(Vela)              11–25            $0.68\pm0.03$           68%         mHA     [@pavlovetal01]
     8     PSR B1706–44                   $\sim$17      0.82$^{+0.01}_{-0.34}$       68%         mHA     [@mcgowanetal04]
     9     PSR J0538+2817                 $30 \pm4$           $\sim 0.87$             –          mHA     [@zp04]
     10    PSR B2334+61                   $\sim 41$          $\sim 0.69 $             –          mHA     [@zavlin07]
     11    PSR B0656+14                   $\sim$110          0.91$\pm$0.05           90%         BB      [@possentietal96]
     12    PSR B0633+1748 (Geminga)       $\sim$340           $\sim 0.5$              –          BB      [@kargaltsevetal05]
     13    RX J1856.4–3754                $\sim$500         $0.434\pm0.003$          68%        mHA$^*$  [@hoetal07]
     14    PSR B1055–52                   $\sim$540          $\sim 0.75 $             –          BB      [@pz03]
     15    PSR J2043+2740                $\sim 1200$         $\sim 0.44 $             –          mHA     [@zavlin07]
     16    RX J0720.4–3125               $\sim 1300$          $\sim 0.51$             –         HA$^*$   [@motchetal03]

  : Observational limits on surface temperatures of isolated neutron stars[]{data-label="tab-cool-data"}

We will compare cooling theory with observations of surface thermal radiation of isolated neutron stars. The current state of the observations is discussed, e.g., in Refs. [@zavlin07; @deluca07; @kaplan07]. In Table \[tab-cool-data\] we list 16 isolated neutron stars whose effective surface temperatures have been measured or constrained. For brevity, the stars are numbered, and these numbers are used in the text and figures. The data include two neutron stars (1 and 2, the pulsars Crab and J0205+6449) in historical supernova remnants (SNRs); the famous Vela pulsar (7) and the similar PSR B1706–44 (8); the “pulsar-twins” J0538+2817 and B2334+61 