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== Characteristics ==
== Characteristics ==
As one of the objects observed and noted by researchers analyzing the Parkes quarter-Jansky flat-spectrum sample at [[Parkes Observatory]],<ref>{{Cite journal |last1=Wall |first1=J. V. |last2=Jackson |first2=C. A. |last3=Shaver |first3=P. A. |last4=Hook |first4=I. M. |last5=Kellermann |first5=K. I. |date=2005-04-01 |title=The Parkes quarter-Jansky flat-spectrum sample. III. Space density and evolution of QSOs |url=https://ui.adsabs.harvard.edu/abs/2005A&A...434..133W |journal=Astronomy and Astrophysics |volume=434 |issue=1 |pages=133–148 |doi=10.1051/0004-6361:20041786 |arxiv=astro-ph/0408122 |bibcode=2005A&A...434..133W |issn=0004-6361}}</ref><ref>{{Cite journal |last1=Jackson |first1=C. A. |last2=Wall |first2=J. V. |last3=Shaver |first3=P. A. |last4=Kellermann |first4=K. I. |last5=Hook |first5=I. M. |last6=Hawkins |first6=M. R. S. |date=2002-04-01 |title=The Parkes quarter-Jansky flat-spectrum sample. I. Sample selection and source identifications |url=https://ui.adsabs.harvard.edu/abs/2002A&A...386...97J |journal=Astronomy and Astrophysics |volume=386 |pages=97–113 |doi=10.1051/0004-6361:20020119 |bibcode=2002A&A...386...97J |issn=0004-6361}}</ref> A high redshift quasar [[gamma ray]] loud,<ref>{{Cite journal |last1=Shemmer |first1=O. |last2=Netzer |first2=H. |last3=Maiolino |first3=R. |last4=Oliva |first4=E. |last5=Croom |first5=S. |last6=Corbett |first6=E. |last7=di Fabrizio |first7=L. |date=2004-10-01 |title=Near-Infrared Spectroscopy of High-Redshift Active Galactic Nuclei. I. A Metallicity-Accretion Rate Relationship |url=https://ui.adsabs.harvard.edu/abs/2004ApJ...614..547S |journal=The Astrophysical Journal |volume=614 |issue=2 |pages=547–557 |doi=10.1086/423607 |arxiv=astro-ph/0406559 |bibcode=2004ApJ...614..547S |issn=0004-637X}}</ref><ref>{{Cite journal |last=Nair |first=A. D. |date=1997-05-01 |title=Investigating properties of a set of variable AGN with cluster analysis |url=https://ui.adsabs.harvard.edu/abs/1997MNRAS.287..641N |journal=Monthly Notices of the Royal Astronomical Society |volume=287 |issue=3 |pages=641–650 |doi=10.1093/mnras/287.3.641 |bibcode=1997MNRAS.287..641N |issn=0035-8711}}</ref> PKS 1402-012 is classfied a [[blazar]].<ref>{{Cite journal |last1=Xiong |first1=Dingrong |last2=Zhang |first2=Xiong |last3=Bai |first3=Jinming |last4=Zhang |first4=Haojing |date=2015-07-01 |title=Basic properties of Fermi blazars and the 'blazar sequence' |url=https://ui.adsabs.harvard.edu/abs/2015MNRAS.450.3568X |journal=Monthly Notices of the Royal Astronomical Society |volume=450 |issue=4 |pages=3568–3578 |doi=10.1093/mnras/stv812 |arxiv=1504.02706 |bibcode=2015MNRAS.450.3568X |issn=0035-8711}}</ref><ref>{{Cite journal |last1=Mao |first1=Peiyuan |last2=Urry |first2=C. Megan |last3=Massaro |first3=Francesco |last4=Paggi |first4=Alessandro |last5=Cauteruccio |first5=Joe |last6=Künzel |first6=Soren R. |date=2016-06-01 |title=A Comprehensive Statistical Description of Radio-through-Gamma-Ray Spectral Energy Distributions of All Known Blazars |journal=The Astrophysical Journal Supplement Series |volume=224 |issue=2 |pages=26 |doi=10.3847/0067-0049/224/2/26 |doi-access=free |arxiv=1604.03856 |bibcode=2016ApJS..224...26M |issn=0067-0049}}</ref><ref>{{Cite journal |last1=Massaro |first1=E. |last2=Giommi |first2=P. |last3=Leto |first3=C. |last4=Marchegiani |first4=P. |last5=Maselli |first5=A. |last6=Perri |first6=M. |last7=Piranomonte |first7=S. |last8=Sclavi |first8=S. |date=2009-02-01 |title=Roma-BZCAT: a multifrequency catalogue of blazars |url=https://ui.adsabs.harvard.edu/abs/2009A&A...495..691M |journal=Astronomy and Astrophysics |volume=495 |issue=2 |pages=691–696 |doi=10.1051/0004-6361:200810161 |arxiv=0810.2206 |bibcode=2009A&A...495..691M |issn=0004-6361}}</ref> Optically variable,<ref>{{Cite journal |last1=MacLeod |first1=Chelsea L. |last2=Ivezić |first2=Željko |last3=Sesar |first3=Branimir |last4=de Vries |first4=Wim |last5=Kochanek |first5=Christopher S. |last6=Kelly |first6=Brandon C. |last7=Becker |first7=Andrew C. |last8=Lupton |first8=Robert H. |last9=Hall |first9=Patrick B. |last10=Richards |first10=Gordon T. |last11=Anderson |first11=Scott F. |last12=Schneider |first12=Donald P. |date=2012-07-01 |title=A Description of Quasar Variability Measured Using Repeated SDSS and POSS Imaging |url=https://ui.adsabs.harvard.edu/abs/2012ApJ...753..106M |journal=The Astrophysical Journal |volume=753 |issue=2 |pages=106 |doi=10.1088/0004-637X/753/2/106 |arxiv=1112.0679 |bibcode=2012ApJ...753..106M |issn=0004-637X}}</ref> 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.<ref>{{Cite journal |last1=Schleicher |first1=Bernd |last2=Arbet-Engels |first2=Axel |last3=Baack |first3=Dominik |last4=Balbo |first4=Matteo |last5=Biland |first5=Adrian |last6=Blank |first6=Michael |last7=Bretz |first7=Thomas |last8=Bruegge |first8=Kai |last9=Bulinski |first9=Michael |last10=Buss |first10=Jens |last11=Doerr |first11=Manuel |last12=Dorner |first12=Daniela |last13=Elsaesser |first13=Dominik |last14=Grischagin |first14=Sergej |last15=Hildebrand |first15=Dorothee |date=2019-05-01 |title=Fractional Variability—A Tool to Study Blazar Variability |journal=Galaxies |volume=7 |issue=2 |pages=62 |doi=10.3390/galaxies7020062|doi-access=free |bibcode=2019Galax...7...62S }}</ref> It is notable to be a target of prior [[X-ray astronomy|X-ray observations]] mentioned by the Einstein quasar database.<ref>{{Cite journal |last1=Wilkes |first1=Belinda J. |last2=Tananbaum |first2=Harvey |last3=Worrall |first3=D. M. |last4=Avni |first4=Yoram |last5=Oey |first5=M. S. |last6=Flanagan |first6=Joan |date=1994-05-01 |title=The Einstein Database of IPC X-Ray Observations of Optically Selected and Radio-selected Quasars. I. |url=https://ui.adsabs.harvard.edu/abs/1994ApJS...92...53W |journal=The Astrophysical Journal Supplement Series |volume=92 |pages=53 |doi=10.1086/191959 |bibcode=1994ApJS...92...53W |issn=0067-0049}}</ref>
As one of the objects observed and noted by researchers analyzing the Parkes quarter-Jansky flat-spectrum sample at [[Parkes Observatory]],<ref>{{Cite journal |last1=Wall |first1=J. V. |last2=Jackson |first2=C. A. |last3=Shaver |first3=P. A. |last4=Hook |first4=I. M. |last5=Kellermann |first5=K. I. |date=2005-04-01 |title=The Parkes quarter-Jansky flat-spectrum sample. III. Space density and evolution of QSOs |url=https://ui.adsabs.harvard.edu/abs/2005A&A...434..133W |journal=Astronomy and Astrophysics |volume=434 |issue=1 |pages=133–148 |doi=10.1051/0004-6361:20041786 |arxiv=astro-ph/0408122 |bibcode=2005A&A...434..133W |issn=0004-6361}}</ref><ref>{{Cite journal |last1=Jackson |first1=C. A. |last2=Wall |first2=J. V. |last3=Shaver |first3=P. A. |last4=Kellermann |first4=K. I. |last5=Hook |first5=I. M. |last6=Hawkins |first6=M. R. S. |date=2002-04-01 |title=The Parkes quarter-Jansky flat-spectrum sample. I. Sample selection and source identifications |url=https://ui.adsabs.harvard.edu/abs/2002A&A...386...97J |journal=Astronomy and Astrophysics |volume=386 |pages=97–113 |doi=10.1051/0004-6361:20020119 |bibcode=2002A&A...386...97J |issn=0004-6361}}</ref> PKS 1402-012 is classfied a [[blazar]].<ref>{{Cite journal |last1=Xiong |first1=Dingrong |last2=Zhang |first2=Xiong |last3=Bai |first3=Jinming |last4=Zhang |first4=Haojing |date=2015-07-01 |title=Basic properties of Fermi blazars and the 'blazar sequence' |url=https://ui.adsabs.harvard.edu/abs/2015MNRAS.450.3568X |journal=Monthly Notices of the Royal Astronomical Society |volume=450 |issue=4 |pages=3568–3578 |doi=10.1093/mnras/stv812 |arxiv=1504.02706 |bibcode=2015MNRAS.450.3568X |issn=0035-8711}}</ref><ref>{{Cite journal |last1=Mao |first1=Peiyuan |last2=Urry |first2=C. Megan |last3=Massaro |first3=Francesco |last4=Paggi |first4=Alessandro |last5=Cauteruccio |first5=Joe |last6=Künzel |first6=Soren R. |date=2016-06-01 |title=A Comprehensive Statistical Description of Radio-through-Gamma-Ray Spectral Energy Distributions of All Known Blazars |journal=The Astrophysical Journal Supplement Series |volume=224 |issue=2 |pages=26 |doi=10.3847/0067-0049/224/2/26 |doi-access=free |arxiv=1604.03856 |bibcode=2016ApJS..224...26M |issn=0067-0049}}</ref><ref>{{Cite journal |last1=Massaro |first1=E. |last2=Giommi |first2=P. |last3=Leto |first3=C. |last4=Marchegiani |first4=P. |last5=Maselli |first5=A. |last6=Perri |first6=M. |last7=Piranomonte |first7=S. |last8=Sclavi |first8=S. |date=2009-02-01 |title=Roma-BZCAT: a multifrequency catalogue of blazars |url=https://ui.adsabs.harvard.edu/abs/2009A&A...495..691M |journal=Astronomy and Astrophysics |volume=495 |issue=2 |pages=691–696 |doi=10.1051/0004-6361:200810161 |arxiv=0810.2206 |bibcode=2009A&A...495..691M |issn=0004-6361}}</ref> Optically variable,<ref>{{Cite journal |last1=MacLeod |first1=Chelsea L. |last2=Ivezić |first2=Željko |last3=Sesar |first3=Branimir |last4=de Vries |first4=Wim |last5=Kochanek |first5=Christopher S. |last6=Kelly |first6=Brandon C. |last7=Becker |first7=Andrew C. |last8=Lupton |first8=Robert H. |last9=Hall |first9=Patrick B. |last10=Richards |first10=Gordon T. |last11=Anderson |first11=Scott F. |last12=Schneider |first12=Donald P. |date=2012-07-01 |title=A Description of Quasar Variability Measured Using Repeated SDSS and POSS Imaging |url=https://ui.adsabs.harvard.edu/abs/2012ApJ...753..106M |journal=The Astrophysical Journal |volume=753 |issue=2 |pages=106 |doi=10.1088/0004-637X/753/2/106 |arxiv=1112.0679 |bibcode=2012ApJ...753..106M |issn=0004-637X}}</ref> 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.<ref>{{Cite journal |last1=Schleicher |first1=Bernd |last2=Arbet-Engels |first2=Axel |last3=Baack |first3=Dominik |last4=Balbo |first4=Matteo |last5=Biland |first5=Adrian |last6=Blank |first6=Michael |last7=Bretz |first7=Thomas |last8=Bruegge |first8=Kai |last9=Bulinski |first9=Michael |last10=Buss |first10=Jens |last11=Doerr |first11=Manuel |last12=Dorner |first12=Daniela |last13=Elsaesser |first13=Dominik |last14=Grischagin |first14=Sergej |last15=Hildebrand |first15=Dorothee |date=2019-05-01 |title=Fractional Variability—A Tool to Study Blazar Variability |journal=Galaxies |volume=7 |issue=2 |pages=62 |doi=10.3390/galaxies7020062|doi-access=free |bibcode=2019Galax...7...62S }}</ref> It is notable to be a target of prior [[X-ray astronomy|X-ray observations]] mentioned by the Einstein quasar database<ref>{{Cite journal |last1=Wilkes |first1=Belinda J. |last2=Tananbaum |first2=Harvey |last3=Worrall |first3=D. M. |last4=Avni |first4=Yoram |last5=Oey |first5=M. S. |last6=Flanagan |first6=Joan |date=1994-05-01 |title=The Einstein Database of IPC X-Ray Observations of Optically Selected and Radio-selected Quasars. I. |url=https://ui.adsabs.harvard.edu/abs/1994ApJS...92...53W |journal=The Astrophysical Journal Supplement Series |volume=92 |pages=53 |doi=10.1086/191959 |bibcode=1994ApJS...92...53W |issn=0067-0049}}</ref> and a high redshift [[gamma ray]] loud quasar.<ref>{{Cite journal |last1=Shemmer |first1=O. |last2=Netzer |first2=H. |last3=Maiolino |first3=R. |last4=Oliva |first4=E. |last5=Croom |first5=S. |last6=Corbett |first6=E. |last7=di Fabrizio |first7=L. |date=2004-10-01 |title=Near-Infrared Spectroscopy of High-Redshift Active Galactic Nuclei. I. A Metallicity-Accretion Rate Relationship |url=https://ui.adsabs.harvard.edu/abs/2004ApJ...614..547S |journal=The Astrophysical Journal |volume=614 |issue=2 |pages=547–557 |arxiv=astro-ph/0406559 |bibcode=2004ApJ...614..547S |doi=10.1086/423607 |issn=0004-637X}}</ref><ref>{{Cite journal |last=Nair |first=A. D. |date=1997-05-01 |title=Investigating properties of a set of variable AGN with cluster analysis |url=https://ui.adsabs.harvard.edu/abs/1997MNRAS.287..641N |journal=Monthly Notices of the Royal Astronomical Society |volume=287 |issue=3 |pages=641–650 |bibcode=1997MNRAS.287..641N |doi=10.1093/mnras/287.3.641 |issn=0035-8711}}</ref>


PKS 1402-012 is also a [[BL Lacertae object|BL Lac object]]<ref>{{Cite journal |last1=Landoni |first1=M. |last2=Falomo |first2=R. |last3=Treves |first3=A. |last4=Sbarufatti |first4=B. |date=October 2014 |title=Spectroscopy of BL Lacertae objects of extraordinary luminosity |url=http://dx.doi.org/10.1051/0004-6361/201424232 |journal=Astronomy & Astrophysics |volume=570 |pages=A126 |doi=10.1051/0004-6361/201424232 |arxiv=1407.3085 |bibcode=2014A&A...570A.126L |issn=0004-6361}}</ref> and such has a [[Luminosity|bolometric luminosity]] of 10<sup>44</sup> ≲ L≲ 10<sup>48</sup> erg s<sup>−1</sup> with a weak [[Spectral line|emission-line]] showing EW(C iv)≲10 Å, with a high [[Eddington luminosity|Eddington]] ratio, in relationship to the modified [[Baldwin effect]].<ref>{{Cite journal |last1=Shemmer |first1=Ohad |last2=Lieber |first2=Sara |date=2015-06-01 |title=Weak Emission-line Quasars in the Context of a Modified Baldwin Effect |url=https://ui.adsabs.harvard.edu/abs/2015ApJ...805..124S |journal=The Astrophysical Journal |volume=805 |issue=2 |pages=124 |doi=10.1088/0004-637X/805/2/124 |arxiv=1503.07547 |bibcode=2015ApJ...805..124S |issn=0004-637X}}</ref> Like other quasars, PKS 1402-012 has a [[Flux density|flux-density]] distribution and [[Luminous efficiency function|luminosity function]] stronger than 2.4 mJy<ref name=":0">{{Cite journal |last1=Condon |first1=J. J. |last2=Kellermann |first2=K. I. |last3=Kimball |first3=Amy E. |last4=Ivezic |first4=Zeljko |last5=Perley |first5=R. A. |date=2013-04-12 |title=AGN and Starburst Radio Emission from Optically Selected QSOs |journal=The Astrophysical Journal |volume=768 |issue=1 |pages=37 |doi=10.1088/0004-637X/768/1/37 |arxiv=1303.3448 |issn=0004-637X}}</ref> 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.<ref>{{Cite journal |last1=Jackson |first1=C. A. |last2=Wall |first2=J. V. |last3=Shaver |first3=P. A. |last4=Kellermann |first4=K. I. |last5=Hook |first5=I. M. |last6=Hawkins |first6=M. R. S. |date=April 2002 |title=The Parkes quarter-Jansky flat-spectrum sample |url=http://dx.doi.org/10.1051/0004-6361:20020119 |journal=Astronomy & Astrophysics |volume=386 |issue=1 |pages=97–113 |doi=10.1051/0004-6361:20020119 |bibcode=2002A&A...386...97J |issn=0004-6361}}</ref>
PKS 1402-012 is also a [[BL Lacertae object|BL Lac object]]<ref>{{Cite journal |last1=Landoni |first1=M. |last2=Falomo |first2=R. |last3=Treves |first3=A. |last4=Sbarufatti |first4=B. |date=October 2014 |title=Spectroscopy of BL Lacertae objects of extraordinary luminosity |url=http://dx.doi.org/10.1051/0004-6361/201424232 |journal=Astronomy & Astrophysics |volume=570 |pages=A126 |doi=10.1051/0004-6361/201424232 |arxiv=1407.3085 |bibcode=2014A&A...570A.126L |issn=0004-6361}}</ref> and such has a [[Luminosity|bolometric luminosity]] of 10<sup>44</sup> ≲ L≲ 10<sup>48</sup> erg s<sup>−1</sup> with a weak [[Spectral line|emission-line]] showing EW(C iv)≲10 Å, with a high [[Eddington luminosity|Eddington]] ratio, in relationship to the modified [[Baldwin effect]].<ref>{{Cite journal |last1=Shemmer |first1=Ohad |last2=Lieber |first2=Sara |date=2015-06-01 |title=Weak Emission-line Quasars in the Context of a Modified Baldwin Effect |url=https://ui.adsabs.harvard.edu/abs/2015ApJ...805..124S |journal=The Astrophysical Journal |volume=805 |issue=2 |pages=124 |doi=10.1088/0004-637X/805/2/124 |arxiv=1503.07547 |bibcode=2015ApJ...805..124S |issn=0004-637X}}</ref> Like other quasars, PKS 1402-012 has a [[Flux density|flux-density]] distribution and [[Luminous efficiency function|luminosity function]] stronger than 2.4 mJy<ref name=":0">{{Cite journal |last1=Condon |first1=J. J. |last2=Kellermann |first2=K. I. |last3=Kimball |first3=Amy E. |last4=Ivezic |first4=Zeljko |last5=Perley |first5=R. A. |date=2013-04-12 |title=AGN and Starburst Radio Emission from Optically Selected QSOs |journal=The Astrophysical Journal |volume=768 |issue=1 |pages=37 |doi=10.1088/0004-637X/768/1/37 |arxiv=1303.3448 |issn=0004-637X}}</ref> 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.<ref>{{Cite journal |last1=Jackson |first1=C. A. |last2=Wall |first2=J. V. |last3=Shaver |first3=P. A. |last4=Kellermann |first4=K. I. |last5=Hook |first5=I. M. |last6=Hawkins |first6=M. R. S. |date=April 2002 |title=The Parkes quarter-Jansky flat-spectrum sample |url=http://dx.doi.org/10.1051/0004-6361:20020119 |journal=Astronomy & Astrophysics |volume=386 |issue=1 |pages=97–113 |doi=10.1051/0004-6361:20020119 |bibcode=2002A&A...386...97J |issn=0004-6361}}</ref>

Revision as of 11:13, 11 June 2024

PKS 1402-012
The quasar PKS 1402-012, seen by DESI Legacy Surveys
Observation data (J2000.0 epoch)
ConstellationVirgo
Right ascension14h 04m 45.895s
Declination-01d 30m 21.947s
Redshift2.518154
Heliocentric radial velocity754,924 km/s
Distance10.732 Gly (light travel time distance)
Apparent magnitude (V)0.149
Apparent magnitude (B)0.197
Surface brightness18.3
Characteristics
TypeOpt.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]

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 classfied 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]

References

  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-06-11.
  2. ^ Wall, J. V.; Jackson, C. A.; Shaver, P. A.; Hook, I. M.; Kellermann, K. I. (2005-04-01). "The Parkes quarter-Jansky flat-spectrum sample. III. Space density and evolution of QSOs". Astronomy and Astrophysics. 434 (1): 133–148. arXiv:astro-ph/0408122. Bibcode:2005A&A...434..133W. doi:10.1051/0004-6361:20041786. ISSN 0004-6361.
  3. ^ Jackson, C. A.; Wall, J. V.; Shaver, P. A.; Kellermann, K. I.; Hook, I. M.; Hawkins, M. R. S. (2002-04-01). "The Parkes quarter-Jansky flat-spectrum sample. I. Sample selection and source identifications". Astronomy and Astrophysics. 386: 97–113. Bibcode:2002A&A...386...97J. doi:10.1051/0004-6361:20020119. ISSN 0004-6361.
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