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| PKS 0528+134 | |
|---|---|
| Name | PKS 0528+134 |
| Type | blazar |
| Ra | 05h 30m 56.40s |
| Dec | +13° 31′ 55.0″ |
| Redshift | 2.07 |
| Constellation | Orion |
| Other names | B0526+138, 4C +13.41 |
PKS 0528+134 is a high-redshift, flat-spectrum radio quasar classified as a blazar, notable for strong variability and bright gamma-ray emission. It has been the subject of long-term monitoring by multiple observatories and missions, and it figures in studies of active galactic nuclei, relativistic jets, and cosmological evolution. The object is situated toward Orion and has played a role in calibrating multiwavelength campaigns involving radio, optical, X-ray, and gamma-ray facilities.
The source appears in radio catalogs alongside objects like 3C 273, BL Lacertae, 3C 279, and PKS 0537-441 and has been compared with quasars studied by Sloan Digital Sky Survey, Very Large Array, and Hubble Space Telescope teams. Studies often reference surveys and facilities including Fermi Gamma-ray Space Telescope, EGRET, Very Long Baseline Array, Chandra X-ray Observatory, and ROSAT. Authors who have modeled its spectral energy distribution cite theoretical frameworks advanced by researchers affiliated with Harvard-Smithsonian Center for Astrophysics, Max Planck Institute for Radio Astronomy, CERN, NASA, and European Space Agency.
Initial radio detections placed the source in early surveys alongside entries from Third Cambridge Catalogue of Radio Sources, Bonn Survey, and Green Bank Telescope catalogs, with subsequent optical identification referencing standards used by Palomar Observatory and spectroscopic follow-up at facilities like Keck Observatory and Kitt Peak National Observatory. Radio interferometry with arrays such as MERLIN and European VLBI Network refined positions used by optical spectroscopists from institutions including Institute of Astronomy, Cambridge, Caltech, and Jet Propulsion Laboratory. Cross-matching procedures involved databases maintained by NASA/IPAC Extragalactic Database and classification frameworks developed by teams at National Radio Astronomy Observatory.
The redshift determination relied on spectroscopy methods similar to those applied to 3C 286, PKS 1222+216, and TXS 0506+056, using emission-line identifications and cosmological parameters associated with measurements by Planck Collaboration, Wilkinson Microwave Anisotropy Probe, and distance ladders calibrated by Hubble Space Telescope observations. The commonly cited redshift value places the object at cosmological distances relevant to studies invoking parameters from Lambda-CDM model interpretations by researchers at University of Cambridge and Princeton University. Distance estimates are used in luminosity comparisons with samples compiled by Fermi LAT collaboration, Swift Observatory teams, and legacy surveys like 2MASS.
Multiwavelength campaigns have coordinated instruments such as Fermi Gamma-ray Space Telescope, AGILE, BeppoSAX, XMM-Newton, Chandra X-ray Observatory, Hubble Space Telescope, Spitzer Space Telescope, Subaru Telescope, ALMA, SMA, and radio arrays including Very Long Baseline Array, Very Large Array, and European VLBI Network. Results are compared with spectral templates developed by researchers at University of Chicago, Columbia University, Max Planck Institute for Astrophysics, and studies published in journals like The Astrophysical Journal and Monthly Notices of the Royal Astronomical Society. Multi-epoch photometry and spectroscopy link variability patterns to models proposed by teams at University of California, Berkeley, University of Oxford, and Instituto de Astrofísica de Canarias.
High-resolution imaging reveals core-jet morphology analogous to structures in sources like 3C 273, M87, and Cen A, with parsec-scale components mapped by Very Long Baseline Array and proper motions interpreted in the context of relativistic beaming theories advanced by scientists at Princeton University, Stanford University, and California Institute of Technology. Polarization studies reference methods developed at Rutherford Appleton Laboratory and Max Planck Institute for Radio Astronomy and compare magnetic field alignments to those observed in BL Lacertae objects and bright quasars from the MOJAVE program. Morphological classifications draw on frameworks used by the Fanaroff–Riley classification tradition and jet simulations from groups at NASA Ames Research Center and Los Alamos National Laboratory.
The source exhibits variability across radio, optical, X-ray, and gamma-ray bands, paralleling behavior seen in 3C 279, PKS 1510-089, and OJ 287. Flaring episodes monitored by Fermi LAT, EGRET, and AGILE have been analyzed alongside contemporaneous X-ray data from Swift and Chandra, with theoretical interpretations referencing particle acceleration models developed at CERN, Max Planck Institute for Astrophysics, and Lawrence Berkeley National Laboratory. Correlations between bands are evaluated using statistical techniques common to teams at University College London, University of Arizona, and Leiden University.
Imaging constraints from Hubble Space Telescope and adaptive optics on Keck Observatory inform limits on host morphology, comparing environments to studies of host galaxies in samples by Sloan Digital Sky Survey, COSMOS survey, and CANDELS. The source environment is discussed in the context of large-scale structure maps by 2dF Galaxy Redshift Survey and SDSS teams, and galaxy evolution models from Max Planck Institute for Astronomy and Institute of Astronomy, Cambridge are used to interpret host properties and potential interactions with neighboring systems cataloged by NASA Extragalactic Database.