Gamma-ray flaring activity from the gravitationally lensed blazar PKS 1830-211 observed by Fermi LAT
Creators: name: The Fermi LAT Collaboration
name: Abdo, A. A.
name: Ackermann, M.
name: Ajello, M.
name: Allafort, A.
name: Amin, M. A.
name: Baldini, L.
name: Barbiellini, G.
name: Bastieri, D.
name: Bechtol, K.
name: Bellazzini, R.
name: Blandford, R. D.
name: Bonamente, E.
name: Borgland, A. W.
name: Bregeon, J.
name: Brigida, M.
name: Buehler, R.
name: Bulmash, D.
name: Buson, S.
name: Caliandro, G. A.
name: Cameron, R. A.
name: Caraveo, P. A.
name: Cavazzuti, E.
name: Cecchi, C.
name: Charles, E.
name: Cheung, C. C.
name: Chiang, J.
name: Chiaro, G.
name: Ciprini, S.
name: Claus, R.
name: Cohen-Tanugi, J.
name: Conrad, J.
name: Corbet, R. H. D.
name: Cutini, S.
name: D'Ammando, F.
name: de Angelis, A.
name: de Palma, F.
name: Dermer, C. D.
name: Drell, P. S.
name: Drlica-Wagner, A.
name: Favuzzi, C.
name: Finke, J.
name: Focke, W. B.
name: Fukazawa, Y.
name: Fusco, P.
name: Gargano, F.
name: Gasparrini, D.
name: Gehrels, N.
name: Giglietto, N.
name: Giordano, F.
name: Giroletti, M.
name: Glanzman, T.
name: Grenier, I. A.
name: Grove, J. E.
name: Guiriec, S.
name: Hadasch, D.
name: Hayashida, M.
name: Hays, E.
name: Hughes, R. E.
name: Inoue, Y.
name: Jackson, M. S.
name: Jogler, T.
name: Jòhannesson, G.
name: Johnson, A. S.
name: Kamae, T.
name: Knödlseder, J.
name: Kuss, M.
name: Lande, J.
name: Larsson, S.
name: Latronico, L.
name: Longo, F.
name: Loparco, F.
name: Lott, B.
name: Lovellette, M. N.
name: Lubrano, P.
name: Madejski, G. M.
name: Mazziotta, M. N.
name: Mehault, J.
name: Michelson, P. F.
name: Mizuno, T.
name: Monzani, M. E.
name: Morselli, A.
name: Moskalenko, I. V.
name: Murgia, S.
name: Nemmen, R.
name: Nuss, E.
name: Ohno, M.
name: Ohsugi, T.
name: Paneque, D.
name: Perkins, J. S.
name: Pesce-Rollins, M.
name: Piron, F.
name: Pivato, G.
name: Porter, T. A.
name: Rainò, S.
name: Rando, R.
name: Razzano, M.
name: Reimer, A.
name: Reimer, O.
name: Reyes, L. C.
name: Ritz, S.
name: Romoli, C.
name: Roth, M.
name: Parkinson, P. M. Saz
name: Sgrò, C.
name: Siskind, E. J.
name: Spandre, G.
name: Spinelli, P.
name: Takahashi, H.
name: Takeuchi, Y.
name: Tanaka, T.
name: Thayer, J. G.
name: Thayer, J. B.
name: Thompson, D. J.
name: Tibaldo, L.
name: Tinivella, M.
name: Torres, D. F.
name: Tosti, G.
name: Troja, E.
name: Tronconi, V.
name: Usher, T. L.
name: Vandenbroucke, J.
name: Vasileiou, V.
name: Vianello, G.
name: Vitale, V.
name: Waite, A. P.
name: Werner, M.
name: Winer, B. L.
name: Wood, K. S.
Publisher: name: arXiv
Year: 2014
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope routinely detects the highly dust-absorbed, reddened, and MeV-peaked flat spectrum radio quasar PKS 1830-211 (z=2.507). Its apparent isotropic gamma-ray luminosity (E&gt;100 MeV) averaged over $\sim$ 3 years of observations and peaking on 2010 October 14/15 at 2.9 X 10^{50} erg s^{-1}, makes it among the brightest high-redshift Fermi blazars. No published model with a single lens can account for all of the observed characteristics of this complex system. Based on radio observations, one expects time delayed variability to follow about 25 days after a primary flare, with flux about a factor 1.5 less. Two large gamma-ray flares of PKS 1830-211 have been detected by the LAT in the considered period and no substantial evidence for such a delayed activity was found. This allows us to place a lower limit of about 6 on the gamma rays flux ratio between the two lensed images. Swift XRT observations from a dedicated Target of Opportunity program indicate a hard spectrum and with no significant correlation of X-ray flux with the gamma-ray variability. The spectral energy distribution can be modeled with inverse Compton scattering of thermal photons from the dusty torus. The implications of the LAT data in terms of variability, the lack of evident delayed flare events, and different radio and gamma-ray flux ratios are discussed. Microlensing effects, absorption, size and location of the emitting regions, the complex mass distribution of the system, an energy-dependent inner structure of the source, and flux suppression by the lens galaxy for one image path may be considered as hypotheses for understanding our results.
description: 14 pages, 6 figures, 2 tables. Accepted by the The Astrophysical Journal. Corresponding authors: S. Ciprini (ASI ASDC &amp; INAF OAR, Rome, Italy), S. Buson (INAF Padova &amp; Univ. of Padova, Padova, Italy), J. Finke (NRL, Washington, DC, USA), F. D'Ammando (INAF IRA, Bologna, Italy)