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Oxford University Press (OUP), Monthly Notices of the Royal Astronomical Society, 3(425), p. 2015-2026

DOI: 10.1111/j.1365-2966.2012.21540.x

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The characterization of the distant blazar GB6 J1239+0443 from flaring and low activity periods

Journal article published in 2012 by L. Pacciani, I. Donnarumma ORCID, K. D. Denney, R. J. Assef, Y. Ikejiri, M. Yamanaka, M. Uemura, A. Domingo, P. Giommi, A. Tarchi, F. Verrecchia, F. Longo, S. Rainó, M. Giusti, S. Vercellone and other authors.
This paper is made freely available by the publisher.
This paper is made freely available by the publisher.

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Abstract

In 2008 AGILE and Fermi detected gamma-ray flaring activity from the unidentified EGRET source 3EG J1236+0457, recently associated with a flat spectrum radio quasar GB6 J1239+0443 at z=1.762. The optical counterpart of the gamma-ray source underwent a flux enhancement of a factor 15-30 in 6 years, and of ~10 in six months. We interpret this flare-up in terms of a transition from an accretion-disk dominated emission to a synchrotron-jet dominated one. We analysed a Sloan Digital Sky Survey (SDSS) archival optical spectrum taken during a period of low radio and optical activity of the source. We estimated the mass of the central black hole using the width of the CIV emission line. In our work, we have also investigated SDSS archival optical photometric data and UV GALEX observations to estimate the thermal-disk emission contribution of GB6 J1239+0443. Our analysis of the gamma-ray data taken during the flaring episodes indicates a flat gamma-ray spectrum, with an extension of up to 15 GeV, with no statistically-relevant sign of absorption from the broad line region, suggesting that the blazar-zone is located beyond the broad line region. This result is confirmed by the modeling of the broad-band spectral energy distribution (well constrained by the available multiwavelength data) of the flaring activity periods and by the accretion disk luminosity and black hole mass estimated by us using archival data. ; Comment: 30 pages, 7 figures, 4 tables MNRAS Accepted on 2012 June 18