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AGILE detects enhanced gamma-ray activity of the Blazar 3C 454.3

ATel #6182; F. Verrecchia, F. Lucarelli, C. Pittori (ASDC and INAF/OAR), V. Fioretti (INAF/IASF-Bo), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), S. Vercellone (INAF/IASF-Pa), I. Donnarumma (INAF/IAPS), A. Bulgarelli (INAF/IASF-Bo), G. Piano (INAF/IAPS), E. Striani (CIFS and INAF/IAPS), M. Cardillo (INAF/OA-Arcetri and INAF/IAPS), F. Gianotti, M. Trifoglio (INAF/IASF-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Chen (Wits University and INAF/IASF-Mi), S. Colafrancesco (INAF/OAR and Wits University), E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda, A. Argan, G. Pucella, S. Sabatini, A. Trois, V. Vittorini (INAF/IAPS), F. Fuschino, M. Galli, C. Labanti, M. Marisaldi, G. Di Cocco (INAF/IASF-Bo), A. Pellizzoni (INAF/OA-Cagliari), M. Pilia (ASTRON, the Netherlands), G. Barbiellini, E. Vallazza (INFN Trieste), F. Longo (Univ. Trieste and INFN Trieste), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Univ. dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), P. Giommi (ASDC), L. Salotti, and G. Valentini (ASI)
on 28 May 2014; 14:51 UT
Credential Certification: Francesco Verrecchia (francesco.verrecchia@asdc.asi.it)

Subjects: Gamma Ray, >GeV, AGN, Blazar, Transient

Referred to by ATel #: 6213, 6217, 6232, 6234, 6236, 6237, 6266

The AGILE satellite detects gamma-ray activity from the FSRQ 3C 454.3 after an extended period of low flux levels during 2013. The source entered the AGILE Field of View at the end of April, 2014, and an enhanced variable emission above 100 MeV has been detected since May 18th.

A maximum likelihood analysis of the AGILE-GRID data for the integration period between 2014-05-25 03:00 UT and 2014-05-27 03:00 UT, gives a flux F=(2.4 +/- 0.8)x 10^-6 ph/cm^-2/s^-1 (E > 100 MeV).

This measurement was obtained with AGILE observing a large portion of the sky in spinning mode.

Multifrequency observations of the source are strongly encouraged.