Disentangling the AGN and star-formation contributions to the radio-X-ray emission of radio-loud quasars at 1<z<2

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dc.contributor.authorAzadi, Mojegan
dc.contributor.authorWilkes, Belinda
dc.contributor.authorKuraszkiewicz, Joanna
dc.contributor.authorMcDowell, Jonathan
dc.contributor.authorSiebenmorgen, Ralf
dc.contributor.authorAshby, Matthew
dc.contributor.authorBirkinshaw, Mark
dc.contributor.authorWorrall, Diana
dc.contributor.authorAbrams, Natasha
dc.contributor.authorBarthel, Peter
dc.contributor.authorFazio, Giovanni
dc.contributor.authorHaas, Martin
dc.contributor.authorHyman, Sóley
dc.contributor.authorMartínez-Galarza, Rafael
dc.contributor.authorMeyer, Eileen
dc.date.accessioned2021-03-30T16:50:15Z
dc.date.available2021-03-30T16:50:15Z
dc.date.issued2020-11-11
dc.description.abstractTo constrain the emission mechanisms responsible for generating the energy powering the active galactic nuclei (AGN) and their host galaxies, it is essential to disentangle the contributions from both as a function of wavelength. Here we introduce a state-of-the-art AGN radio-to-X-ray spectral energy distribution fitting model (ARXSED). ARXSED uses multiple components to replicate the emission from the AGN and their hosts. At radio wavelengths, ARXSED accounts for radiation from the radio structures (e.g., lobes,jets). At near-infrared to far-infrared wavelengths, ARXSED combines a clumpy medium and a homogeneous disk to account for the radiation from the torus. At the optical-UV and X-ray, ARXSED accounts for the emission from the accretion disk. An underlying component from radio to UV wavelengths accounts for the emission from the host galaxy. Here we present the results of ARXSED fits to the panchromatic SEDs of 20 radio-loud quasars from the 3CRR sample at 1<z≲2. We find that a single power-law is unable to fit the radio emission when compact radio structures (core, hot spots) are present. We find that the non-thermal emission from the quasars' radio structures contributes significantly (>70%) to the submm luminosity in half the sample, impacting the submm-based star formation rate estimates. We present the median intrinsic SED of the radio-loud quasars at z>1 and find that the median SED of \cite{Elvis1994} is unable to describe the SED of the radio-selected AGN at z>1. The AGN torus and accretion disk parameters inferred from our fitting technique agree with those in the literature for similar samples. We find that the orientation of the torus/accretion disk does not line up with the inclination of the radio jets in our sample.en_US
dc.description.sponsorshipSupport for this work was provided by the National Aeronautics and Space Administration and the Chandra X-ray Center (CXC), which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060 (BJW, MAz,JK). The scientific results in this article are based to a significant degree on observations made by the Chandra X-ray Observatory (CXO). This research has made use of data obtained from the Chandra Data Archive. This research has made use of data provided by the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. and data from the Sloan Digital Sky Survey (SDSS). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. This research is based on observations made by Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We acknowledge the use of Ned Wright’s calculator (Wright 2006) and NASA/IPAC Extragalactic Database (NED), operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge the use of IRAF which is distributed by the National Optical Astronomy Observatories, and operated by the Association of Universities for Research in Astronomy, Inc., under contract to the National Science Foundation.en_US
dc.description.urihttps://arxiv.org/abs/2011.03130en_US
dc.format.extent28 pagesen_US
dc.genrejournal articles preprintsen_US
dc.identifierdoi:10.13016/m2sr9w-t4gi
dc.identifier.citationAzadi, Mojegan; Wilkes, Belinda; Kuraszkiewicz, Joanna; McDowell, Jonathan; Siebenmorgen, Ralf; Ashby, Matthew; Birkinshaw, Mark; Worrall, Diana; Abrams, Natasha; Barthel, Peter; Fazio, Giovanni; Haas, Martin; Hyman, Sóley; Martínez-Galarza, Rafael; Meyer, Eileen; Disentangling the AGN and star-formation contributions to the radio-X-ray emission of radio-loud quasars at 1<z<2; High Energy Astrophysical Phenomena (2020); https://arxiv.org/abs/2011.03130en_US
dc.identifier.urihttp://hdl.handle.net/11603/21254
dc.language.isoen_USen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Physics Department Collection
dc.relation.ispartofUMBC Faculty Collection
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.subjectquasarsen_US
dc.subjectradio-louden_US
dc.subjectAGNen_US
dc.subjecthigh-redshiften_US
dc.subjectSEDen_US
dc.subjectgalaxiesen_US
dc.subjectactiveen_US
dc.subject3CRRen_US
dc.titleDisentangling the AGN and star-formation contributions to the radio-X-ray emission of radio-loud quasars at 1<z<2en_US
dc.typeTexten_US

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