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Fig. 3

image

Cumulative fraction of the energy output of the known Galactic pulsar population with ages < 107 yr (Manchester et al. 2005) created using the instantaneous energy output into electrons Ee as well as the energy output integrated up to 104 and 105 yr electron lifetimes. For comparison purposes, we show the cumulative γ-ray luminosity at 1 TeV from a generic PWN model as a function of system age, both for a constant magnetic field and a magnetic field evolving in time. The cumulative fraction of pulsars indicates that the energy output into electrons and γ-ray luminosity is dominated by a small fraction of young, energetic pulsars.

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