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|Title:||Properties of flat-spectrum radio-loud narrow-line Seyfert 1 galaxies||Authors:||FOSCHINI, LUIGI
Peterson, B. M.
Kovalev, Y. Y.
Lisakov, M. M.
Lister, M. L.
Richards, J. L.
La Mura, G.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||575||First Page:||A13||Abstract:||We have conducted a multiwavelength survey of 42 radio loud narrow-1ine Seyfert 1 galaxies (RLNLS1s), selected by searching among all the known sources of this type and omitting those with steep radio spectra. We analyse data from radio frequencies to X-rays, and supplement these with information available from online catalogues and the literature in order to cover the full electromagnetic spectrum. This is the largest known multiwavelength survey for this type of source. We detected 90% of the sources in X-rays and found 17% at γ rays. Extreme variability at high energies was also found, down to timescales as short as hours. In some sources, dramatic spectral and flux changes suggest interplay between a relativistic jet and the accretion disk. The estimated masses of the central black holes are in the range ~10<SUP>6-8</SUP> M<SUB>☉</SUB>, lower than those of blazars, while the accretion luminosities span a range from ~0.01 to ~0.49 times the Eddington limit, with an outlier at 0.003, similar to those of quasars. The distribution of the calculated jet power spans a range from ~10<SUP>42.6</SUP> to ~10<SUP>45.6</SUP> erg s<SUP>-1</SUP>, generally lower than quasars and BL Lac objects, but partially overlapping with the latter. Once normalised by the mass of the central black holes, the jet power of the three types of active galactic nuclei are consistent with each other, indicating that the jets are similar and the observational differences are due to scaling factors. Despite the observational differences, the central engine of RLNLS1s is apparently quite similar to that of blazars. The historical difficulties in finding radio-loud narrow-line Seyfert 1 galaxies might be due to their low power and to intermittent jetactivity. <P />Tables 4-9 and Figs. 8-13 are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201424972/olm">http://www.aanda.org</A>||Acknowledgments:||We would like to thank the members of the Fermi LAT Collaboration – David Thompson, Denis Bastieri, Jeremy Perkins, and Filippo D’Ammando – for a critical review of the manuscript. Part of the Swift observations have been supported by the contract ASI-INAF I/004/11/0. The Metsähovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others) Y.Y.K. and M.M.L. are partly supported by the Russian Foundation for Basic Research (project 13-02-12103). Y.Y.K. is also supported by the Dynasty Foundation. B.M.P. is supported by the NSF through grant AST-1008882. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009 ; 2013 ). The MOJAVE program is supported under NASA Fermi grant NNX12AO87G. J.L.R. acknowledges support from NASA through Fermi Guest Investigator grant NNX13AO79G. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/ . SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.||URI:||http://hdl.handle.net/20.500.12386/23153||URL:||https://www.aanda.org/articles/aa/abs/2015/03/aa24972-14/aa24972-14.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201424972||Bibcode ADS:||2015A&A...575A..13F||Fulltext:||open|
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