期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 502, 期 3, 页码 4154-4169出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab302
关键词
accretion, accretion discs; galaxies: jets; quasars: emission lines; quasars: general; galaxies: star formation; radio continuum: galaxies
资金
- Science and Technology Facilities Council (STFC)
- Herchel Smith Fellowship at Cambridge
- STFC via the Institute of Astronomy, Cambridge, Consolidated Grant
- Royal Society
- European Research Council
- NOVA
- NWO
- CNRS-INSU
- SURF Co-operative
- UK Science and Technology Funding Council
- Julich Supercomputing Centre
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- Brazilian Participation Group
- Carnegie Institution for Science
- Carnegie Mellon University
- Center for Astrophysics \ Harvard Smithsonian
- Chilean Participation Group
- French Participation Group
- Instituto de Astrofisica de Canarias
- The Johns Hopkins University
- Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo
- Korean Participation Group
- Lawrence Berkeley National Laboratory
- Leibniz Institut fur Astrophysik Potsdam (AIP)
- MaxPlanck-Institut fur Astronomie (MPIA Heidelberg)
- Max-PlanckInstitut fur Astrophysik (MPA Garching)
- Max-Planck-Institut fur Extraterrestrische Physik (MPE)
- National Astronomical Observatories of China
- New Mexico State University
- New York University
- University of Notre Dame
- Observatario Nacional/MCTI
- The Ohio StateUniversity
- Pennsylvania State University
- ShanghaiAstronomical Observatory
- United Kingdom Participation Group
- Universidad Nacional Autonoma de Mexico
- University of Arizona
- University of Colorado Boulder
- University of Oxford
- University of Portsmouth
- University of Utah
- University of Virginia
- University of Washington
- University of Wisconsin
- Vanderbilt University
- Yale University
- Center for High Performance Computing at the University of Utah
By investigating the low-frequency radio and ultraviolet properties of a sample of around 10,500 quasars, it was found that the radio detection rate increases with blueshift while the radio-loud fraction decreases. The radio-quiet population shows a range of He II equivalent widths, while the radio-loud population mostly exhibits strong He II. The presence of similar ultraviolet properties but differing radio properties among quasars suggests that radio and ultraviolet emission may be tracing activity occurring on different time-scales.
We present an investigation of the low-frequency radio and ultraviolet properties of a sample of similar or equal to 10 500 quasars from the Sloan Digital Sky Survey Data Release 14, observed as part of the first data release of the Low-Frequency-Array Two-metre Sky Survey. The quasars have redshifts 1.5 < z < 3.5 and luminosities 44.6 < log(10) (L-bol/erg s(-1)) < 47.2. We employ ultraviolet spectral reconstructions based on an independent component analysis to parametrize the CIV.1549-emission line that is used to infer the strength of accretion disc winds, and the He II.1640 line, an indicator of the soft X-ray flux. We find that radio-detected quasars are found in the same region of CIV blueshift versus equivalent-width space as radio-undetected quasars, but that the loudest, most luminous and largest radio sources exist preferentially at low CIV blueshifts. Additionally, the radio-detection fraction increases with blueshift whereas the radio-loud fraction decreases. In the radio-quiet population, we observe a range of He II equivalent widths as well as a Baldwin effect with bolometric luminosity, whilst the radio-loud population has mostly strong He II, consistent with a stronger soft X-ray flux. The presence of strong He II is a necessary but not sufficient condition to detect radio-loud emission suggesting some degree of stochasticity in jet formation. Using energetic arguments and Monte Carlo simulations, we explore the plausibility of winds, compact jets, and star formation as sources of the radio quiet emission, ruling out none. The existence of quasars with similar ultraviolet properties but differing radio properties suggests, perhaps, that the radio and ultraviolet emission is tracing activity occurring on different time-scales.
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