All Figures

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{8227f1.eps}\end{figure}$ Figure 1: a) 4 $\times$ 4 arcmin image centered on PSR B1929+10 in the energy band of 0.5-8 keV. Top is north and left is east. The image is created by merging both Chandra observations. It is binned with a factor of 0.5 arcsec and adaptively smoothed with a kernel of $\sigma < 2$ arcsec. b) The close-up view of the central 1 $\times$ 1 arcmin region as illustrated in a). The proper motion corrected pulsar position is indicated by the white cross. An arc-like feature associated with the pulsar is observed. The proper motion direction of the pulsar (Chatterjee et al. 2004) is illustrated by the arrow. Contour lines at the levels of (6.1-26) $\times$ 10^-6 counts arcsec^-2 s^-1 are overlaid.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8227f2.eps}\end{figure}$ Figure 2: Vignetting corrected brightness profile of the field around PSR B1929+10. The energy range is 0.5-8 keV. The profile expected for a point source is indicated by a dotted line. The average background level and its $1\sigma$ deviation are indicated by horizontal lines, which were calculated by sampling the source-free regions around the pulsar within a 1 $\times$ 1 arcmin field-of-view. The inset shows the sixteen bins used in computing the profile. Each bin is 1'' $\times$ 15''.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{8227f3.eps}\end{figure}$ Figure 3: The 5 $\times$ 5 arcmin region around PSR B1929+10 in the energy band of 0.5-8 keV. The image is created by merging both Chandra observations. It has a binning factor of 2 arcsec and is adaptively smoothed with a kernel of $\sigma < 6$ arcsec. Top is north and left is east. The contours from the XMM-Newton's MOS1/2 0.2-10 keV band image at the levels of 0.09 and 0.44 counts arcsec^-2 are overlaid. The proper motion corrected pulsar position is indicated by the white cross. The proper motion direction of the pulsar is indicated by the arrow in the image.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{8227f4.eps} \end{figure}$ Figure 4: Energy spectra of PSR B1929+10 as observed with the Chandra ACIS-S3 detector on 04 Dec. 2005 and 28 May 2006 and simultaneously fitted to an absorbed power-law model ( upper panel) and contribution to the $\chi ^{2}$ fit statistic ( lower panel).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8227f5.eps} \end{figure}$ Figure 5: $1\sigma$ , $2\sigma$ and $3\sigma$ confidence contours calculated for 1 parameter of interest for the power-law model fitted to the spectrum of PSR B1929+10.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{8227f6.eps} \end{figure}$ Figure 6: 1 $\times$ 1 arcmin raw image (0.5-8 keV) centered on PSR B1929+10. Data from both Chandra observations were used. The extraction regions used for the spectral analysis of the arc-like feature are illustrated.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8227f7.eps}\end{figure}$ Figure 7: Energy spectra of the arc-like structure associated with PSR B1929+10 as observed by the Chandra ACIS-S3 detector on 04 Dec. 2005 and 28 May 2006, and simultaneously fitted to an absorbed power-law model ( upper panel) and contribution to the $\chi ^{2}$ fit statistic ( lower panel).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{8227f4.eps} \end{figure}$	Figure 4: Energy spectra of PSR B1929+10 as observed with the Chandra ACIS-S3 detector on 04 Dec. 2005 and 28 May 2006 and simultaneously fitted to an absorbed power-law model ( upper panel) and contribution to the $\chi ^{2}$ fit statistic ( lower panel).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8227f5.eps} \end{figure}$	Figure 5: $1\sigma$ , $2\sigma$ and $3\sigma$ confidence contours calculated for 1 parameter of interest for the power-law model fitted to the spectrum of PSR B1929+10.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{8227f6.eps} \end{figure}$	Figure 6: 1 $\times$ 1 arcmin raw image (0.5-8 keV) centered on PSR B1929+10. Data from both Chandra observations were used. The extraction regions used for the spectral analysis of the arc-like feature are illustrated.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8227f7.eps}\end{figure}$	Figure 7: Energy spectra of the arc-like structure associated with PSR B1929+10 as observed by the Chandra ACIS-S3 detector on 04 Dec. 2005 and 28 May 2006, and simultaneously fitted to an absorbed power-law model ( upper panel) and contribution to the $\chi ^{2}$ fit statistic ( lower panel).
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