PKS 0451-28

Last updated
PKS 0451-28
DES-DR1 image of PKS 0451-28.jpg
PKS 0451-28 captured by Dark Energy Survey
Observation data (J2000.0 epoch)
Constellation Caelum
Right ascension 04h 53m 14.65s
Declination -28d 07m 37.33s
Redshift 2.559000
Heliocentric radial velocity 767,169 km/s
Distance 10.762 Gly (light travel time distance)
Apparent magnitude  (V)0.085
Apparent magnitude  (B)0.113
Surface brightness 18.5
Characteristics
Type FSRQ, 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]

Contents

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]

Related Research Articles

The Eddington luminosity, also referred to as the Eddington limit, is the maximum luminosity a body can achieve when there is balance between the force of radiation acting outward and the gravitational force acting inward. The state of balance is called hydrostatic equilibrium. When a star exceeds the Eddington luminosity, it will initiate a very intense radiation-driven stellar wind from its outer layers. Since most massive stars have luminosities far below the Eddington luminosity, their winds are driven mostly by the less intense line absorption. The Eddington limit is invoked to explain the observed luminosities of accreting black holes such as quasars.

<span class="mw-page-title-main">Blazar</span> Very compact quasi-stellar radio source

A blazar is an active galactic nucleus (AGN) with a relativistic jet directed very nearly towards an observer. Relativistic beaming of electromagnetic radiation from the jet makes blazars appear much brighter than they would be if the jet were pointed in a direction away from Earth. Blazars are powerful sources of emission across the electromagnetic spectrum and are observed to be sources of high-energy gamma ray photons. Blazars are highly variable sources, often undergoing rapid and dramatic fluctuations in brightness on short timescales. Some blazar jets appear to exhibit superluminal motion, another consequence of material in the jet traveling toward the observer at nearly the speed of light.

<span class="mw-page-title-main">GRB 160625B</span>

GRB 160625B was a bright gamma-ray burst (GRB) detected by NASA's Fermi Gamma-ray Space Telescope on 25 June 2016 and, three minutes later, by the Large Area Telescope. This was followed by a bright prompt optical flash, during which variable linear polarization was measured. This was the first time that these observations were made when the GRB was still bright and active. The source of the GRB was a possible black hole, within the Delphinus constellation, about 9 billion light-years (light travel distance) away (a redshift of z = 1.406). It had a fluence of 5.7×10−4 erg cm−2, and energy of 5 × 1054 erg. The burst lasted over 11 minutes (680 s), and is one of the most energetic bursts ever recorded.

TXS 0506+056 is a very high energy blazar – a quasar with a relativistic jet pointing directly towards Earth – of BL Lac-type. With a redshift of 0.3365 ± 0.0010, it has a luminosity distance of about 1.75 gigaparsecs. Its approximate location on the sky is off the left shoulder of the constellation Orion. Discovered as a radio source in 1983, the blazar has since been observed across the entire electromagnetic spectrum.

<span class="mw-page-title-main">AP Librae</span> Active galactic nucleus in the constellation Libra

AP Librae is a BL Lacertae object located at a distance of 700 million light years in the southern constellation of Libra. In the visual band it is one of the most active blazars known. AP Lib is surrounded by an extended source with a spectrum characteristic of a red-shifted giant elliptical galaxy. The derived visual magnitude of this region is 15.0, and it follows a radially decreasing brightness that is characteristic of an elliptical. Seven fainter galaxies are visible within an angular radius of 9′, suggesting it is the brightest member of a galactic cluster.

<span class="mw-page-title-main">3C 345</span> Quasar in the Hercules constellation

3C 345 is a blazar/flat spectrum radio quasar located in the constellation of Hercules. It is noted for hosting a superluminal jet and its variability in almost all wave bands.

<span class="mw-page-title-main">IC 4516</span> Galaxy located in Boötes

IC 4516 is a type E elliptical galaxy located in Boötes. Its redshift is 0.045618 which corresponds IC 4516 to be located 667 million light-years from Earth. The galaxy was discovered by Lewis Swift on June 2, 1898, which was his last discovery after spending half a century observing astronomical objects, starting with the observation of the Great Comet in 1843.

<span class="mw-page-title-main">4C +71.07</span> Quasar in the constellation Ursa Major

4C +71.07 known as S5 0836+71, is a quasar located in the constellation Ursa Major. Based on its high redshift, the object is located 10.7 billion light-years away from Earth and such, classified as a blazar with a flat-spectrum radio source and features a radio jet.

<span class="mw-page-title-main">PKS 0537-286</span> Quasar in the constellation Columba

PKS 0537-286, also known as QSO B0537-286, is a quasar located in the constellation Columba. With a redshift of 3.104, the object is located 11.4 billion light years away and belongs to the flat spectrum radio quasar blazar subclass (FSQR). It is one of the most luminous known high-redshift quasars.

<span class="mw-page-title-main">PKS 0438-436</span> Quasar in the constellation Caelum

PKS 0438-436, also known as PKS J0440-4333, is a quasar located in constellation Caelum. With a high redshift of 2.86, the object is located 11.2 billion light-years from Earth and is classified as a blazar due to its flat-spectrum radio source, (in terms of the flux density as with α < 0.5 and its optical polarization.

<span class="mw-page-title-main">PKS 2126-158</span> Quasar in the constellation Capricornus

PKS 2126-158, also known as PKS 2126-15, is a quasar located in Capricornus. It has a redshift of 3.268000, which corresponds to the distance of 11.5 billion light years. It is classified as a gigahertz peaked-spectrum quasar (GPS) with a flat-spectrum radio source and a blazar, a type of active galaxy shooting an astrophysical jet towards Earth.

<span class="mw-page-title-main">PKS 0226-559</span>

PKS 0226-559 known as PMN J0228-5546 is a quasar located in the constellation Horologium. At the redshift of 2.464, the object is roughly 10.6 billion light-years from Earth.

<span class="mw-page-title-main">PKS 1144-379</span>

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

<span class="mw-page-title-main">PKS 1402-012</span>

PKS 1402-012, also known as UM 632, is a quasar located in the constellation of Virgo. With a redshift of 2.51, the object is located 10.7 billion light-years from Earth.

<span class="mw-page-title-main">PKS 1148-001</span> Quasar in the constellation Virgo

PKS 1148-001 also known as UM 458 and 4C -00.47, is a quasar located in the constellation of Virgo. Its redshift is 1.979, estimating the object to be located 10.2 billion light-years from Earth.

<span class="mw-page-title-main">4C +03.10</span> Quasar in the constellation Orion

4C +03.10 also known as PKS 0505+03 and OG +008, is a quasar located in the constellation of Orion. At a redshift of 2.46, the object is located 10.6 billion light-years away from Earth.

<span class="mw-page-title-main">PKS 1402+044</span>

PKS 1402+044 is a quasar located in the constellation of Virgo. It has a redshift of 3.207, estimating the object to be located 11.3 billion light-years away from Earth.

<span class="mw-page-title-main">PKS 2338+000</span>

PKS 2338+000 also known as PGC 1162543 and OGC 123, is a massive type-cD elliptical galaxy located in the constellation of Pisces. With a redshift of 0.276, the galaxy is located 3.5 billion light-years from Earth. The galaxy is the brightest cluster galaxy inside the galaxy cluster RX J2341+0018 which is a rich cluster, X-ray luminous.

<span class="mw-page-title-main">7C 1415+2556</span>

7C 1415+2556 also known as 2E 1415+2557 and PGC 1747267, is a BL Lac object with an X-ray flux of >=4×10-13 ergs s-1 cm-2, located in the constellation of Boötes. With a redshift of 0.24, the galaxy is located 3.2 billion light-years from Earth. It was discovered in 1988 as part of a program of optical polarimetry of a complete sample of radio sources.

<span class="mw-page-title-main">RIQ J1336+1725</span>

RIQ J1336+1725 also known as PB 4007 and PG 1333+177, is a quasar located in the constellation of Coma Berenices. At a low redshift of 0.55, the object is located 6.5 billion light-years from Earth. This quasar is known to have a Lyman edge region that is formed by its thermally emitting accretion disk.

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. 1 2 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. 1 2 3 4 5 6 7 8 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. 1 2 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.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.