AGILE, Fermi, Swift, and GASP/WEBT multi-wavelength observations of the high-redshift blazar 4C +71.07 in outburst
Journal
Date Issued
2019
Author(s)
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Donnarumma, I.
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Munar-Adrover, P.
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Acosta-Pulido, J. A.
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Agudo, I.
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Arkharov, A. A.
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Bach, U.
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Bachev, R.
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Borman, G. A.
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Butuzova, M. S.
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Casadio, C.
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Damljanovic, G.
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Doroshenko, V. T.
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Efimova, N. V.
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Ehgamberdiev, Sh. A.
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Gómez, J. L.
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Grishina, T. S.
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Järvelä, E.
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Klimanov, S. A.
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Kopatskaya, E. N.
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Kurtanidze, O. M.
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Lähteenmäki, A.
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Larionov, V. M.
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Larionova, L. V.
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Mihov, B.
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Mirzaqulov, D. O.
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Molina, S. N.
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Morozova, D. A.
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Nazarov, S. V.
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Savchenko, S. S.
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Semkov, E.
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Slavcheva-Mihova, L.
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Strigachev, A.
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Tornikoski, M.
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Troitskaya, Yu. V.
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Vince, O.
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Cattaneo, P. W.
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Colafrancesco, S.
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Longo, F.
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Morselli, A.
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Paoletti, F.
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Abstract
Context. The flat-spectrum radio quasar 4C +71.07 is a high-redshift (z = 2.172), γ-loud blazar whose optical emission is dominated by thermal radiation from the accretion disc.
Aims: 4C +71.07 has been detected in outburst twice by the AGILE γ-ray satellite during the period from the end of October to mid-November 2015, when it reached a γ-ray flux of the order of F(E > 100 MeV)=(1.2 ± 0.3)×10-6 photons cm-2 s-1 and F(E > 100 MeV)=(3.1 ± 0.6)×10-6 photons cm-2 s-1, respectively, allowing us to investigate the properties of the jet and the emission region.
Methods: We investigated its spectral energy distribution by means of almost-simultaneous observations covering the cm, mm, near-infrared, optical, ultraviolet, X-ray, and γ-ray energy bands obtained by the GASP-WEBT Consortium and the Swift, AGILE, and Fermi satellites.
Results: The spectral energy distribution of the second γ-ray flare (whose energy coverage is more dense) can be modelled by means of a one-zone leptonic model, yielding a total jet power of about 4 × 1047 erg s-1.
Conclusions: During the most prominent γ-ray flaring period our model is consistent with a dissipation region within the broad-line region. Moreover, this class of high-redshift, flat-spectrum radio quasars with high-mass black holes might be good targets for future γ-ray satellites such as e-ASTROGAM.
Aims: 4C +71.07 has been detected in outburst twice by the AGILE γ-ray satellite during the period from the end of October to mid-November 2015, when it reached a γ-ray flux of the order of F(E > 100 MeV)=(1.2 ± 0.3)×10-6 photons cm-2 s-1 and F(E > 100 MeV)=(3.1 ± 0.6)×10-6 photons cm-2 s-1, respectively, allowing us to investigate the properties of the jet and the emission region.
Methods: We investigated its spectral energy distribution by means of almost-simultaneous observations covering the cm, mm, near-infrared, optical, ultraviolet, X-ray, and γ-ray energy bands obtained by the GASP-WEBT Consortium and the Swift, AGILE, and Fermi satellites.
Results: The spectral energy distribution of the second γ-ray flare (whose energy coverage is more dense) can be modelled by means of a one-zone leptonic model, yielding a total jet power of about 4 × 1047 erg s-1.
Conclusions: During the most prominent γ-ray flaring period our model is consistent with a dissipation region within the broad-line region. Moreover, this class of high-redshift, flat-spectrum radio quasars with high-mass black holes might be good targets for future γ-ray satellites such as e-ASTROGAM.
Partly based on data taken and assembled by the WEBT collaboration and stored in the WEBT archive at the Osservatorio Astrofisico di Torino - INAF (http://www.oato.inaf.it/blazars/webt).
Volume
621
Start page
A82
Issn Identifier
0004-6361
Ads BibCode
2019A&A...621A..82V
Rights
open.access
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