X-ray luminosity of ordinary and millisecond pulsars investigated in this study versus their spindown powers Ė calculated with YMW+17-based distances (left) and NE2001-based distances (right). Sources with parallax measurements are displayed with yellow. The up-pointing triangles show the 1–10 keV non-thermal luminosities obtained via the PL assumption (with Γ = 1.7) for the underlying spectra, and the down-pointing triangles show the 0.3–2.0 keV thermal luminosities obtained via the BB assumption (with kT = 300 eV) (see discussion in Sect. 2.4). The spectrum-derived PL flux for J1831–0952 is shown as a green triangle. Ė values are corrected for the Shklovskii effect where relevant (Shklovskii 1970).