All Figures

$\begin{figure} \par\setlength{\unitlength}{1mm} \begin{picture} (180,120)(0,0) ... ...width=59mm,bb=43 43 362.36 364,clip]{H4269F1_6.eps} } \end{picture} \end{figure}$ Figure 1: The central part of the Crab nebula in the infrared, $J_{\rm s}$ (left), H (middle) and $K_{\rm s}$ (right). Observations obtained with ISAAC on 13 October 2000. The pulsar is the lower right (South Preceding) of the two bright objects near the center of the field. The field of view shown is $60\hbox {$^{\prime \prime }$ }\times 60\hbox {$^{\prime \prime }$ }$ centered on the pulsar. North is up and East to the left. The upper panels show the original images, and the lower panels show the images where several objects, including the pulsar, have been PSF subtracted. The lower panels are intended to reveal the knot positioned very close to the pulsar. Detailed color images of these frames are presented in Sollerman & Flyckt (2002).
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In the text

$\begin{figure} \par\includegraphics[width=13.7cm,clip]{H4269F2.ps} \end{figure}$ Figure 2: Spectral energy distribution of the Crab pulsar. The optical and UV data are from Sollerman et al. (2000). The triangles are our new ISAAC measurements. Also shown (squares) are the fluxes of the knot, here multiplied by a factor ten. The optical data for the knot is from HST. The knot data error bars illustrate an uncertainty of $10\%$ in the flux. All observed fluxes were dereddened using R=3.1 and E(B-V)=0.52.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{H4269F3.eps} \end{figure}$ Figure 3: Comparison between the pulsars with observed near-IR emission, from Shibanov et al. (2003). See text for discussion.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{H4269F3.eps} \end{figure}$	Figure 3: Comparison between the pulsars with observed near-IR emission, from Shibanov et al. (2003). See text for discussion.
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