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Fig. 3


Left: spin-down power Ė divided by the square of the distance d as a function of the period P, for MSPs in the Galactic disk. PSRs J18233021A and J18242452A, two MSPs in globular clusters but detected in γ rays, are included in the plot. Green stars represent γ-ray MSPs, undetected ones are shown as red circles. Guillemot & Tauris (2014) explain non-detections of energetic and distant MSPs in γ rays as due to unfavorable viewing angles. All Ė values are corrected for the effect of the acceleration in the Galactic potential. Filled symbols indicate pulsars for which we could correct for the kinematic Shklovskii effect. The right-hand panel shows the cumulative fraction of MSPs detected in γ rays, with decreasing Ė/d2 as indicated by the green arrow. Right: spin-down power values for the MSPs with Ė/d2 ≥ 1.5 × 1032 erg s-1 kpc-2. Half of the MSPs in this sample are seen with the Fermi-LAT. The green histogram shows the γ-detected MSPs, the empty histogram corresponds to the total number of MSPs in each Ė decade. The dashed line shows the fraction of γ-detected MSPs per Ė decade.

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