711.
  19. ^ Kedziora-Chudczer, L. L.; Jauncey, D. L.; Wieringa, M. H.; Reynolds, J. E.; Tzioumis, A. K. (1998). "1998ASPC..144..271K Page 271". IAU Colloq. 164: Radio Emission from Galactic and Extragalactic Compact Sources. 144: 271. Bibcode:1998ASPC..144..271K. Retrieved 2024-06-08.
  20. ^ Fan, J. H.; Lin, R. G. (July 2000). "Optical Variability and Periodicity Analysis for Blazars. I. Light Curves for Radio-selected BL Lacertae Objects". The Astrophysical Journal. 537 (1): 101–122. Bibcode:2000ApJ...537..101F. doi:10.1086/308996. ISSN 0004-637X.
  21. ^ Said, N. M. M.; Ellingsen, S. P.; Shabala, S.; Orosz, G.; Liu, J.; Bignall, H. E.; McCallum, J. N.; Reynolds, C. (2021-12-01). "Investigating the evolution of PKS B1144-379: comparison of VLBI and scintillation techniques". Monthly Notices of the Royal Astronomical Society. 508 (2): 2881–2896. Bibcode:2021MNRAS.508.2881S. doi:10.1093/mnras/stab2724. ISSN 0035-8711.
  22. ^ a b Said, N M M; Ellingsen, S P; Bignall, H E; Shabala, S; McCallum, J N; Reynolds, C (2020-09-02). "Interstellar scintillation of an extreme scintillator: PKS B1144−379". Monthly Notices of the Royal Astronomical Society. 498 (4): 4615–4634. doi:10.1093/mnras/staa2642. ISSN 0035-8711.
  23. ^ Turner, R. J.; Ellingsen, S. P.; Shabala, S. S.; Blanchard, J.; Lovell, J. E. J.; McCallum, J. N.; Cimò, G. (2012-07-10). "BL LAC OBJECT PKS B1144–379: An Extreme Scintillator". The Astrophysical Journal. 754 (2): L19. arXiv:1206.6914. Bibcode:2012ApJ...754L..19T. doi:10.1088/2041-8205/754/2/l19. ISSN 2041-8205.
  24. ^ Ghisellini, G.; Tavecchio, F.; Foschini, L.; Ghirlanda, G.; Maraschi, L.; Celotti, A. (2009-11-26). "General physical properties of bright Fermi blazars". Monthly Notices of the Royal Astronomical Society. 402 (1): 497–518. arXiv:0909.0932. doi:10.1111/j.1365-2966.2009.15898.x. ISSN 0035-8711.
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