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{{Infobox galaxy|name=] 0528+134|epoch=]|constellation name=]|ra={{RA|05|30|56.4167}}|dec={{DEC|+13|31|55.150}}|z=2.060000|h_radial_v=617,573 ]|dist_ly=10.135 ]|appmag_v=20.00|type=LPQ, FSRQ; HPQ, Blazar|names=2E 1289, INTREF 250, ] 2824388, TXS 0528+134, OHIO G 147, 1Jy 0528+134, NAIC 0528+134, ] J0530+13|image=File:PKS 0528+134 PanSTARRS i.r.g.jpg|caption=The blazar PKS 0528+134.}} {{Infobox galaxy|name=] 0528+134|epoch=]|constellation name=]|ra={{RA|05|30|56.4167}}|dec={{DEC|+13|31|55.150}}|z=2.060000|h_radial_v=617,573 ]|dist_ly=10.135 ]|appmag_v=20.00|type=LPQ, FSRQ; HPQ, Blazar|names=2E 1289, INTREF 250, ] 2824388, TXS 0528+134, OHIO G 147, 1Jy 0528+134, NAIC 0528+134, ] J0530+13|image=File:PKS 0528+134 PanSTARRS i.r.g.jpg|caption=The blazar PKS 0528+134.}}


'''PKS 0528+134''' is a distant ] located in the ] towards the ] of ].<ref>{{Cite journal |last=Mukherjee |first=R. |last2=Bottcher |first2=M. |last3=Hartman |first3=R. C. |last4=Sreekumar |first4=P. |last5=Thompson |first5=D. J. |last6=Mahoney |first6=W. A. |last7=Pursimo |first7=T. |last8=Sillanpaa |first8=A. |last9=Takalo |first9=L. O. |date=1999-12-10 |title=Broadband Spectral Analysis of PKS 0528+134: A Report on Six Years of EGRET Observations |url=https://doi.org/10.1086/308057 |journal=The Astrophysical Journal |volume=527 |issue=1 |pages=132–142 |doi=10.1086/308057 |issn=0004-637X}}</ref><ref>{{Citation |last=Ghisellini |first=G. |title=The blazar PKS 0528+134: new results from BeppoSAX observations |date=1999-06-09 |url=https://arxiv.org/abs/astro-ph/9906165 |access-date=2024-12-21 |doi=10.48550/arXiv.astro-ph/9906165 |last2=Costamante |first2=L. |last3=Tagliaferri |first3=G. |last4=Maraschi |first4=L. |last5=Celotti |first5=A. |last6=Fossati |first6=G. |last7=Pian |first7=E. |last8=Comastri |first8=A. |last9=Francesco |first9=G. De}}</ref> This is a compact radio ], classified as radio-loud with a ] of (z) 2.07<ref>{{Cite journal |last=Sambruna |first=Rita M. |last2=Urry |first2=C. Megan |last3=Maraschi |first3=L. |last4=Ghisellini |first4=G. |last5=Mukherjee |first5=R. |last6=Pesce |first6=Joseph E. |last7=Wagner |first7=S. J. |last8=Wehrle |first8=A. E. |last9=Hartman |first9=R. C. |last10=Lin |first10=Y. C. |last11=von Montigny |first11=C. |date=1997-01-10 |title=The High‐Energy Continuum Emission of the Gamma‐Ray Blazar PKS 0528+134 |url=https://iopscience.iop.org/article/10.1086/303493/fulltext/ |journal=The Astrophysical Journal |volume=474 |issue=2 |pages=639–649 |doi=10.1086/303493 |issn=0004-637X}}</ref> yet having low ].<ref>{{Cite journal |last=Tornikoski |first=M. |last2=Jussila |first2=I. |last3=Johansson |first3=P. |last4=Lainela |first4=M. |last5=Valtaoja |first5=E. |date=2001-03 |title=Radio Spectra and Variability of Gigahertz-Peaked Spectrum Radio Sources and Candidates |url=https://iopscience.iop.org/article/10.1086/319417/fulltext/ |journal=The Astronomical Journal |volume=121 |issue=3 |pages=1306–1318 |doi=10.1086/319417 |issn=0004-6256}}</ref> It was first discovered in 1977 by ]<ref>{{Cite journal |last=Condon |first=J. J. |last2=Hicks |first2=P. D. |last3=Jauncey |first3=D. L. |date=1977-09 |title=Optical identifications of Parkes sources with flat spectra. |url=https://ui.adsabs.harvard.edu/abs/1977AJ.....82..692C/abstract |journal=The Astronomical Journal |language=en |volume=82 |pages=692–700 |doi=10.1086/112109 |issn=0004-6256}}</ref> as a ] and contains a ] that appears as flat making it a flat-spectrum radio quasar.<ref>{{Cite journal |last=Mukherjee |first=R. |date=2000 |title=Spectral variability in the blazar PKS 0528+134 |url=https://doi.org/10.1063/1.1291344 |journal=AIP Conference Proceedings |publisher=AIP |volume=515 |pages=66–70 |doi=10.1063/1.1291344}}</ref><ref>{{Cite journal |last=Bottcher |first=M. |last2=Collmar |first2=W. |date=1998 |title=Spectral variability in PKS 0528+134 at gamma-ray energies |url=https://adsabs.harvard.edu/full/1998A%26A...329L..57B |journal=Astronomy & Astrophysics |volume=329 |pages=57-60 |bibcode=1998A&A...329L..57B}}</ref><ref>{{Cite journal |last=Ghosh |first=K.K. |last2=Ramsey |first2=B.D. |last3=Sadun |first3=A.C. |last4=Soundararajaperumal |first4=S. |date=1999 |title=Optical Variability of Blazars |url=https://iopscience.iop.org/article/10.1086/313313/fulltext/ |journal=The Astrophysical Journal Supplement Series |volume=127 |pages=11-26}}</ref> It has an optical ] of 19.5.<ref>{{Cite journal |last=Mukherjee |first=R. |last2=Bottcher |first2=M. |last3=Hartman |first3=R. C. |last4=Sreekumar |first4=P. |last5=Thompson |first5=D. J. |last6=Mahoney |first6=W. A. |last7=Pursimo |first7=T. |last8=Sillanpaa |first8=A. |last9=Takalo |first9=L. O. |date=1999-12-10 |title=Broadband Spectral Analysis of PKS 0528+134: A Report on Six Years of EGRET Observations |url=https://doi.org/10.1086/308057 |journal=The Astrophysical Journal |volume=527 |issue=1 |pages=132–142 |doi=10.1086/308057 |issn=0004-637X}}</ref> '''PKS 0528+134''' is a distant ] located in the ] towards the ] of ].<ref>{{Cite journal |last1=Mukherjee |first1=R. |last2=Bottcher |first2=M. |last3=Hartman |first3=R. C. |last4=Sreekumar |first4=P. |last5=Thompson |first5=D. J. |last6=Mahoney |first6=W. A. |last7=Pursimo |first7=T. |last8=Sillanpaa |first8=A. |last9=Takalo |first9=L. O. |date=1999-12-10 |title=Broadband Spectral Analysis of PKS 0528+134: A Report on Six Years of EGRET Observations |url=https://doi.org/10.1086/308057 |journal=The Astrophysical Journal |volume=527 |issue=1 |pages=132–142 |doi=10.1086/308057 |issn=0004-637X}}</ref><ref>{{Citation |last1=Ghisellini |first1=G. |title=The blazar PKS 0528+134: new results from BeppoSAX observations |date=1999-06-09 |last2=Costamante |first2=L. |last3=Tagliaferri |first3=G. |last4=Maraschi |first4=L. |last5=Celotti |first5=A. |last6=Fossati |first6=G. |last7=Pian |first7=E. |last8=Comastri |first8=A. |last9=Francesco |first9=G. De|arxiv=astro-ph/9906165 }}</ref> This is a compact radio ], classified as radio-loud with a ] of (z) 2.07<ref>{{Cite journal |last1=Sambruna |first1=Rita M. |last2=Urry |first2=C. Megan |last3=Maraschi |first3=L. |last4=Ghisellini |first4=G. |last5=Mukherjee |first5=R. |last6=Pesce |first6=Joseph E. |last7=Wagner |first7=S. J. |last8=Wehrle |first8=A. E. |last9=Hartman |first9=R. C. |last10=Lin |first10=Y. C. |last11=von Montigny |first11=C. |date=1997-01-10 |title=The High-Energy Continuum Emission of the Gamma-Ray Blazar PKS 0528+134 |url=https://iopscience.iop.org/article/10.1086/303493/fulltext/ |journal=The Astrophysical Journal |volume=474 |issue=2 |pages=639–649 |doi=10.1086/303493 |issn=0004-637X}}</ref> yet having low ].<ref>{{Cite journal |last1=Tornikoski |first1=M. |last2=Jussila |first2=I. |last3=Johansson |first3=P. |last4=Lainela |first4=M. |last5=Valtaoja |first5=E. |date=March 2001 |title=Radio Spectra and Variability of Gigahertz-Peaked Spectrum Radio Sources and Candidates |url=https://iopscience.iop.org/article/10.1086/319417/fulltext/ |journal=The Astronomical Journal |volume=121 |issue=3 |pages=1306–1318 |doi=10.1086/319417 |issn=0004-6256}}</ref> It was first discovered in 1977 by ]<ref>{{Cite journal |last1=Condon |first1=J. J. |last2=Hicks |first2=P. D. |last3=Jauncey |first3=D. L. |date=September 1977 |title=Optical identifications of Parkes sources with flat spectra. |url=https://ui.adsabs.harvard.edu/abs/1977AJ.....82..692C/abstract |journal=The Astronomical Journal |language=en |volume=82 |pages=692–700 |doi=10.1086/112109 |bibcode=1977AJ.....82..692C |issn=0004-6256}}</ref> as a ] and contains a ] that appears as flat making it a flat-spectrum radio quasar.<ref>{{Cite journal |last=Mukherjee |first=R. |date=2000 |title=Spectral variability in the blazar PKS 0528+134 |url=https://doi.org/10.1063/1.1291344 |journal=AIP Conference Proceedings |publisher=AIP |volume=515 |pages=66–70 |doi=10.1063/1.1291344}}</ref><ref>{{Cite journal |last1=Bottcher |first1=M. |last2=Collmar |first2=W. |date=1998 |title=Spectral variability in PKS 0528+134 at gamma-ray energies |url=https://adsabs.harvard.edu/full/1998A%26A...329L..57B |journal=Astronomy & Astrophysics |volume=329 |pages=57–60 |arxiv=astro-ph/9711032 |bibcode=1998A&A...329L..57B}}</ref><ref>{{Cite journal |last1=Ghosh |first1=K.K. |last2=Ramsey |first2=B.D. |last3=Sadun |first3=A.C. |last4=Soundararajaperumal |first4=S. |date=1999 |title=Optical Variability of Blazars |url=https://iopscience.iop.org/article/10.1086/313313/fulltext/ |journal=The Astrophysical Journal Supplement Series |volume=127 |pages=11–26|doi=10.1086/313313 }}</ref> It has an optical ] of 19.5.<ref>{{Cite journal |last1=Mukherjee |first1=R. |last2=Bottcher |first2=M. |last3=Hartman |first3=R. C. |last4=Sreekumar |first4=P. |last5=Thompson |first5=D. J. |last6=Mahoney |first6=W. A. |last7=Pursimo |first7=T. |last8=Sillanpaa |first8=A. |last9=Takalo |first9=L. O. |date=1999-12-10 |title=Broadband Spectral Analysis of PKS 0528+134: A Report on Six Years of EGRET Observations |url=https://doi.org/10.1086/308057 |journal=The Astrophysical Journal |volume=527 |issue=1 |pages=132–142 |doi=10.1086/308057 |issn=0004-637X}}</ref>


== Description == == Description ==
PKS 0528+134 is found variable on the ] and a source of high energy ].<ref>{{Cite journal |last=Hunter |first=S. D. |last2=Bertsch |first2=D. L. |last3=Fichtel |first3=C. E. |last4=Hartman |first4=R. C. |last5=Thompson |first5=D. J. |last6=Kanbach |first6=G. |last7=Mayer-Hasselwander |first7=H. A. |last8=Montigny |first8=C. V. |last9=Pinkau |first9=K. |last10=Rothermel |first10=H. |last11=Sommer |first11=M. |last12=Lin |first12=Y. C. |last13=Michelson |first13=P. F. |last14=Nolan |first14=P. L. |last15=Kniffen |first15=D. A. |date=1992-05 |title=Detection of High Energy Gamma Rays From Quasars PKS0528+134, 4C38.41 and 0836+710 |url=https://ui.adsabs.harvard.edu/abs/1992AAS...180.1005H/abstract |journal=American Astronomical Society Meeting Abstracts #180 |language=en |volume=180 |pages=10.05}}</ref> It showed long-term variability on time scales at high ]. Between 1981 and 1982, PKS 0528+134 exhibited a drop in its 4.8, 8.0 and 14.5 ] flux value by about 4-5 ] (Jy), with a lowest recorded flux of 1.5 Jy in 1990. A drastic increase in ] emission was detected in PKS 0528+134 beginning 1991.<ref>{{Cite journal |last=Hunter |first=S.D. |last2=Bertsch |first2=D.L. |last3=Dingus |first3=B.L. |last4=Fichtel |first4=C.E. |last5=Hartman |first5=R.C. |last6=Kanbach |first6=G. |date=1993 |title=Detection of high-energy gamma rays from quasar PKS 0528 + 134 by EGRET on the Compton Gamma Ray Observatory |url=https://adsabs.harvard.edu/full/1993ApJ...409..134H |journal=Astrophysical Journal |volume=409 |issue=1 |pages=134-138 |bibcode=1993ApJ...409..134H |issn=0004-637X}}</ref> That same year, it showed a nonthermal outburst suggesting a period of relativistic ] being ejected.<ref name=":0">{{Cite journal |last=Zhang |first=Y.F. |last2=Marscher |first2=A.P. |last3=Aller |first3=H.D. |last4=Aller |first4=M.F. |last5=Terasranta |first5=H. |last6=Valtaoja |first6=E. |date=1994 |title=Radio and X-ray observations of the gamma-ray bright quasar PKS 0528+134 |url=https://articles.adsabs.harvard.edu//full/1994ApJ...432...91Z/0000094.000.html |journal=Astrophysical Journal |volume=432 |issue=1 |pages=91-102 |issn=0004-637X}}</ref> PKS 0528+134 also had two radio ] outbursts.<ref>{{Cite journal |last=Qian |first=Shan-jie |last2=Britzen |first2=S. |last3=Witzel |first3=A. |last4=Krichbaum |first4=T. |last5=Kraus |first5=A. |last6=Waltman |first6=E.B. |last7=Valtaoja |first7=E. |last8=Aller |first8=H.D. |date=1998-07 |title=An analysis of the mm-radio outbursts in the gamma-ray source PKS 0528 + 134 |url=https://doi.org/10.1016/s0275-1062(98)00038-1 |journal=Chinese Astronomy and Astrophysics |volume=22 |issue=3 |pages=280–287 |doi=10.1016/s0275-1062(98)00038-1 |issn=0275-1062}}</ref> PKS 0528+134 is found variable on the ] and a source of high energy ].<ref>{{Cite journal |last1=Hunter |first1=S. D. |last2=Bertsch |first2=D. L. |last3=Fichtel |first3=C. E. |last4=Hartman |first4=R. C. |last5=Thompson |first5=D. J. |last6=Kanbach |first6=G. |last7=Mayer-Hasselwander |first7=H. A. |last8=Montigny |first8=C. V. |last9=Pinkau |first9=K. |last10=Rothermel |first10=H. |last11=Sommer |first11=M. |last12=Lin |first12=Y. C. |last13=Michelson |first13=P. F. |last14=Nolan |first14=P. L. |last15=Kniffen |first15=D. A. |date=May 1992 |title=Detection of High Energy Gamma Rays From Quasars PKS0528+134, 4C38.41 and 0836+710 |url=https://ui.adsabs.harvard.edu/abs/1992AAS...180.1005H/abstract |journal=American Astronomical Society Meeting Abstracts #180 |language=en |volume=180 |pages=10.05|bibcode=1992AAS...180.1005H }}</ref> It showed long-term variability on time scales at high ]. Between 1981 and 1982, PKS 0528+134 exhibited a drop in its 4.8, 8.0 and 14.5 ] flux value by about 4-5 ] (Jy), with a lowest recorded flux of 1.5 Jy in 1990. A drastic increase in ] emission was detected in PKS 0528+134 beginning 1991.<ref>{{Cite journal |last1=Hunter |first1=S.D. |last2=Bertsch |first2=D.L. |last3=Dingus |first3=B.L. |last4=Fichtel |first4=C.E. |last5=Hartman |first5=R.C. |last6=Kanbach |first6=G. |date=1993 |title=Detection of high-energy gamma rays from quasar PKS 0528 + 134 by EGRET on the Compton Gamma Ray Observatory |url=https://adsabs.harvard.edu/full/1993ApJ...409..134H |journal=Astrophysical Journal |volume=409 |issue=1 |pages=134–138 |doi=10.1086/172648 |bibcode=1993ApJ...409..134H |issn=0004-637X}}</ref> That same year, it showed a nonthermal outburst suggesting a period of relativistic ] being ejected.<ref name=":0">{{Cite journal |last1=Zhang |first1=Y.F. |last2=Marscher |first2=A.P. |last3=Aller |first3=H.D. |last4=Aller |first4=M.F. |last5=Terasranta |first5=H. |last6=Valtaoja |first6=E. |date=1994 |title=Radio and X-ray observations of the gamma-ray bright quasar PKS 0528+134 |url=https://articles.adsabs.harvard.edu//full/1994ApJ...432...91Z/0000094.000.html |journal=Astrophysical Journal |volume=432 |issue=1 |pages=91–102 |doi=10.1086/174551 |bibcode=1994ApJ...432...91Z |issn=0004-637X}}</ref> PKS 0528+134 also had two radio ] outbursts.<ref>{{Cite journal |last1=Qian |first1=Shan-jie |last2=Britzen |first2=S. |last3=Witzel |first3=A. |last4=Krichbaum |first4=T. |last5=Kraus |first5=A. |last6=Waltman |first6=E.B. |last7=Valtaoja |first7=E. |last8=Aller |first8=H.D. |date=July 1998 |title=An analysis of the mm-radio outbursts in the gamma-ray source PKS 0528 + 134 |url=https://doi.org/10.1016/s0275-1062(98)00038-1 |journal=Chinese Astronomy and Astrophysics |volume=22 |issue=3 |pages=280–287 |doi=10.1016/s0275-1062(98)00038-1 |issn=0275-1062}}</ref>


Between the months of July and December 2009, PKS 0528+134 reached a state of quiescence. When observed by astronomers, they found no traces of either significant flux or spectral variability in most ] although flux variability was discovered in optical regime, followed by a weak pattern of spectral softening. This suggests the ] of PKS 0528+134 might play a role at the optical spectrum's blue end. Optical ] also suggests PKS 0528+134 has an extreme degree of ], indicating possibility of ] providing emission at the optical spectrum's red end.<ref>{{Cite journal |last=Palma |first=N.I. |last2=Böttcher |first2=M. |last3=Calle |first3=I. de la |last4=Agudo |first4=I. |last5=Aller |first5=M. |last6=Aller |first6=H. |last7=Bach |first7=U. |last8=Benítez |first8=E. |last9=Buemi |first9=C.S. |last10=Escande |first10=L. |date=June 2011 |title=MULTIWAVELENGTH OBSERVATIONS OF THE GAMMA-RAY BLAZAR PKS 0528+134 IN QUIESCENCE |url=https://iopscience.iop.org/article/10.1088/0004-637X/735/1/60#apj391430s8 |journal=The Astrophysical Journal |volume=735 |issue=60 |doi=10.1088/0004-637X/735/1/60}}</ref> Between the months of July and December 2009, PKS 0528+134 reached a state of quiescence. When observed by astronomers, they found no traces of either significant flux or spectral variability in most ] although flux variability was discovered in optical regime, followed by a weak pattern of spectral softening. This suggests the ] of PKS 0528+134 might play a role at the optical spectrum's blue end. Optical ] also suggests PKS 0528+134 has an extreme degree of ], indicating possibility of ] providing emission at the optical spectrum's red end.<ref>{{Cite journal |last1=Palma |first1=N.I. |last2=Böttcher |first2=M. |last3=Calle |first3=I. de la |last4=Agudo |first4=I. |last5=Aller |first5=M. |last6=Aller |first6=H. |last7=Bach |first7=U. |last8=Benítez |first8=E. |last9=Buemi |first9=C.S. |last10=Escande |first10=L. |date=June 2011 |title=Multiwavelength Observations of the Gamma-Ray Blazar PKS 0528+134 in Quiescence |url=https://iopscience.iop.org/article/10.1088/0004-637X/735/1/60#apj391430s8 |journal=The Astrophysical Journal |volume=735 |issue=60 |page=60 |doi=10.1088/0004-637X/735/1/60|arxiv=1104.3557 }}</ref>


Radio images made by the ] at 22 GHz shows radio structure of PKS 0528+134 as a 5 mas extended one-sided ] with a more diffused northwest component at a ] of 50° and two other components located in the west direction of various distances.<ref name=":0" /><ref name=":1">{{Cite journal |last=Jorstad |first=Svetlana G. |last2=Marscher |first2=Alan P. |last3=Mattox |first3=John R. |last4=Wehrle |first4=Ann E. |last5=Bloom |first5=Steven D. |last6=Yurchenko |first6=Alexei V. |date=2001-06 |title=Multiepoch Very Long Baseline Array Observations of EGRET‐detected Quasars and BL Lacertae Objects: Superluminal Motion of Gamma‐Ray Bright Blazars |url=https://iopscience.iop.org/article/10.1086/320858/fulltext/ |journal=The Astrophysical Journal Supplement Series |volume=134 |issue=2 |pages=181–240 |doi=10.1086/320858 |issn=0067-0049}}</ref> At 43 GHz, the structure is further resolved into five components showing ] reaching high as 23 h<sup>-1</sup> with increasing motions per distance from the core. An inverted core spectrum is also discovered.<ref name=":1" /> ] finds three of its components shows progressive acceleration with a strongly polarized northern knot feature.<ref>{{Cite journal |last=Jorstad |first=Svetlana G. |last2=Marscher |first2=Alan P. |last3=Lister |first3=Matthew L. |last4=Stirling |first4=Alastair M. |last5=Cawthorne |first5=Timothy V. |last6=Gear |first6=Walter K. |last7=Gómez |first7=José L. |last8=Stevens |first8=Jason A. |last9=Smith |first9=Paul S. |last10=Forster |first10=James R. |last11=Robson |first11=E. Ian |date=2005-10 |title=Polarimetric Observations of 15 Active Galactic Nuclei at High Frequencies: Jet Kinematics from Bimonthly Monitoring with the Very Long Baseline Array |url=https://iopscience.iop.org/article/10.1086/444593/fulltext/ |journal=The Astronomical Journal |volume=130 |issue=4 |pages=1418–1465 |doi=10.1086/444593 |issn=0004-6256}}</ref> A new component is also found at higher frequencies.<ref>{{Cite journal |last=Cai |first=H.-B. |last2=Shen |first2=Z.-Q. |last3=Chen |first3=X. |last4=Shang |first4=L.-L. |date=2006-09-12 |title=Quasi-simultaneous five-frequency VLBA observations of PKS 0528+134 |url=https://www.aanda.org/articles/aa/pdf/2006/42/aa5094-06.pdf |journal=Astronomy &amp; Astrophysics |volume=458 |issue=3 |pages=753–760 |doi=10.1051/0004-6361:20065094 |issn=0004-6361}}</ref> Radio images made by the ] at 22 GHz shows radio structure of PKS 0528+134 as a 5 mas extended one-sided ] with a more diffused northwest component at a ] of 50° and two other components located in the west direction of various distances.<ref name=":0" /><ref name=":1">{{Cite journal |last1=Jorstad |first1=Svetlana G. |last2=Marscher |first2=Alan P. |last3=Mattox |first3=John R. |last4=Wehrle |first4=Ann E. |last5=Bloom |first5=Steven D. |last6=Yurchenko |first6=Alexei V. |date=June 2001 |title=Multiepoch Very Long Baseline Array Observations of EGRET-detected Quasars and BL Lacertae Objects: Superluminal Motion of Gamma-Ray Bright Blazars |url=https://iopscience.iop.org/article/10.1086/320858/fulltext/ |journal=The Astrophysical Journal Supplement Series |volume=134 |issue=2 |pages=181–240 |doi=10.1086/320858 |issn=0067-0049}}</ref> At 43 GHz, the structure is further resolved into five components showing ] reaching high as 23 h<sup>-1</sup> with increasing motions per distance from the core. An inverted core spectrum is also discovered.<ref name=":1" /> ] finds three of its components shows progressive acceleration with a strongly polarized northern knot feature.<ref>{{Cite journal |last1=Jorstad |first1=Svetlana G. |last2=Marscher |first2=Alan P. |last3=Lister |first3=Matthew L. |last4=Stirling |first4=Alastair M. |last5=Cawthorne |first5=Timothy V. |last6=Gear |first6=Walter K. |last7=Gómez |first7=José L. |last8=Stevens |first8=Jason A. |last9=Smith |first9=Paul S. |last10=Forster |first10=James R. |last11=Robson |first11=E. Ian |date=October 2005 |title=Polarimetric Observations of 15 Active Galactic Nuclei at High Frequencies: Jet Kinematics from Bimonthly Monitoring with the Very Long Baseline Array |url=https://iopscience.iop.org/article/10.1086/444593/fulltext/ |journal=The Astronomical Journal |volume=130 |issue=4 |pages=1418–1465 |doi=10.1086/444593 |issn=0004-6256}}</ref> A new component is also found at higher frequencies.<ref>{{Cite journal |last1=Cai |first1=H.-B. |last2=Shen |first2=Z.-Q. |last3=Chen |first3=X. |last4=Shang |first4=L.-L. |date=2006-09-12 |title=Quasi-simultaneous five-frequency VLBA observations of PKS 0528+134 |url=https://www.aanda.org/articles/aa/pdf/2006/42/aa5094-06.pdf |journal=Astronomy & Astrophysics |volume=458 |issue=3 |pages=753–760 |doi=10.1051/0004-6361:20065094 |issn=0004-6361}}</ref>


The ] mass of PKS 0528+134 is estimated to be 85 x 10<sup>8</sup> M<sub>ʘ</sub> based on an equation calculation integrated between the values of 3 and 30 ] via flux measurements made by the Imaging Compton Telescope. A luminosity value of 4.1 x 10<sup>49</sup> ] has also been calculated for the object as well.<ref>{{Cite journal |last=Collmar |first=W. |last2=Bennett |first2=K. |last3=Bloemen |first3=H. |last4=Blom |first4=J.J. |last5=Hermsen |first5=W. |date=1997 |title=COMPTEL observations of the quasar PKS 0528+134 during the first The ] mass of PKS 0528+134 is estimated to be 85 x 10<sup>8</sup> M<sub>ʘ</sub> based on an equation calculation integrated between the values of 3 and 30 ] via flux measurements made by the Imaging Compton Telescope. A luminosity value of 4.1 x 10<sup>49</sup> ] has also been calculated for the object as well.<ref>{{Cite journal |last1=Collmar |first1=W. |last2=Bennett |first2=K. |last3=Bloemen |first3=H. |last4=Blom |first4=J.J. |last5=Hermsen |first5=W. |date=1997 |title=COMPTEL observations of the quasar PKS 0528+134 during the first 3.5 years of the CGRO mission |url=https://adsabs.harvard.edu/full/1997A%26A...328...33C |journal=Astronomy & Astrophysics |volume=328 |pages=33–42|arxiv=astro-ph/9711198 |bibcode=1997A&A...328...33C }}</ref>
3.5 years of the CGRO mission |url=https://adsabs.harvard.edu/full/1997A%26A...328...33C |journal=Astronomy & Astrophysics |volume=328 |pages=33-42}}</ref>


== References == == References ==

Latest revision as of 13:19, 21 December 2024

Blazar in the constellation Orion
PKS 0528+134
The blazar PKS 0528+134.
Observation data (J2000.0 epoch)
ConstellationOrion
Right ascension05 30 56.4167
Declination+13° 31′ 55.150″
Redshift2.060000
Heliocentric radial velocity617,573 km/s
Distance10.135 Gly
Apparent magnitude (V)20.00
Characteristics
TypeLPQ, FSRQ; HPQ, Blazar
Other designations
2E 1289, INTREF 250, LEDA 2824388, TXS 0528+134, OHIO G 147, 1Jy 0528+134, NAIC 0528+134, QSO J0530+13

PKS 0528+134 is a distant blazar located in the Galactic anticenter towards the constellation of Orion. This is a compact radio quasar, classified as radio-loud with a redshift of (z) 2.07 yet having low polarization. It was first discovered in 1977 by astronomers as a radio source and contains a radio spectrum that appears as flat making it a flat-spectrum radio quasar. It has an optical brightness of 19.5.

Description

PKS 0528+134 is found variable on the electromagnetic spectrum and a source of high energy gamma rays. It showed long-term variability on time scales at high radio frequencies. Between 1981 and 1982, PKS 0528+134 exhibited a drop in its 4.8, 8.0 and 14.5 GHz flux value by about 4-5 Jansky (Jy), with a lowest recorded flux of 1.5 Jy in 1990. A drastic increase in gamma ray emission was detected in PKS 0528+134 beginning 1991. That same year, it showed a nonthermal outburst suggesting a period of relativistic plasma being ejected. PKS 0528+134 also had two radio millimeter outbursts.

Between the months of July and December 2009, PKS 0528+134 reached a state of quiescence. When observed by astronomers, they found no traces of either significant flux or spectral variability in most radio bands although flux variability was discovered in optical regime, followed by a weak pattern of spectral softening. This suggests the accretion disk of PKS 0528+134 might play a role at the optical spectrum's blue end. Optical spectropolarimetry also suggests PKS 0528+134 has an extreme degree of polarization, indicating possibility of synchrotron radiation providing emission at the optical spectrum's red end.

Radio images made by the Very Long Baseline Interferometry at 22 GHz shows radio structure of PKS 0528+134 as a 5 mas extended one-sided jet with a more diffused northwest component at a position angle of 50° and two other components located in the west direction of various distances. At 43 GHz, the structure is further resolved into five components showing superluminal motions reaching high as 23 h with increasing motions per distance from the core. An inverted core spectrum is also discovered. Very Long Baseline Array finds three of its components shows progressive acceleration with a strongly polarized northern knot feature. A new component is also found at higher frequencies.

The supermassive black hole mass of PKS 0528+134 is estimated to be 85 x 10 Mʘ based on an equation calculation integrated between the values of 3 and 30 MeV via flux measurements made by the Imaging Compton Telescope. A luminosity value of 4.1 x 10 ergs has also been calculated for the object as well.

References

  1. Mukherjee, R.; Bottcher, M.; Hartman, R. C.; Sreekumar, P.; Thompson, D. J.; Mahoney, W. A.; Pursimo, T.; Sillanpaa, A.; Takalo, L. O. (1999-12-10). "Broadband Spectral Analysis of PKS 0528+134: A Report on Six Years of EGRET Observations". The Astrophysical Journal. 527 (1): 132–142. doi:10.1086/308057. ISSN 0004-637X.
  2. Ghisellini, G.; Costamante, L.; Tagliaferri, G.; Maraschi, L.; Celotti, A.; Fossati, G.; Pian, E.; Comastri, A.; Francesco, G. De (1999-06-09), The blazar PKS 0528+134: new results from BeppoSAX observations, arXiv:astro-ph/9906165
  3. Sambruna, Rita M.; Urry, C. Megan; Maraschi, L.; Ghisellini, G.; Mukherjee, R.; Pesce, Joseph E.; Wagner, S. J.; Wehrle, A. E.; Hartman, R. C.; Lin, Y. C.; von Montigny, C. (1997-01-10). "The High-Energy Continuum Emission of the Gamma-Ray Blazar PKS 0528+134". The Astrophysical Journal. 474 (2): 639–649. doi:10.1086/303493. ISSN 0004-637X.
  4. Tornikoski, M.; Jussila, I.; Johansson, P.; Lainela, M.; Valtaoja, E. (March 2001). "Radio Spectra and Variability of Gigahertz-Peaked Spectrum Radio Sources and Candidates". The Astronomical Journal. 121 (3): 1306–1318. doi:10.1086/319417. ISSN 0004-6256.
  5. Condon, J. J.; Hicks, P. D.; Jauncey, D. L. (September 1977). "Optical identifications of Parkes sources with flat spectra". The Astronomical Journal. 82: 692–700. Bibcode:1977AJ.....82..692C. doi:10.1086/112109. ISSN 0004-6256.
  6. Mukherjee, R. (2000). "Spectral variability in the blazar PKS 0528+134". AIP Conference Proceedings. 515. AIP: 66–70. doi:10.1063/1.1291344.
  7. Bottcher, M.; Collmar, W. (1998). "Spectral variability in PKS 0528+134 at gamma-ray energies". Astronomy & Astrophysics. 329: 57–60. arXiv:astro-ph/9711032. Bibcode:1998A&A...329L..57B.
  8. Ghosh, K.K.; Ramsey, B.D.; Sadun, A.C.; Soundararajaperumal, S. (1999). "Optical Variability of Blazars". The Astrophysical Journal Supplement Series. 127: 11–26. doi:10.1086/313313.
  9. Mukherjee, R.; Bottcher, M.; Hartman, R. C.; Sreekumar, P.; Thompson, D. J.; Mahoney, W. A.; Pursimo, T.; Sillanpaa, A.; Takalo, L. O. (1999-12-10). "Broadband Spectral Analysis of PKS 0528+134: A Report on Six Years of EGRET Observations". The Astrophysical Journal. 527 (1): 132–142. doi:10.1086/308057. ISSN 0004-637X.
  10. Hunter, S. D.; Bertsch, D. L.; Fichtel, C. E.; Hartman, R. C.; Thompson, D. J.; Kanbach, G.; Mayer-Hasselwander, H. A.; Montigny, C. V.; Pinkau, K.; Rothermel, H.; Sommer, M.; Lin, Y. C.; Michelson, P. F.; Nolan, P. L.; Kniffen, D. A. (May 1992). "Detection of High Energy Gamma Rays From Quasars PKS0528+134, 4C38.41 and 0836+710". American Astronomical Society Meeting Abstracts #180. 180: 10.05. Bibcode:1992AAS...180.1005H.
  11. Hunter, S.D.; Bertsch, D.L.; Dingus, B.L.; Fichtel, C.E.; Hartman, R.C.; Kanbach, G. (1993). "Detection of high-energy gamma rays from quasar PKS 0528 + 134 by EGRET on the Compton Gamma Ray Observatory". Astrophysical Journal. 409 (1): 134–138. Bibcode:1993ApJ...409..134H. doi:10.1086/172648. ISSN 0004-637X.
  12. ^ Zhang, Y.F.; Marscher, A.P.; Aller, H.D.; Aller, M.F.; Terasranta, H.; Valtaoja, E. (1994). "Radio and X-ray observations of the gamma-ray bright quasar PKS 0528+134". Astrophysical Journal. 432 (1): 91–102. Bibcode:1994ApJ...432...91Z. doi:10.1086/174551. ISSN 0004-637X.
  13. Qian, Shan-jie; Britzen, S.; Witzel, A.; Krichbaum, T.; Kraus, A.; Waltman, E.B.; Valtaoja, E.; Aller, H.D. (July 1998). "An analysis of the mm-radio outbursts in the gamma-ray source PKS 0528 + 134". Chinese Astronomy and Astrophysics. 22 (3): 280–287. doi:10.1016/s0275-1062(98)00038-1. ISSN 0275-1062.
  14. Palma, N.I.; Böttcher, M.; Calle, I. de la; Agudo, I.; Aller, M.; Aller, H.; Bach, U.; Benítez, E.; Buemi, C.S.; Escande, L. (June 2011). "Multiwavelength Observations of the Gamma-Ray Blazar PKS 0528+134 in Quiescence". The Astrophysical Journal. 735 (60): 60. arXiv:1104.3557. doi:10.1088/0004-637X/735/1/60.
  15. ^ Jorstad, Svetlana G.; Marscher, Alan P.; Mattox, John R.; Wehrle, Ann E.; Bloom, Steven D.; Yurchenko, Alexei V. (June 2001). "Multiepoch Very Long Baseline Array Observations of EGRET-detected Quasars and BL Lacertae Objects: Superluminal Motion of Gamma-Ray Bright Blazars". The Astrophysical Journal Supplement Series. 134 (2): 181–240. doi:10.1086/320858. ISSN 0067-0049.
  16. Jorstad, Svetlana G.; Marscher, Alan P.; Lister, Matthew L.; Stirling, Alastair M.; Cawthorne, Timothy V.; Gear, Walter K.; Gómez, José L.; Stevens, Jason A.; Smith, Paul S.; Forster, James R.; Robson, E. Ian (October 2005). "Polarimetric Observations of 15 Active Galactic Nuclei at High Frequencies: Jet Kinematics from Bimonthly Monitoring with the Very Long Baseline Array". The Astronomical Journal. 130 (4): 1418–1465. doi:10.1086/444593. ISSN 0004-6256.
  17. Cai, H.-B.; Shen, Z.-Q.; Chen, X.; Shang, L.-L. (2006-09-12). "Quasi-simultaneous five-frequency VLBA observations of PKS 0528+134" (PDF). Astronomy & Astrophysics. 458 (3): 753–760. doi:10.1051/0004-6361:20065094. ISSN 0004-6361.
  18. Collmar, W.; Bennett, K.; Bloemen, H.; Blom, J.J.; Hermsen, W. (1997). "COMPTEL observations of the quasar PKS 0528+134 during the first 3.5 years of the CGRO mission". Astronomy & Astrophysics. 328: 33–42. arXiv:astro-ph/9711198. Bibcode:1997A&A...328...33C.

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