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 J1823−3021A and J1824−2452A, 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.