All Figures

$\begin{figure} \includegraphics[width=155mm,clip]{7728fig1.ps} \end{figure}$ Figure 1: PSR B1133+16 field as seen in the B band with the VLT/FORS1 using a standard resolution mode during the 2003-2004 period. The position of the pulsar is marked by +. The large box marks the FOV of high-resolution mode observations during the 2001 period. The $\times$ -shaped crosses and numbers mark the USNO-B1.0 reference stars from Table 4 and secondary photometric standard stars from Table 7, respectively. The region within a small box is enlarged in Figs. 2 and 4.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[width=86.5mm,clip]{aa7728-07f2a.eps} \... ...udegraphics[width=83.5mm, bb=88 253 458 583, clip]{7728fig2d.ps} }\end{figure}$ Figure 2: Fragments of the PSR B1133+16 field images obtained in the optical B and $R_{\rm c}$ bands with the VLT/FORS1 and in 0.2-10 keV X-ray range with the Chandra/ACIS-S at different epochs, as indicated in the plots. All images are smoothed with $\sim$ 1 $^{\prime \prime }$ Gaussian kernel, and the fragment sizes are $\sim$ 14 $^{\prime \prime }$ $\times~$ 14 $^{\prime \prime }$ . The + and $\times$ mark the expected radio positions of the pulsar at the observing epochs in the optical and X-ray images, respectively. The ellipses show $3\sigma$ position uncertainties, and the arrows show the direction of the pulsar proper motion and its path over about 20 yrs. The shift in the pulsar from 2001 to 2003 is indicated in the $R_{\rm c}$ image. The contour of object A seen in the 2001 B-band image is overlaid on the 2003 B-band image. The contours on the X-ray image are from the 2003 B-band image. Note that object B in the 2003 B-band image nicely fits the position of the candidate X-ray counterpart of the pulsar in the ACIS-S image.
Open with DEXTER

In the text

$\begin{figure} {\includegraphics[width=8.8cm, clip=]{7728fig3.eps} }\end{figure}$ Figure 3: The observed E-W spatial profiles of the regions containing objects A and Bextracted from the 2001 (top) and 2003 (bottom) B-band images of Fig. 2 along the slit with PA of 90 $^\circ$ and Dec = +15:51:11.49. The slit length is 4 $.\!\!^{\prime\prime}$ 6 and its width is 0 $.\!\!^{\prime\prime}$ 6. The coordinate origin of the horizontal axis corresponds to the eastern edge of the slit with RA = 11:36:03.317. The background was subtracted. Vertical dots mark the positions of A and B defined from the peaks of the profiles in the top and bottom panels, respectively. The short dashed line in the top panel shows a smoothed A profile that is used as a template to fit the A +B profile in the bottom panel as a sum of the two sources. The resulting fit is shown by the long dashed line, while short dashed lines show the contributions of A and B.
Open with DEXTER

In the text

$\begin{figure} \begin{tabular}{cc} \includegraphics[width=84.5mm, bb=144 296 400... ...s[width=84.5mm, bb=73 245 462 584, clip]{7728fig4c.ps}\end{tabular} \end{figure}$ Figure 4: The same as in Fig. 2 but for the H $_{\alpha }$ and (H $_\alpha -R$ ) images, with the contours from the X-ray image overlaid. The X-ray image with the (H $_\alpha -R$ ) image contours overlaid is also shown for comparison.
Open with DEXTER

In the text

$\begin{figure} {\includegraphics[width=70mm, clip]{7728fig5.eps} } \par \end{figure}$ Figure 5: The evolution of the pulsar radio, optical and X-ray luminosities, and respective efficiencies with the characteristic age $\tau$ . The top panel shows corresponding spin-down luminosities.
Open with DEXTER

In the text

$\begin{figure} {\includegraphics[width=8.8cm, clip]{7728fig6.eps} } \par \end{figure}$ Figure 6: Relations between the optical $\eta _{\rm Opt}$ and X-ray $\eta _{\rm X}$ efficiencies in the B-band and 2-10 keV ranges. Solid line shows the best linear regression fit for a sample of pulsars from Zharikov et al. (2006). The dot-dashed line is the similar fit only for the set of the pulsars that includes PSR B1133+16 counterpart candidate and excludes the youngest Crab and PSR J0540-69. Numbers are the line slopes with their errors in brackets.
Open with DEXTER

In the text

$\begin{figure} \begin{tabular}{cc} \includegraphics[width=84.5mm, bb=144 296 400... ...s[width=84.5mm, bb=73 245 462 584, clip]{7728fig4c.ps}\end{tabular} \end{figure}$	Figure 4: The same as in Fig. 2 but for the H $_{\alpha }$ and (H $_\alpha -R$ ) images, with the contours from the X-ray image overlaid. The X-ray image with the (H $_\alpha -R$ ) image contours overlaid is also shown for comparison.
Open with DEXTER

$\begin{figure} {\includegraphics[width=70mm, clip]{7728fig5.eps} } \par \end{figure}$	Figure 5: The evolution of the pulsar radio, optical and X-ray luminosities, and respective efficiencies with the characteristic age $\tau$ . The top panel shows corresponding spin-down luminosities.
Open with DEXTER