All Figures

$\begin{figure} \par\includegraphics[width=13.5cm,clip]{7486fig1.ps}\end{figure}$ Figure 1: $6'' \times 6''$ sections of the VLT/ NACO $K_{\rm s}$ and H band images of the PSR J1119-6127 field. North to the top, East to the left. The effect of the worse AO correction (see Sect. 2.1) is recognized from the asymmetric PSF of the stars in the field. The circle ( $0\hbox{$.\!\!^{\prime\prime}$ }3$ radius) corresponds to the pulsar radio position uncertainty after accounting for the accuracy of our astrometric solution (see Sect. 2.2).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7486fig2.ps}\end{figure}$ Figure 2: Expected IR spectrum of a fallback disk of inner radius $R_{\rm in}=R_{\rm lc}$ and two values of the disk accretion rate $\dot{M}$ : solid line: maximum value of $\dot{M}$ compatible with the IR limits; dashed line: maximum value of $\dot{M}$ compatible with the pulsar's spin down rate. The IR flux upper limits have been corrected for the interstellar extinction applying the relations of Fitzpatrick (1999) for A_V = 5, as derived from the X-ray absorption $N_{\rm H} = 9^{+5}_{-3}$ $\times$ 10²¹ cm^-2(Gonzalez & Safi-Harb 2003) and the relation $A_V = N_{\rm H}/1.79$ $\times$ 10²¹ atoms cm^-2 mag^-1 (Predhel & Schmitt 1995).
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{7486fig3.ps}\hspace*{3mm} \includegraphics[width=6cm,clip]{7486fig4.ps}\end{figure}$ Figure 3: left panel: measured K-band luminosities for all the isolated NSs listed in Table 2 as a function of the NSs rotational energy loss $\dot{E}$ . For J1119-6127 (labelled in the figures) we have plotted the IR luminosity upper limits corresponding to the most extreme distance/absorption values. For 4U 0142+61 we have plotted the IR luminosity lower limit corresponding to a lower limit on the source distance of 5 kpc (Hullemann et al. 2004). Red filled circles and blue filled squares indicate rotation-powered pulsars and magnetars, respectively. The red dashed line corresponds to the linear fit for rotation-powered pulsars while the solid line shows the limit case ${\rm Log} (L_{K}) = {\rm Log} (\dot E)$ . Right panel: the derived IR efficiencies, defined as the ratio between L_K and $\dot{E}$ , as a function of the dipole magnetic field B inferred from the NS spin down. Timing parameters have been taken from the ATNF Pulsar Database (http://www.atnf.csiro.au/research/pulsar/psrcat) for rotation-powered pulsars, and from Woods & Thompson (2006) for the magnetars. For both 1E 1048-5937 and SGR 1806-20 we have taken as a reference the average $\dot{P}$ value.
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In the text