We report the detection of high-energy γ-rays from the quiescent Sun with the Large Area Telescope on board the Fermi Gamma-Ray Space Telescope (Fermi) during the first 18 months of the mission. These observations correspond to the recent period of low solar activity when the emission induced by cosmic rays (CRs) is brightest. For the first time, the high statistical significance of the observations allows clear separation of the two components: the point-like emission from the solar disk due to CR cascades in the solar atmosphere and extended emission from the inverse Compton (IC) scattering of CR electrons on solar photons in the heliosphere. The observed integral flux (≥100MeV) from the solar disk is (4.6 ± 0.2[statistical error] +1.0 - 0.8[systematic error]) × 10 -7cm-2s-1, which is 7 times higher than predicted by the "nominal" model of Seckel etal. In contrast, the observed integral flux (≥100MeV) of the extended emission from a region of 20° radius centered on the Sun, but excluding the disk itself, (6.8 ± 0.7[stat.]+0.5 - 0.4[syst.]) × 10 -7cm-2s-1, along with the observed spectrum and the angular profile, is in good agreement with the theoretical predictions for the IC emission.
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