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PKS 1402+044
PKS 1402+044 captured by DESI Legacy Surveys
Observation data (J2000.0 epoch)
ConstellationVirgo
Right ascension14h 05m 01.12s
Declination+04d 15m 35.82s
Redshift3.207977
Heliocentric radial velocity961,727 km/s
Distance11.323 Gly (light travel time distance)
Apparent magnitude (V)0.074
Apparent magnitude (B)0.098
Surface brightness19.6
Characteristics
TypeFSRQ; BAL, BLLAC
Other designations
NVSS J140501+041536, FIRST J140501.1+041535, PGC 2827828, TXS 1402+044, IRCF J140501.1+041535, ZS 1402+043, MRC 1402+044, PMN J1405+0415, SDSS J140501.12+041535.7

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.[1][2]

Characteristics[edit]

PKS 1402+044 is classified a broad absorption-line quasar (BAL QSO) observed by Sloan Digital Sky Survey[3] with a flat-spectrum radio source.[4][5] It is also classified a blazar, a type of active galaxy[6][7] and such produces a powerful astrophysical jet that is shot out into the depths of intergalactic space.[8] Observations made by the European VLBI network, finds the jet is weakly distorted and considered most distant in the universe's history.[9]

The blazar is known to be in its quiescent state, but it shows repeated periods of outbursts that are visible throughout the electromagnetic spectrum.[10] According to observations from Gamma-Ray Blazar Survey and Fermi Gamma-Ray Space Telescope, PKS 1402+044 is found optically variable with >6σ significance,[11] γ-ray detected and more Compton dominated than high synchrotron peaked (HSP) BL Lac objects.[12]

Through radio imaging by researchers, the quasar is core-dominated with fluctuating radio emission and radio morphology found smaller in comparison of steep-spectrum quasars.[13] It is also the brightest X-ray quasar but with compact dispersion of <logL χ1>=46.15±0.25 at high redshift.[14] The quasar is radio-loud with straightened jet magnetic fields along its source axis and a lobe field found to have a misaligned orientation.[15]

Observations of PKS 1402+044[edit]

The intrinsic C iv in BAL QSO fractions like PKS 1402+044 is calculated as 41 ± 5 per cent. The allows the researchers to study further on the quasar's luminosity and redshift. From the high redshifts between z≃ 4.0 to z≃ 2.0, factor of 3.5 ± 0.4 of the intrinsic fraction does declines but no luminosity reliance. However the rate of change of the intrinsic fraction has 3σ limits with a luminosity value of -6.9 and 7.0 percent dex−1.[16] Moreover, the quasar has a stronger narrow C IV λ1549 absorption line, than EWrest>=0.5 Å.[17]

PKS 1402+044 has a weak emission-line. Researchers who studied the quasar, found it reveals a sign of hot thermal dust emission (T ~ 1000 K) containing a rest-frame of 0.1-5 μm spectral energy distribution, alike to normal quasars. Apart from that, polarization, variability, and radio properties are quite different from BL Lac objects, thus eliminating the possibilities of continuum boosting by the quasar's relativistic jet.[18]

Researchers who investigated the frequency-dependent radio properties of the jet in PKS 1402+044, found the quasar of "core-jet" morphology. The core-jet features extends out to kilo-parsec scales, with perpendicular spectral index and shallow brightness temperature. As the core is further away, the distance of the jet increases. This suggests the jet is collimated by the magnetic field, with mass of the central object estimated to be ~109 ~ M_⊙, which the upper limit of the jet proper motion of PKS 1402+044 is 0.03 mas yr−1 (~3c) when placed at east–west direction.[19]

Host galaxy[edit]

The host galaxy of PKS 1402+044 is a large disk galaxy.[20][21] It is an active galaxy containing an ionizing photons per second rate of Q_H I ∼ 1056 and a monochromatic λ = 912 Å luminosity of LUV ∼ 1023 W Hz−1.[22] Moreover, the host galaxy has an extremely bright radio core[23] with a galactic halo surrounding the regions with a dense parameter of interstellar gas.[24] According to researcher investigating on limits from detectable continuum flux from PKS 1402+044, a gas cloud is associated with the galaxy.[25]

Dampen Lyα System[edit]

The dampen Lyα System[26] within the region of PKS 1402+044 is metal rich containing values of [logN(Zn+)>=13.15 or logN(Si+)>=15.95]. The system shows strong signatures of Zn II λ2026 and Si II λ1808 lines, indicating it is due to Type II supernovae.[27] Moreover, 90% of hydrogen mass is embedded inside the dampen Lyα system with values of N(HI) >1.6 × 1017 atom cm−2. The column density of the dampened Lyα System is calculated to 1.6 × 1021 atom cm-2 at z < 3.5.[28] As for hydrogen ion ionization rate in PKS 1402+044 is evaluated to be 1.9+1.2-1.0×10−12 s−1.[29][30]

Moreover, the Lyman-alpha forest lines in PKS 1402+044 are powerful and broad, when compared with similar lines that is further from quasars. These are larger and have no mutual relationship with the luminosity of the quasar, its radio loudness or optical spectral index. These signs shows there are more lines at high redshifts but have weak connections caused by presence of associated metal line systems.[31] The covering factor for absorbing clouds inside the extended emission-line region of PKS 1402+044 is either minor or identical to 0.15 when noticed by spectroscopic observation in which researchers seek for Lyman-limit regions of 32 quasars.[32]

Green Bank Telescope (GBT) and Berkeley-Illinois-Maryland Association (BIMA) array observed PKS 1402+044 and discovered the redshifted millimetre absorptions had increased and reached 3σ limits of τ<= 0.1. This is a significant improvement, which the researchers provided restrictions for millimetre absorptions beneath the atmospheric cut-off for the Lyman and Werner H2 bands in ultraviolet measurements of (zabs<~ 1.8).[33]

Black hole[edit]

The black hole found in PKS 1402+044 has a mass of log MBH, M○ > 9 with a luminous accretion disk weighing Ldisk >1046 erg s−1. The broadband spectral energy distribution inside the black hole is influenced by high-energy radiation, indicating the jets are fast moving and the most luminous date-to-date.[34]

According to researchers who used a virial black hole mass estimator based on the Hβ, Mg II, and C IV emission lines,[35] the black hole mass is gauged to be μ 0 = 0.55 ± 0.22, ξ μR = 1.09 ± 0.10, and {ξ }μ X=-{0.59}-0.15+0.16 with natural logarithm of the Gaussian intrinsic scatter measured with a log-mass direction {ln}{ɛ }μ =-{0.04}-0.13+0.14. This suggests improvements when compared to earlier mass scaling result, given the active galactic nuclei sample size has increased from 18 to 30.[36]

References[edit]

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source: https://en.wikipedia.org/wiki/PKS_1402%2B044

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