PKS 1402-012

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PKS 1402-012
DESI Legacy Surveys image of PKS 1402-012.jpg
The quasar PKS 1402-012, seen by DESI Legacy Surveys
Observation data (J2000.0 epoch)
Constellation Virgo
Right ascension 14h 04m 45.895s
Declination -01d 30m 21.947s
Redshift 2.518154
Heliocentric radial velocity 754,924 km/s
Distance 10.732 Gly (light travel time distance)
Apparent magnitude  (V)0.149
Apparent magnitude  (B)0.197
Surface brightness 18.3
Characteristics
Type Opt.var, RLQ
Other designations
UM 632, 2QZ J140445.8-013022, PGC 50193, NVSS J140445-013021, QUEST 123404, TXS 1402-012, IRCF J140445.8-013021

PKS 1402-012 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. [1]

Contents

Characteristics

As one of the objects observed and noted by researchers analyzing the Parkes quarter-Jansky flat-spectrum sample at Parkes Observatory, [2] [3] PKS 1402-012 is classified a blazar. [4] [5] [6] Optically variable, [7] it is a type of active galaxy shooting out an astrophysical jet towards the direction of Earth, PKS 1402-012 is found to emit out large amounts radiation over the whole electromagnetic spectrum up to TeV energies. [8] It is notable to be a target of prior X-ray observations mentioned by the Einstein quasar database [9] and a high redshift gamma ray loud quasar. [10] [11]

PKS 1402-012 is also a BL Lac object [12] and such has a bolometric luminosity of 1044 ≲ L≲ 1048 erg s−1 with a weak emission-line showing EW(C iv)≲10 Å, with a high Eddington ratio, in relationship to the modified Baldwin effect. [13] Like other quasars, PKS 1402-012 has a flux-density distribution and luminosity function stronger than 2.4 mJy [14] The flux-density varies time to time. In 1972, the flux density was at 0.67 Jy with the flux-density decreasing to 0.15 Jy in 1989. [15]

The host galaxy of PKS 1402-012 is a massive starburst early-type galaxy, located inside an overdense rich galaxy cluster at a >=2σ level. [16] It is found in amidst of a violent star-forming event, producing a significant fraction of stars with 0.5 billion years [17] and large quantities of high-density ionized gas in its regions. [18] The quasar contains an extragalactic radio source, [19] which is responsible for powering strong star formations with rates of ~500 M_sun per year, consistent with its "quasar mode" accretion in which cold gas flows fuel both the AGN and starburst. [14] [20]

According to Hubble Space Telescope, PKS 1402-012 is a gravitational lensed quasar which researchers noted ground based direct imaging characterized by a good dynamical range is the best observational strategy in the long term. [21] [22]

Absorption-line system

PKS 1402-012 has an absorption-line. [23] In a study of 821 quasars and 8558 absorption-line systems sampled in the quasar spectra, researchers found lines of heavy elements and neutral hydrogen in PKS 1402–012. [24] Apart from that, the quasar also shows detections of HI 21 cm absorption, [25] a strong C IV absorber stronger EWrest>=0.5 Å [26] and damped Lyman α (DLA) system, containing ~90 per cent of the neutral HI mass. [27] [28]

Through observation by researchers for its spectral line equivalent widths, the quasar also contains O [III] narrow lines and C IV λ1549 and Mg II λ2799 broad lines, correlating positively with R I at 4σ-8σ level but no strong depended on R suggesting the line-of-sight angle to the radio-jet axis of PKS 1402-012 decreases. [29] Furthermore, they found Ca ii absorbers with a rest frame equaling to widths of Wr,3934 = 15-799 mÅ and column density of log N(Ca ii) = 11.25-13.04, following a steep power law pattern of, f(N) ∝ N - β and slope angle - β = -1.68. [30]

Researchers also detected a 21-cm absorption in Mg ii absorbers of PKS 1402–012. Through results, they found the quasar has a linear size of LS < 100 pc, since its detection rate is higher at cm wavelengths. With a velocity width of ΔV > 100 km s−1, PKS 1402-012 also shows an extended radio morphology at arcsecond scales. Researchers noted the 21-cm detection rate in strong Mg ii systems is constant over 0.5 < zabs < 1.5; that is over ~30% of the total age of universe. [31]

Black hole

According to researchers who used a mass estimator based on the Hβ, Mg II, and C IV emission lines, [32] they found the supermassive black hole in PKS 1402-012 is found to grow at an exponentially rate with a solar mass range estimated 108.8-1010.7 Msolar and high luminosity of 1045.2<λLλ(5100 Å)<1047.3 ergs s−1. [33]

The growth rate of the black hole is found longer compared to the age of the universe with a corresponding epoch, suggesting there was an earlier episode of faster growth at z >~3. [33]

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References

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  32. ↑ Shen, Yue; Greene, Jenny E.; Strauss, Michael A.; Richards, Gordon T.; Schneider, Donald P. (2008-06-01). "Biases in Virial Black Hole Masses: An SDSS Perspective". The Astrophysical Journal. 680 (1): 169–190. arXiv: 0709.3098 . Bibcode:2008ApJ...680..169S. doi:10.1086/587475. ISSN   0004-637X.
  33. 1 2 Netzer, Hagai; Lira, Paulina; Trakhtenbrot, Benny; Shemmer, Ohad; Cury, Iara (2007-12-01). "Black Hole Mass and Growth Rate at High Redshift". The Astrophysical Journal. 671 (2): 1256–1263. arXiv: 0708.3787 . Bibcode:2007ApJ...671.1256N. doi:10.1086/523035. ISSN   0004-637X.
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