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Two active states of the narrow-line gamma-ray-loud AGN GB 1310+487
dc.contributor.author | V. SOKOLOVSKY, K. | |
dc.contributor.author | K. SCHINZEL, F. | |
dc.contributor.author | T. TANAKA, Y. | |
dc.contributor.author | K. ABOLMASOV, P. | |
dc.contributor.author | ANGELAKIS, E. | |
dc.contributor.author | BULGARELLI, A. | |
dc.contributor.author | CARRASCO, L. | |
dc.contributor.author | B. CENKO, S. | |
dc.contributor.author | C. CHEUNG, C. | |
dc.contributor.author | I. CLUBB, K. | |
dc.contributor.author | D'AMMANDO, F. | |
hal.structure.identifier | GLAST | |
dc.contributor.author | ESCANDE, L. | |
hal.structure.identifier | Laboratoire Leprince-Ringuet [LLR] | |
dc.contributor.author | J. FEGAN, S. | |
dc.contributor.author | V. FILIPPENKO, A. | |
dc.contributor.author | D. FINKE, J. | |
dc.contributor.author | FUHRMANN, L. | |
dc.contributor.author | FUKAZAWA, Y. | |
dc.contributor.author | HAYS, E. | |
dc.contributor.author | E. HEALEY, S. | |
dc.contributor.author | IKEJIRI, Y. | |
dc.contributor.author | ITOH, R. | |
dc.contributor.author | S. KAWABATA, K. | |
dc.contributor.author | KOMATSU, T. | |
dc.contributor.author | A. KOVALEV, Yu. | |
dc.contributor.author | KOVALEV, Y.Y. | |
dc.contributor.author | P. KRICHBAUM, T. | |
dc.contributor.author | LARSSON, S. | |
dc.contributor.author | L. LISTER, M. | |
hal.structure.identifier | GLAST | |
dc.contributor.author | LOTT, B. | |
dc.contributor.author | MAX-MOERBECK, W. | |
dc.contributor.author | NESTORAS, I. | |
dc.contributor.author | PITTORI, C. | |
dc.contributor.author | PURSIMO, T. | |
dc.contributor.author | B. PUSHKAREV, A. | |
dc.contributor.author | C. S. READHEAD, A. | |
dc.contributor.author | RECILLAS, E. | |
dc.contributor.author | L. RICHARDS, J. | |
dc.contributor.author | RIQUELME, D. | |
dc.contributor.author | W. ROMANI, R. | |
dc.contributor.author | SAKIMOTO, K. | |
dc.contributor.author | SASADA, M. | |
dc.contributor.author | SCHMIDT, R. | |
dc.contributor.author | S. SHAW, M. | |
dc.contributor.author | SIEVERS, A. | |
dc.contributor.author | J. THOMPSON, D. | |
dc.contributor.author | UEMURA, M. | |
dc.contributor.author | UNGERECHTS, H. | |
dc.contributor.author | VERCELLONE, S. | |
dc.contributor.author | VERRECCHIA, F. | |
dc.contributor.author | YAMANAKA, M. | |
dc.contributor.author | YOSHIDA, M. | |
dc.contributor.author | A. ZENSUS, J. | |
dc.date.issued | 2014 | |
dc.identifier.issn | 0004-6361 | |
dc.description.abstractEn | Previously unremarkable, the extragalactic radio source GB 1310+487 showed a gamma-ray flare on 2009 November 18, reaching a daily flux of ~10^-6 photons/cm^2/s at energies E>100 MeV and becoming one of the brightest GeV sources for about two weeks. Its optical spectrum is not typical for a blazar, instead, it resembles those of narrow emission-line galaxies. We investigate changes of the object's radio-to-GeV spectral energy distribution (SED) during and after the prominent GeV flare with the aim to determine the nature of the object and constrain the origin of the variable high-energy emission. The data collected by the Fermi and AGILE satellites at gamma-ray energies, Swift at X-ray and ultraviolet, Kanata, NOT, and Keck telescopes at optical, OAGH and WISE at infrared, and IRAM 30m, OVRO 40m, Effelsberg 100m, RATAN-600, and VLBA at radio, are analysed together to trace the SED evolution on timescales of months. The gamma-ray/radio-loud narrow-line active galactic nucleus (AGN) is located at redshift z=0.638. It is shining through an unrelated foreground galaxy at z=0.500. The AGN light is likely amplified by a factor of a few because of gravitational lensing. The AGN SED shows a two-humped structure typical of blazars and gamma-ray-loud NLSy1 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. 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. | |
dc.language.iso | en | |
dc.publisher | EDP Sciences | |
dc.title.en | Two active states of the narrow-line gamma-ray-loud AGN GB 1310+487 | |
dc.type | Article de revue | |
dc.identifier.doi | 10.1051/0004-6361/201220703 | |
dc.subject.hal | Physique [physics]/Astrophysique [astro-ph]/Phénomènes cosmiques de haute energie [astro-ph.HE] | |
dc.subject.hal | Planète et Univers [physics]/Astrophysique [astro-ph]/Phénomènes cosmiques de haute energie [astro-ph.HE] | |
dc.identifier.arxiv | 1401.2151 | |
bordeaux.journal | Astronomy and Astrophysics - A&A | |
bordeaux.page | A26 | |
bordeaux.volume | 565 | |
bordeaux.peerReviewed | oui | |
hal.identifier | in2p3-01019653 | |
hal.version | 1 | |
hal.popular | non | |
hal.audience | Non spécifiée | |
hal.origin.link | https://hal.archives-ouvertes.fr//in2p3-01019653v1 | |
bordeaux.COinS | ctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2014&rft.volume=565&rft.spage=A26&rft.epage=A26&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=V.%20SOKOLOVSKY,%20K.&K.%20SCHINZEL,%20F.&T.%20TANAKA,%20Y.&K.%20ABOLMASOV,%20P.&ANGELAKIS,%20E.&rft.genre=article |
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