The Discovery of a Highly Accreting, Radio-loud Quasar at z = 6.82
AffiliationSteward Observatory, University of Arizona
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PublisherIOP Publishing Ltd
CitationBañados, E., Mazzucchelli, C., Momjian, E., Eilers, A. C., Wang, F., Schindler, J. T., ... & Yang, J. (2021). The discovery of a highly accreting, radio-loud quasar at z= 6.82. The Astrophysical Journal, 909(1), 80.
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AbstractRadio sources at the highest redshifts can provide unique information on the first massive galaxies and black holes, the densest primordial environments, and the epoch of reionization. The number of astronomical objects identified at z > 6 has increased dramatically over the last few years, but previously only three radio-loud (R 2500 = f ν,5 GHz/f ν,2500 Å > 10) sources had been reported at z > 6, with the most distant being a quasar at z = 6.18. Here we present the discovery and characterization of PSO J172.3556+18.7734, a radio-loud quasar at z = 6.823. This source has an Mg ii-based black hole mass of ∼3 × 108 M o˙ and is one of the fastest accreting quasars, consistent with super-Eddington accretion. The ionized region around the quasar is among the largest measured at these redshifts, implying an active phase longer than the average lifetime of the z ⪆ 6 quasar population. From archival data, there is evidence that its 1.4 GHz emission has decreased by a factor of two over the last two decades. The quasar's radio spectrum between 1.4 and 3.0 GHz is steep (α = -1.31). Assuming the measured radio slope and extrapolating to rest-frame 5 GHz, the quasar has a radio-loudness parameter R 2500 ∼ 90. A second steep radio source (α = -0.83) of comparable brightness to the quasar is only 23.″1 away (∼120 kpc at z = 6.82; projection probability <2%), but shows no optical or near-infrared counterpart. Further follow-up is required to establish whether these two sources are physically associated. © 2021. The Author(s). Published by the American Astronomical Society..
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Except where otherwise noted, this item's license is described as Copyright © 2021 The Author(s). Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.