All Figures

$\begin{figure*} \par\setlength{\unitlength}{1mm} \resizebox{12cm}{!}{ \begin{p... ...eight=5.15cm,bb=76 155 527 620,clip]{4178fig1c.ps}} \end{picture}} \end{figure*}$ Figure 1: $20\hbox {$^{\prime \prime }$ }\times 20\hbox {$^{\prime \prime }$ }$ fragments of the Subaru images of the PSR B0656+14 field in the B, R, and I bands. Units of RA (horizontal axis) are hours, minutes and seconds, and units of Dec (vertical one) are degrees, arcminutes and arcseconds. A box in the right panel marks the region which is magnified in Fig. 6 and discussed in Sect. 2.2.
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In the text

$\begin{figure} \par\setlength{\unitlength}{1mm} \begin{picture} (54,108)(0,0) \... ...idth=5.2cm,bb=130 205 485 570,clip]{4178fig2b.ps} } \end{picture}\end{figure}$ Figure 2: $20'' \times 20''$ fragments of the Subaru images of the Geminga field in the R ( top) and I ( bottom) bands. Axes orientation and label notations are the same as in Fig. 1.
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In the text

$\begin{figure} \setlength{\unitlength}{1mm} \begin{picture} (180,60)(0,0) \put(... ...[width=5.7cm, bb=37 127 575 665,clip]{4178fig3c.ps} } \end{picture} \end{figure}$ Figure 3: Left: a fragment of the Geminga field image obtained with the ESO/NTT in the I band (Bignami et al. 1996). The contours of the Subaru I band image are overlaid and the dashed-line arrow shows the direction of the pulsar motion; the cross marks the position of the pulsar at the epoch of the ESO/NTT observations. Middle and right: near-infrared images of the same field obtained with the HST/NICMOS in the ${\it F110W}$ and ${\it F160W}$ bands, respectively (Harlow et al. 1998). Boxes mark regions with Geminga, they are magnified in Fig. 4.
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In the text

$\begin{figure} \par\setlength{\unitlength}{1mm} \begin{picture} (90,45)(0,0) \p... ...width=4.3cm, bb=35 124 576 670,clip]{4178fig4b.ps} } \end{picture} \end{figure}$ Figure 4: $4'' \times 4''$ images of Geminga in the ${\it F110W}$ ( left) and ${\it F160W}$ ( right) bands. The circle annulus in the left panel mark the expected Geminga positions at the epochs of I-band observations with the NTT (1) and Subaru (2), respectively, while the long arrow shows the pulsar path calculated based on the proper motion measurements of Caraveo et al. (1996). Contours of the Subaru image in I band are overlaid in the right panel where the arrow shows the shift of Geminga due to its proper motion over 3.2 yr between the HST and Subaru observations; "+'' and 1 $\sigma$ -ellipse mark the expected positions of the pulsar at the epochs of the HST and Subaru observations, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm, bb=40 130 570 660, clip]{4178fig5.ps} \end{figure}$ Figure 5: A magnified fragment of the Subaru I band image of Geminga demonstrating an arc-like structure resembling a head of a bow-shock due to the pulsar supersonic motion in the interstellar matter (cf. contours in Fig.4). The motion direction is shown by arrow, the pulsar position is marked by a cross.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,bb=40 130 570 660,clip]{4178fig6.ps} \end{figure}$ Figure 6: Magnified fragment of the Subaru I band image of PSR B0656+14 demonstrating possible existence of a PWN or a bow-shock structure around the pulsar (extended object in the center of the image). Contours are overlaid to underline the shape of the structure; the arrow shows the direction of the pulsar proper motion, the pulsar position is marked by a cross
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In the text

$\begin{figure*} \par\setlength{\unitlength}{1mm} \hspace*{3mm}\resizebox{12cm}{... ...{\includegraphics[width=80mm, clip]{4178fig7b.eps}} \end{picture}} \end{figure*}$ Figure 7: Dereddened NIR-UV broadband spectra of PSR B0656+14 ( left) and Geminga ( right) summarizing the best up to date quality observations obtained with different telescopes, instruments and filters, as indicated in the plots and listed in Tables 5 and 6. Note a nonmonotonic structure and remarkable similarity of the broadband spectra for both pulsars. Thin solid curves show the spectroscopic data obtained for PSR B0656+14 in the NUV (Shibanov et al. 2005) and for Geminga in the FUV (Kargaltsev et al. 2005). Dashed lines are the low energy extensions of the unabsorbed soft blackbody (BB) and power law (PL) spectral components derived from the combined BB+BB+PL spectral fits in X-rays. Parameters of the fits are taken from Koptsevich et al. (2001) for PSR B0656+14 and from Kargaltsev et al. (2005) for Geminga. The second, hard BB components are negligible for both pulsars in the NIR-UV range and not shown in the plots. Dotted and dot-dashed lines in the right panel show the PL fit of the Geminga optical data in the range from ${\it F160W}$ through ${\it F430W}$ bands and its sum with the BB, respectively (see Sect. 4.1.3 for details).
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In the text

$\begin{figure} \includegraphics[width=11cm, bb=132 145 510 716]{4178fig8.ps} \end{figure}$ Figure 8: Unabsorbed multiwavelength spectra of the two pulsars using available data from radio through gamma-rays, as notified in the plot. X-ray spectral components are extended to the optical range, while the optical one - to X-rays.
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In the text

$\begin{figure} \par\setlength{\unitlength}{1mm} \begin{picture} (54,108)(0,0) \... ...idth=5.2cm,bb=130 205 485 570,clip]{4178fig2b.ps} } \end{picture}\end{figure}$	Figure 2: $20'' \times 20''$ fragments of the Subaru images of the Geminga field in the R ( top) and I ( bottom) bands. Axes orientation and label notations are the same as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=5.5cm, bb=40 130 570 660, clip]{4178fig5.ps} \end{figure}$	Figure 5: A magnified fragment of the Subaru I band image of Geminga demonstrating an arc-like structure resembling a head of a bow-shock due to the pulsar supersonic motion in the interstellar matter (cf. contours in Fig.4). The motion direction is shown by arrow, the pulsar position is marked by a cross.
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$\begin{figure} \par\includegraphics[width=5.5cm,bb=40 130 570 660,clip]{4178fig6.ps} \end{figure}$	Figure 6: Magnified fragment of the Subaru I band image of PSR B0656+14 demonstrating possible existence of a PWN or a bow-shock structure around the pulsar (extended object in the center of the image). Contours are overlaid to underline the shape of the structure; the arrow shows the direction of the pulsar proper motion, the pulsar position is marked by a cross
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$\begin{figure} \includegraphics[width=11cm, bb=132 145 510 716]{4178fig8.ps} \end{figure}$	Figure 8: Unabsorbed multiwavelength spectra of the two pulsars using available data from radio through gamma-rays, as notified in the plot. X-ray spectral components are extended to the optical range, while the optical one - to X-rays.
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