Abdo, A. A.A. A.AbdoGiommi, PaoloPaoloGiommiAjello, M.M.AjelloAckermann, M.M.AckermannAjello, M.M.AjelloTosti, G.G.TostiCutini, SaraSaraCutiniGasparrini, DarioDarioGasparriniGiommi, PaoloPaoloGiommi2020-09-172020-09-172020-09-172020-09-172011-07-01https://hdl.handle.net/20.500.13025/2238The Astrophysical Journal Letters, Volume 736, Issue 1, article id. L11, (2011).We report on the discovery of ≥100 MeV γ-rays from the binary system PSR B1259−63/LS 2883 using the Large Area Telescope (LAT) on board Fermi. The system comprises a radio pulsar in orbit around a Be star. We report on LAT observations from near apastron to ~128 days after the time of periastron, tp, on 2010 December 15. No γ-ray emission was detected from this source when it was far from periastron. Faint γ-ray emission appeared as the pulsar approached periastron. At ~tp + 30 days, the ≥100 MeV γ-ray flux increased over a period of a few days to a peak flux 20–30 times that seen during the pre-periastron period, but with a softer spectrum. For the following month, it was seen to be variable on daily timescales, but remained at ~(1–4) × 10−6 cm−2 s−1 before starting to fade at ~tp + 57 days. The total γ-ray luminosity observed during this period is comparable to the spin-down power of the pulsar. Simultaneous radio and X-ray observations of the source showed no corresponding dramatic changes in radio and X-ray flux between the pre-periastron and post-periastron flares. We discuss possible explanations for the observed γ-ray-only flaring of the source.binaries eclipsinggamma rays starspulsars individual PSR B1259--63X-rays binariesjournal article54dcce0e8580fe1368eeb4cb54dcce0e8580fe1368eeb4cb10.1088/2041-8205/736/1/L1154dcce0e8580fe1368eeb4cb54dcce0e8580fe1368eeb4cb54dcce0e8580fe1368eeb4cbhttp://iopscience.iop.org/2041-8205/736/1/L11http://dx.doi.org/10.1088/2041-8205/736/1/L112011ApJ...736L..11A54dcce0e8580fe1368eeb4cb