Fig. 8

image

Spectral energy distribution of the PWN G0.13−0.11. The butterflies show the spectral confidence regions of G0.13−0.11 measured with Chandra (Wang et al. 2002), of 1FHL J1746.3−2851 (Ackermann et al. 2013) and of HESS J1746−285. The upper limit is obtained from the 90 cm map of LaRosa et al. (2000). The lines show two models of PWN emission for G0.13−0.11, assuming an IC dominated evolution of the particles (see Sect. 4.2 for details). The X-ray and VHE γ-ray spectra are well accounted for by an electron population injected at a few 1035 erg/s (steady-state model, blue). Part of the flux observed above 10 GeV could be explained assuming a significant decay of the pulsar spin-down power (relic model, red).

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