(9 and 10); the “three musketeers” \[Geminga, PSR B1055–52, and PSR B0656+14 (12, 14, and 11)\]; one compact central object in SNR (RX J0822–4300, source 4); the compact source RX J0007.0+7303 at the center of the SNR CTA 1 (6); two “dim” (“truly isolated”) neutron stars RX J1856.4–3754 and RX J0720.4–3125 (13 and 16); two young and energetic pulsars J1119–6127 and J1357–6429 (3 and 5); and the old pulsar J2043+2740 (15).

The ages and effective surface temperatures of many sources are rather uncertain. For the sources mentioned in [@yakovlevetal04; @gusakovetal04; @kaminkeretal06a] the choice of $t$ and $T_{\rm s}^\infty$ is mainly the same as in these references. The ages of other sources are pulsar spindown ages, and the errobars of $t$ and $T_{\rm s}^\infty$ are chosen in the same way as in [@yakovlevetal04; @gusakovetal04; @kaminkeretal06a]. We have enlarged a possible age range of the source 2 to 5.4 kyr, the pulsar spindown age, because this source can be accidentally projected onto the SNR 3C 58 (Yu.A. Shibanov, private communication, 2007). The values of $T_{\rm s}^\infty$ are inferred from observations (reported in the indicated references) assuming either black-body (BB) spectrum or a hydroden atmosphere model (magnetic or nonmagnetic one, mHA or HA). 