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Fig. 11


Our best-adjusted model to the observed spectral energy distribution of LS 5039. Top: the black curve is the average model spectrum; the synchrotron (~ 1 eV) and inverse Compton (~ 1 GeV) contributions from the Maxwellian population of electrons are in dark blue; the contributions from the power-law population are in light blue. Bottom: the thick, dark blue curve (resp. light blue curve) represents the INFC (resp. SUPC) spectrum, the thin grey curves represent the evolution of the SED in orbital phase steps of 1/30. From left to right, the data shown are: the orbital maximum and minimum X-ray bowties from Suzaku (Takahashi et al. 2009), the BATSE data points and INTEGRAL bowtie (Harmon et al. 2004; Hoffmann et al. 2009), the average COMPTEL data points with bowtie (Collmar & Zhang 2014), the average Fermi-LAT spectrum with data points from 100 MeV to 50 GeV and the best-fit power law with exponential cutoff (Hadasch et al. 2012), the HESS INFC (dark blue bowtie) and SUPC spectra (light blue bowtie) with the associated data points from 100 GeV to 30 TeV (Aharonian et al. 2006).

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