Fig. 9
Spin-down power distributions obtained for each model for the visible γ-ray pulsars. Pink and green refer to radio-loud and radio-quiet fractions of the total population, respectively. The LAT distribution (in black) has been scaled to the total number of visible pulsars for each model to ease the comparison and show the relative lack of young energetic pulsars with Ė > 3 × 1028 W.
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