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Caption: Figure 5.
γ-ray efficiency plotted against characteristic spin-down age for non-recycled γ-ray pulsars with available distance estimates (empty squares), and PSR J1836 + 5925, for which only an upper limit exists (solid triangle). Pulsars with two distance estimates have two markers connected with a dashed line. The solid black square corresponds to the efficiency and age of PSR J2043 + 2740; the solid gray square corresponds to the same pulsar's efficiency but assuming its age and distance are equal to those of the Cygnus Loop, i.e., τ = 12 kyr and D = 540 pc. All values of η in this plot were taken from Abdo et al. (2010a), except those for PSR J0248 + 6021 (τ c = 63 kyr) and PSR J2240 + 5832 (τ c = 151 kyr), which were taken from Theureau et al. (2011). The inset plot, at the bottom right corner, shows the distribution of 10 6 Spearman's rank correlation coefficients, r s, from an equal number of Monte Carlo realisations of the data based on the measured efficiencies and their errors. The median of the distribution is r s = 0.57 +0.06 −0.07, where the uncertainties correspond to the 1σ asymmetric errors.
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