PMN J1616+0459, OS +023,IRCF J161637.5+045932,RX J1616.6+0459,FIRST J61637.5+045932,NVSS J161637+045933, TXS 1614+051[1]
PKS 1614+051 is a distantquasar located in theconstellation ofHercules. Theredshift for this object is (z) 3.21[2][1] and it was first identified byastronomers in 1983.[3] It is classified as a radio-loud quasar[4][5] and contains aradio spectrum that appears as flat.[6] It is also referred as a high frequency peaker and agigahertz peaked-spectrum source, making it one of the most powerful sources known.[7][8]
PKS 1614+051 is variable on theelectromagnetic spectrum. When shown on a multi-wavelengthlight curve, the object displaysflux density variations usually slow, with one flaring period which was detected at 5–22 GHzfrequencies and started towards the end of 2009. At 37 GHz, PKS 1614+051 showed aflare in January 2014 and several faint localized flares detected in 2009, 2020 and 2022. Observations also showed it has a low variability level of 0.02 and a short variability time of 12 days.[6]
The structure of PKS 1614+051 is compact. When detected inradio imaging, the source is found to have double morphology, consisting of an invertedspectrum radio core and a secondary component which is located 0.8arcseconds away from it at aposition angle of -30°.[9]Very Long Baseline Interferometry (VLBI) observations conducted in 1992, found an elongated beam in the structure, orientated at -11°. This suggests the structure might be aligned together with its arc-scale structure.[10] When imaged byVery Long Baseline Array (VLBA) at 8.4 GHz, the source shows a bright north component and a slightly resolved structure located south-west.[11]Polarization was also detected in several components inside the core region.[12]
TwoFaraday components were detected in PKS 1614+051 withrotation measures (RM) of 2100 rad m−2 and 500 rad m−2. These suggested two reasons; either they are associated with two foreground layers (depolarization by RM gradients or through external beamdepolarization) or by two inner layers which emit radiation and rotate at same time intervals, via twosynchrotron components present in the quasar's radio spectrum.[13]
Ground-based observations suggested the galaxy might beinteracting with PKS 1614+051.[16] A detection of a 50 kiloparsecLyman-alpha gas bridge between it and the quasar by Multi-Object Spectroscopic Explorer (MUSE) would later confirm this theory. Evidence also points out that the gas is extending towards two other companion galaxies, suggesting the interaction is not affecting only the main companion galaxy.[17]
^abSotnikova, Yu V.; Mikhailov, A. G.; Volvach, A. E.; Kudryavtsev, D. O.; Mufakharov, T. V.; Vlasyuk, V. V.; Khabibullina, M. L.; Kudryashova, A. A.; Mingaliev, M. G.; Erkenov, A. K.; Kovalev, Yu A.; Kovalev, Y. Y.; Kharinov, M. A.; Semenova, T. A.; Udovitskiy, R. Yu (December 2024). "Radio and Optical Properties of the Blazar PKS 1614+051 at z=3.21".Astrophysical Bulletin.79 (4):548–572.arXiv:2501.12694.doi:10.1134/S199034132460087X.
^Sotnikova, Yu; Mikhailov, A.; Mufakharov, T.; An, T.; Kudryavtsev, D.; Mingaliev, M.; Udovitskiy, R.; Kudryashova, A.; Stolyarov, V. (2024-06-03), "High-Redshift Quasars at z ≥ 3: Radio Variability and MPS/GPS Candidates",Galaxies,12 (3): 25,arXiv:2406.01458,Bibcode:2024Galax..12...25S,doi:10.3390/galaxies12030025
