{"paper":{"title":"The structure and emission model of the relativistic jet in the quasar 3C 279 inferred from radio to high-energy gamma-ray observations in 2008-2010","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.HE","authors_text":"A. A. Arkharov, A. Berdyugin, A. Di Paola, A. E. Wehrle, A. Lahteenmaki, A. Lamerato, A. P. Marscher, A. Readhead, A. Reimer, A. Rossi, A. Sillanpaa, A. Szostek, B. Jordan, B. Taylor, C. M. Raiteri, C. S. Buemi, C. Trigilio, D. A. Blinov, D. A. Morozova, D. Carosati, D. C.-J. Bock, D. Hiriart, E. Benitez, E. Cavazzuti, E. Forne, E. G. Larionova, E. Koptelova, E. Lindfors, E. N. Kopatskaya, G. Kimeridze, G. M. Madejski, G. Tosti, G. Umana, H. D. Aller, I. Agudo, I. M. McHardy, I. S. Troitsky, J. Chiang, J. Greiner, J. Heidt, J. L. Gomez, J. L. Richards, J. P. Macquart, J. Tammi, K. Blumenthal, K. Nalewajko, K. Nilsson, K. Sakimoto, K. S. Kawabata, L. A. Sigua, L. Stawarz, L. Takalo, L. V. Larionova, M. A. Gurwell, M. Boettcher, M. Dolci, M. F. Aller, M. G. Nikolashvili, M. Hayashida, M. Joshi, M. Kino, M. Sasada, M. Sikora, M. Tornikoski, M. Uemura, M. Villata, M. Yamanaka, N. Gehrels, N. V. Efimova, O. M. Kurtanidze, P. Leto, P. Ogle, P. Roustazadeh, R. Buehler, R. D. Blandford, R. Itoh, R. Reinthal, S. Ciprini, S. G. Jorstad, S. Larsson, S. N. Molina, S. Sato, T. Kruehler, T. Sakamoto, T. S. Konstantinova, T. Tanaka, U. Bach, V. M. Larionov, W. Collmar, W. Max-Moerbeck, W. P. Chen, Y. Fukazawa, Y. Uchiyama","submitted_at":"2012-06-04T20:00:29Z","abstract_excerpt":"We present time-resolved broad-band observations of the quasar 3C 279 obtained from multi-wavelength campaigns conducted during the first two years of the Fermi Gamma-ray Space Telescope mission. While investigating the previously reported gamma-ray/optical flare accompanied by a change in optical polarization, we found that the optical emission appears delayed with respect to the gamma-ray emission by about 10 days. X-ray observations reveal a pair of `isolated' flares separated by ~90 days, with only weak gamma-ray/optical counterparts. The spectral structure measured by Spitzer reveals a sy"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1206.0745","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}