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Two Active States of the Narrow-Line Gamma-Ray-Loud AGN GB 1310 + 487Context. Previously unremarkable, the extragalactic radio source GB1310 487 showed gamma-ray flare on 2009 November 18, reaching a daily flux of approximately 10(exp -6) photons cm(exp -2) s(exp -1) at energies E greater than 100MeV and became one of the brightest GeV sources for about two weeks. Its optical spectrum shows strong forbidden-line emission while lacking broad permitted lines, which is not typical for a blazar. Instead, the spectrum resembles those of narrow emission-line galaxies. Aims. We investigate changes in the object's radio-to-GeV spectral energy distribution (SED) during and after the prominent gamma-ray flare with the aim of determining the nature of the object and of constraining the origin of the variable high-energy emission. Methods. The data collected by the Fermi and AGILE satellites at gamma-ray energies; Swift at X-ray and ultraviolet (UV); the Kanata, NOT, and Keck telescopes at optical; OAGH and WISE at infrared (IR); and IRAM30m, OVRO 40m, Effelsberg 100m, RATAN-600, and VLBA at radio are analyzed together to trace the SED evolution on timescales of months. Results. The gamma-ray radio-loud narrow-line active galactic nucleus (AGN) is located at redshift z = 0.638. It shines through an unrelated foreground galaxy at z = 0.500. The AGN light is probably amplified by gravitational lensing. The AGN SED shows a two-humped structure typical of blazars and gamma-ray-loud narrow-line Seyfert 1 galaxies, with the high-energy (inverse-Compton) emission dominating by more than an order of magnitude over the low-energy (synchrotron) emission during gamma-ray flares. The difference between the two SED humps is smaller during the low-activity state. Fermi observations reveal a strong correlation between the gamma-ray flux and spectral index, with the hardest spectrum observed during the brightest gamma-ray state. The gamma-ray flares occurred before and during a slow rising trend in the radio, but no direct association between gamma-ray and radio flares could be established. Conclusions. If the gamma-ray flux is a mixture of synchrotron self-Compton (SSC) and external Compton (EC) emission, the observed GeV spectral variability may result from varying relative contributions of these two emission components. This explanation fits the observed changes in the overall IR to gamma-ray SED.
Document ID
20150011020
Acquisition Source
Goddard Space Flight Center
Document Type
Preprint (Draft being sent to journal)
Authors
Sokolovsky, K. V. (Max-Planck-Inst. fuer Radioastronomie Bonn, Germany)
Schinzel, F. K. (Max-Planck-Inst. fuer Radioastronomie Bonn, Germany)
Tanaka, Y. T. (Hiroshima Univ. Japan)
Abolmasov, P. K. (Moscow State Univ. Russian Federation)
Angelakis, E. (Max-Planck-Inst. fuer Radioastronomie Bonn, Germany)
Bulgarelli, A. (Istituto Nazionale di Astrofisica Spaziale e Fisica Cosmica (INAF-IASF) Bologna, Italy)
Carrasco, L. (Instituto Nacional de Astrofisica, Optica y Electronica Puebla, Mexico)
Cenko, S. B. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Cheung, C. C. (National Academy of Sciences - National Research Council Washington, DC, United States)
Clubb, K. I. (California Univ. Berkeley, CA, United States)
D'Ammando, F. (Perugia Univ. Perugia, Italy)
Escande, L. (Bordeaux 1 Univ. Gradignan, France)
Fegan, S. J. (Ecole Polytechnique Palaiseau, France)
Filippenko, A. V. (California Univ. Berkeley, CA, United States)
Finke, J. D. (Naval Research Lab. Washington, DC, United States)
Fuhrmann, L. (Max-Planck-Inst. fuer Radioastronomie Bonn, Germany)
Fukazawa, Y. (Hiroshima Univ. Japan)
Hays, E. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Healey, S. E. (Stanford Univ. Stanford, CA, United States)
Ikejiri, Y. (Hiroshima Univ. Japan)
Itoh, R. (Hiroshima Univ. Japan)
Kawabata, K. S. (Hiroshima Univ. Japan)
Komatsu, T. (Hiroshima Univ. Japan)
Kovalev, Yu. A. (Lebedev Physical Inst. Moscow, Russian Federation)
Kovalev, Y. Y. (Lebedev Physical Inst. Moscow, Russian Federation)
Krichbaum, T. P. (Max-Planck-Inst. fuer Radioastronomie Bonn, Germany)
Date Acquired
June 17, 2015
Publication Date
March 14, 2014
Publication Information
Publisher: ESO
Subject Category
Astrophysics
Report/Patent Number
GSFC-E-DAA-TN21932
Funding Number(s)
CONTRACT_GRANT: NNX08AW31G
CONTRACT_GRANT: NXX12A075G
CONTRACT_GRANT: NNG06GG1G
CONTRACT_GRANT: 14.518.11.7054
CONTRACT_GRANT: NSF AST-0808050
CONTRACT_GRANT: NNX08AV67G
CONTRACT_GRANT: NNX12AF12GA
Distribution Limits
Public
Copyright
Public Use Permitted.
Keywords
states
Two
active

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