Langbahn Team – Weltmeisterschaft

PKS 0451-28

PKS 0451-28
PKS 0451-28 captured by Dark Energy Survey
Observation data (J2000.0 epoch)
ConstellationCaelum
Right ascension04h 53m 14.65s
Declination-28d 07m 37.33s
Redshift2.559000
Heliocentric radial velocity767,169 km/s
Distance10.762 Gly (light travel time distance)
Apparent magnitude (V)0.085
Apparent magnitude (B)0.113
Surface brightness18.5
Characteristics
TypeFSRQ, blazar
Other designations
RFC J0453-2807, WMAP 131, PGC 2824135, NVSS J045314-280736, MRC 0451-282, PMN J0453-2807, PKS J0453-2807, OF -285, IRCF J045314.6-280737, OCARS 0451-282, 2FGL J0453.1-2807, 5BZQ J0453-2807, 1RXS J045313.9-280737

PKS 0451-28 (full name PKS 0451-282), also known as MRC 0451-282, is a quasar located in the constellation of Caelum. Its redshift is 2.55, estimating the object to be located nearly 10.8 billion light-years away from Earth.[1]

Characteristics

Observed by the 20-GHz Australia Telescope Compact Array radio survey,[2] PKS 0451-28 is classified as a blazar.[3][4] It is a type of an active extragalactic object launching out a relativistic astrophysical jet towards the direction of Earth with the observer's line of sight.[5]

The emitted radiation from PKS 0451-28 shows a strong variability across its entire electro-magnetic spectrum.[6] As a source of non-thermal emission, from radio to high energy (HE; >100 MeV) or very high energy (VHE; >100 GeV) γ-ray bands, the jets of PKS 0451-28 are known to cover the entire spectrum.[7] This tend to vary in a short time-scales such as in minute scales within the γ-ray band causing an increase in luminosity.[8][9] The flux variation in PKS 0451–28, the observed superluminal motion, high degrees of polarization, and other features observed are explained by the relativistic beaming effects.[10]

Moreover, PKS 0451-28 is a flat-spectrum radio quasar (FSRQ). It has a strong emission lines (EW >5 Å)[5] and contains a powerful radio source[11][12] observed by NuSTAR,[13] with a visual magnitude of 16.7 and redshift of 0.9, which its radio fluxes have been catalogued at 1.8 Jy at 5 GHz and 3 Jy at 31 GHz respectively.[14]

Observations of PKS 0451-28

According to researchers, the γ-ray luminosity in PKS 0451-28 is found to exceed 1048 erg s−1 with the highest γ-ray luminosity of (5.54 ± 0.06) × 1048 erg s−1, that is estimated for another blazar, B3 1343+451. Naturally, compared to the distribution of all BL Lacs and FSRQs that are considered γ-ray-emitting, in the Γγ−Lγ plane, the blazars observed, are considered to occupy the highest luminosity range.[15]

Interestingly, PKS 0451-28 appears as a bright X-ray emitter, but however does not have signs of distinguishable features in the X-ray band, only having a flux and photon index similar to those of the other considered sources in blazars.[10] Along with other studied blazars like PKS 0537-286, PKS 1351-108, PKS 0438-43, PKS 0834-20 and TXS 0222+185, a thermal blue-bump component is found in PKS 0451–28, suggesting emission directly from its disc.[16]

Researchers also noted the X-ray flux in PKS 0451-28 is known to be consistent, remaining at (9.52 ± 1.21) × 10−14 erg cm−2 s−1 compared to a few blazars like PKS 0438−43, whose X-ray flux was in a bright X-ray state on December 15, 2016, with a flux of (1.09 ± 0.16) × 10−11 erg cm−2 s−1 as compared with the flux of (1.30 ± 0.31) × 10−11 erg cm−2 s−1 in the quiescent state.[10]

Moreover, the adaptively binned light curves for PKS 0451-28 shows show several episodes of γ-rays brightening, whereas the γ-ray flux increase within day scales is observed. The peak γ-ray flux of (2.20 ± 0.50) × 10−7 photon cm−2 s−1 in PKS 0451-28 is found to be above 163.2 MeV. During the observation, it has a MJD of 56968.60 ± 0.79 with 9.64σ, corresponding to a flux of (3.70 ± 0.84) × 10−7 photon cm−2 s−1 above 100 MeV. During this period, Γγ was 2.06 ± 0.19. This shows only the photon index of PKS 0451-28 varies in time; the variation is highly significant in which the blazar shows a value of P(χ2) ≤ 10−5.[10]

Disc luminosity

The disc luminosity of PKS 0451-28 is estimated to be Ld ≃ (1.09−10.94) × 1046 erg s−1 according to researchers calculating the energetics of the considered source for the blazar by using modelling results.[10]

Supermassive black hole and jet luminosity

The supermassive black hole in PKS 0451-28 has a solar mass of within (1.69−5.35) × 109 M⊙ as calculated by researchers through a traditional virial method.[17][18] Around 5–16 percent is contributed by the Eddington luminosity.[10]

As for jet power in PKS 0451–28, it is in the form of the magnetic field (LB) and relativistic electrons (Le). Researchers calculated the jet power as L = πR2c Γ2Ui, where Ui is either electron (Ue) or magnetic field (UB) energy density.[10] Furthermore, the jet luminosity (defined as L = Le + LB) is ≤1.41 × 1046 erg s−1 for PKS 0451–28. It is found to be lower compared to the disc Ld ≃ (1.09−10.94) × 1046 erg s−1 although it has a significant correlation with the broad-line luminosity in the blazar, hence supporting the theory of jet power having a closer bond with accretion.[19]

The jet power is found to have an approximate value of logLBLR ~ (0.98 ± 0.07)logPjet for all blazars including PKS 0451–28. The values are consistent with the theoretical predicted coefficient of logLBLR-logLjet relation.[10] Results do support the jets in blazars like PKS 0451–28, are powered by energy extraction from both accretion and black hole spin as observed by Fermi.[19] This finds PKS 0451-28 is a powerful blazar with high luminosity and of the same order calculated for other blazars studied[20][21] both distant and nearby[22] since the jet power do not differ substantially and those that are usually estimated for bright FSRQs.[23]

References

  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-06-06.
  2. ^ Ghirlanda, G.; Ghisellini, G.; Tavecchio, F.; Foschini, L. "Correlation of Fermi Large Area Telescope sources with the 20-GHz Australia Telescope Compact Array radio survey". academic.oup.com. Retrieved 2024-06-06.
  3. ^ Donato, D.; Ghisellini, G.; Tagliaferri, G.; Fossati, G. (2001-09-01). "Hard X-ray properties of blazars". Astronomy & Astrophysics. 375 (3): 739–751. arXiv:astro-ph/0105203. Bibcode:2001A&A...375..739D. doi:10.1051/0004-6361:20010675. ISSN 0004-6361.
  4. ^ Xiong, Dingrong; Zhang, Xiong; Bai, Jinming; Zhang, Haojing. "Basic properties of Fermi blazars and the 'blazar sequence'". academic.oup.com. Retrieved 2024-06-06.
  5. ^ a b 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.
  6. ^ Fromm, C. M.; Fuhrmann, L.; Perucho, M. (2015-08-01). "Multi-frequency properties of synthetic blazar radio light curves within the shock-in-jet scenario". Astronomy & Astrophysics. 580: A94. arXiv:1412.7194. Bibcode:2015A&A...580A..94F. doi:10.1051/0004-6361/201424815. ISSN 0004-6361.
  7. ^ Padovani, P.; Alexander, D. M.; Assef, R. J.; De Marco, B.; Giommi, P.; Hickox, R. C.; Richards, G. T.; Smolčić, V.; Hatziminaoglou, E.; Mainieri, V.; Salvato, M. (2017-08-01). "Active galactic nuclei: what's in a name?". Astronomy and Astrophysics Review. 25 (1): 2. arXiv:1707.07134. Bibcode:2017A&ARv..25....2P. doi:10.1007/s00159-017-0102-9. ISSN 0935-4956.
  8. ^ Brown, Anthony M. (2013-05-01). "Locating the γ-ray emission region of the flat spectrum radio quasar PKS 1510-089". Monthly Notices of the Royal Astronomical Society. 431 (1): 824–835. arXiv:1301.7677. Bibcode:2013MNRAS.431..824B. doi:10.1093/mnras/stt218. ISSN 0035-8711.
  9. ^ Nalewajko, Krzysztof (2013-04-01). "The brightest gamma-ray flares of blazars". Monthly Notices of the Royal Astronomical Society. 430 (2): 1324–1333. arXiv:1211.0274. Bibcode:2013MNRAS.430.1324N. doi:10.1093/mnras/sts711. ISSN 0035-8711.
  10. ^ a b c d e f g h Sahakyan, N; Israyelyan, D; Harutyunyan, G; Khachatryan, M; Gasparyan, S. "Multiwavelength study of high-redshift blazars". academic.oup.com. Retrieved 2024-06-06.
  11. ^ Fricke, K. J.; Kollatschny, W.; Witzel, A. (1983). "1983A&A...117...60F Page 61". Astronomy and Astrophysics. 117: 60. Bibcode:1983A&A...117...60F. Retrieved 2024-06-06.
  12. ^ Wall, J. V. (1973). "1973ApL....15..101W Page 101". Astrophysical Letters. 15: 101. Bibcode:1973ApL....15..101W. Retrieved 2024-06-06.
  13. ^ Ghisellini, G.; Perri, M.; Costamante, L.; Tagliaferri, G.; Sbarrato, T.; Campitiello, S.; Madejski, G.; Tavecchio, F.; Ghirlanda, G. (2019-07-01). "A NuSTAR view of powerful γ-ray loud blazars". Astronomy & Astrophysics. 627: A72. arXiv:1906.02955. Bibcode:2019A&A...627A..72G. doi:10.1051/0004-6361/201935750. ISSN 0004-6361.
  14. ^ Bertsch, D. (1998-01-01). "PKS 2255-282". International Astronomical Union Circular (6807): 2. Bibcode:1998IAUC.6807....2B. ISSN 0081-0304.
  15. ^ Ajello, M.; Angioni, R.; Axelsson, M.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Becerra Gonzalez, J.; Bellazzini, R.; Bissaldi, E.; Bloom, E. D.; Bonino, R.; Bottacini, E.; Bruel, P.; Buson, S.; Cafardo, F. (2020-04-01). "The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope". The Astrophysical Journal. 892 (2): 105. arXiv:1905.10771. Bibcode:2020ApJ...892..105A. doi:10.3847/1538-4357/ab791e. ISSN 0004-637X.
  16. ^ Ghisellini, G.; Tavecchio, F.; Ghirlanda, G. "Jet and accretion power in the most powerful Fermi blazars". academic.oup.com. Retrieved 2024-06-06.
  17. ^ Woo, Jong-Hak; Urry, C. Megan (2002-11-10). "Active Galactic Nucleus Black Hole Masses and Bolometric Luminosities". The Astrophysical Journal. 579 (2): 530. arXiv:astro-ph/0207249. Bibcode:2002ApJ...579..530W. doi:10.1086/342878. ISSN 0004-637X.
  18. ^ Wang, Jian-Min; Luo, Bin; Ho, Luis C. (2004-11-01). "The Connection between Jets, Accretion Disks, and Black Hole Mass in Blazars". The Astrophysical Journal. 615 (1): L9 – L12. arXiv:astro-ph/0412074. Bibcode:2004ApJ...615L...9W. doi:10.1086/426060. ISSN 0004-637X.
  19. ^ a b Xiong, D. R.; Zhang, X. "Intrinsic γ-ray luminosity, black hole mass, jet and accretion in Fermi blazars". academic.oup.com. Retrieved 2024-06-06.
  20. ^ Ghisellini, G.; Tagliaferri, G.; Foschini, L.; Ghirlanda, G.; Tavecchio, F. "High-redshift Fermi blazars". academic.oup.com. Retrieved 2024-06-06.
  21. ^ Paliya, Vaidehi S.; Parker, M. L.; Fabian, A. C.; Stalin, C. S. (2016-07-01). "Broadband Observations of High Redshift Blazars". The Astrophysical Journal. 825 (1): 74. arXiv:1604.08566. Bibcode:2016ApJ...825...74P. doi:10.3847/0004-637X/825/1/74. ISSN 0004-637X.
  22. ^ Ghisellini, G.; Tavecchio, F.; Maraschi, L.; Celotti, A.; Sbarrato, T. (2014-11-01). "The power of relativistic jets is larger than the luminosity of their accretion disks". Nature. 515 (7527): 376–378. arXiv:1411.5368. Bibcode:2014Natur.515..376G. doi:10.1038/nature13856. ISSN 0028-0836. PMID 25409827.
  23. ^ Pacciani, L.; Tavecchio, F.; Donnarumma, I.; Stamerra, A.; Carrasco, L.; Recillas, E.; Porras, A.; Uemura, M. (2014-08-01). "Exploring the Blazar Zone in High-energy Flares of FSRQs". The Astrophysical Journal. 790 (1): 45. arXiv:1312.3998. Bibcode:2014ApJ...790...45P. doi:10.1088/0004-637X/790/1/45. ISSN 0004-637X.
Quelle: http://en.wikipedia.org/wiki/PKS_0451-28