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Winds as the origin of radio emission in z=2.5 radio-quiet extremely red quasars

Author(s): Hwang, Hsiang-Chih; Zakamska, Nadia L; Alexandroff, Rachael M; Hamann, Fred; Greene, Jenny E.; et al

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dc.contributor.authorHwang, Hsiang-Chih-
dc.contributor.authorZakamska, Nadia L-
dc.contributor.authorAlexandroff, Rachael M-
dc.contributor.authorHamann, Fred-
dc.contributor.authorGreene, Jenny E.-
dc.contributor.authorPerrotta, Serena-
dc.contributor.authorRichards, Gordon T-
dc.date.accessioned2019-08-29T17:04:29Z-
dc.date.available2019-08-29T17:04:29Z-
dc.date.issued2018-06en_US
dc.identifier.citationHwang, Hsiang-Chih, Zakamska, Nadia L, Alexandroff, Rachael M, Hamann, Fred, Greene, Jenny E, Perrotta, Serena, Richards, Gordon T. (2018). Winds as the origin of radio emission in z=2.5 radio-quiet extremely red quasars. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 477 (830 - 844. doi:10.1093/mnras/sty742en_US
dc.identifier.issn0035-8711-
dc.identifier.urihttp://arks.princeton.edu/ark:/88435/pr1b15m-
dc.description.abstractMost active galactic nuclei (AGNs) are radio quiet, and the origin of their radio emission is not well understood. One hypothesis is that this radio emission is a byproduct of quasar driven winds. In this paper, we present the radio properties of 108 extremely red quasars (ERQs) at z = 2-4. ERQs are among the most luminous quasars (L-bol similar to 10(47-48) erg s(-1)) in the Universe, with signatures of extreme (>> 1000 km s(-1)) outflows in their [O III]lambda 5007 angstrom emission, making them the best subjects to seek the connection between radio and outflow activities. All ERQs but one are unresolved in the radio on similar to 10 kpc scales, and the median radio luminosity of ERQs is nu L-nu[6 GHz] = 10(41.0) erg s(-1), in the radio-quiet regime, but 1-2 orders of magnitude higher than that of other quasar samples. The radio spectra are steep, with a mean spectral index <alpha > = -1.0. In addition, ERQs neatly follow the extrapolation of the low-redshift correlation between radio luminosity and the velocity dispersion of [O III] emitting ionized gas. Uncollimated winds, with a power of one per cent of the bolometric luminosity, can account for all these observations. Such winds would interact with and shock the gas around the quasar and in the host galaxy, resulting in acceleration of relativistic particles and the consequent synchrotron emission observed in the radio. Our observations support the picture in which ERQs are signposts of extremely powerful episodes of quasar feedback, and quasar-driven winds as a contributor of the radio emission in the intermediate regime of radio luminosity nu L-nu = 10(39)-10(42) erg s(-1).en_US
dc.format.extent830 - 844en_US
dc.language.isoen_USen_US
dc.relationhttp://simbad.u-strasbg.fr/simbad/sim-ref?querymethod=bib&simbo=on&submit=submit+bibcode&bibcode=2018MNRAS.477..830Hen_US
dc.relationhttps://ned.ipac.caltech.edu/cgi-bin/objsearch?search_type=Search&refcode=2018MNRAS.477..830Hen_US
dc.relation.ispartofMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETYen_US
dc.rightsFinal published version. Article is made available in OAR by the publisher's permission or policy.en_US
dc.titleWinds as the origin of radio emission in z=2.5 radio-quiet extremely red quasarsen_US
dc.typeJournal Articleen_US
dc.identifier.doidoi:10.1093/mnras/sty742-
dc.date.eissued2018-03-23en_US
dc.identifier.eissn1365-2966-
pu.type.symplectichttp://www.symplectic.co.uk/publications/atom-terms/1.0/journal-articleen_US

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