FERMI-LAT-SCIENTIFIC PLOTS
a9
. Spectral energy distribution of the Crab Nebula from soft to very high energy γ-rays. The Whipple spectrum above 500 GeV (Hillas et al. 1998) is also consistent with these measurements. The fit of the synchrotron component, using COMPTEL and LAT data (blue dashed line), is overlaid. The predicted IC spectra from Atoyan & Aharonian (1996) are overlaid for three different values of the mean magnetic field: 100 μG (solid red line), 200 μG (dashed green line), and the canonical equipartition field of the Crab Nebula 300 μG (dotted blue line). References: CGRO COMPTEL and EGRET, Kuiper et al. 2001; MAGIC, Albert et al. 2008; HESS, Aharonian et al. 2006; CANGAROO, Tanimori et al. 1998; VERITAS, Celik 2007; HEGRA, Aharonian et al. 2004; CELESTE, Smith et al. 2006.
a9
. Spectral energy distribution of the Crab Nebula from soft to very high energy γ-rays. The Whipple spectrum above 500 GeV (Hillas et al. 1998) is also consistent with these measurements. The fit of the synchrotron component, using COMPTEL and LAT data (blue dashed line), is overlaid. The predicted IC spectra from Atoyan & Aharonian (1996) are overlaid for three different values of the mean magnetic field: 100 μG (solid red line), 200 μG (dashed green line), and the canonical equipartition field of the Crab Nebula 300 μG (dotted blue line). References: CGRO COMPTEL and EGRET, Kuiper et al. 2001; MAGIC, Albert et al. 2008; HESS, Aharonian et al. 2006; CANGAROO, Tanimori et al. 1998; VERITAS, Celik 2007; HEGRA, Aharonian et al. 2004; CELESTE, Smith et al. 2006.