All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{9987-f1.epsi} \end{figure}$ Figure 1: The SNR G0.9+0.1 at 330 MHz as taken from Nord et al. (2004).
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In the text

$\begin{figure} \hbox{ \psfig{figure=9987-f2.ps,width= 10 cm} } \end{figure}$ Figure 2: The SNR G0.9+0.1 at $\lambda$ 20 cm. The angular resolution is 13 $.\!\!^{\prime\prime}$ 1 $\times$ 8 $.\!\!^{\prime\prime}$ 6 and the rms noise of 0.25 mJy beam^-1.
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In the text

$\begin{figure} \par\psfig{figure=9987-f3.ps,width=15cm,clip} \end{figure}$ Figure 3: Color image of the central PWN in the SNR G0.9+0.1 at $\lambda$ 6 cm. The angular resolution is 2 $.\!\!^{\prime\prime}$ 9 $\times$ 1 $.\!\!^{\prime\prime}$ 6 and the rms noise 0.07 mJy/b.
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In the text

$\begin{figure} \par\psfig{figure=9987-f4.ps,width=16cm,clip} \end{figure}$ Figure 4: Grey-scale images of the central PWN in the SNR G0.9+0.1 at 90, 20, 6 and 3.6 cm wavelengths. The black cross marks the position of the X-ray point source CXOU J174722.8-280915. The different features individualized in the panel corresponding to the 6 cm image are discussed in the text.
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In the text

$\begin{figure} \par\includegraphics[width=8 cm,clip]{9987-f5.ps} \end{figure}$ Figure 5: Radio spectrum of the PWN in G0.9+0.1. The data from this work are shown by filled circles; data at 1400 and 4850 MHz from Helfand & Becker (1987) and data at 330 MHz from La Rosa et al. (2000) are displayed as open squares. The best linear fit based on the new data plus the 330 MHz (solid line) produces $\alpha =-0.22$ . A linear fit to the new data alone (dashed line) produces $\alpha =-0.14$ . Data from Helfand & Becker (1987) were not used in the fitting. An average $\alpha =-0.18\pm 0.04$ is adopted.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{9987-f6.ps} \end{figure}$ Figure 6: Reprocessed XMM-Newton and Chandra X-ray images displayed together with the 6 cm radio image. Both X-ray images have X-ray contours (white) and a radio contour (black) overlapped to facilitate the identification of features and the multispectral comparison. The location of the pulsar candidate CXOU J174722.8-280915 is marked by a white plus sign.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{9987-f7.ps} \end{figure}$ Figure 7: Spectrum of the PWN in G0.9+0.1 over the range 10⁸to 10¹⁹ Hz, with a spectral index $\alpha _{\rm R}=-0.18$ in the radio regime and $\alpha _{\rm X}=-1.1$ as derived from X-ray data. The extrapolation of the X-ray spectrum intersects that of the radio spectrum at the turnover frequency $\nu _{\rm b}=2.4\times 10^{12}$ Hz.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9987-f8.ps} \end{figure}$ Figure 8: Spectral energy distribution of the PWN in G0.9+0.1 from radio to VHE gamma-ray, joining the new estimates in the radio and X-ray bands with HESS measurements.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9987-f1.epsi} \end{figure}$	Figure 1: The SNR G0.9+0.1 at 330 MHz as taken from Nord et al. (2004).
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$\begin{figure} \hbox{ \psfig{figure=9987-f2.ps,width= 10 cm} } \end{figure}$	Figure 2: The SNR G0.9+0.1 at $\lambda$ 20 cm. The angular resolution is 13 $.\!\!^{\prime\prime}$ 1 $\times$ 8 $.\!\!^{\prime\prime}$ 6 and the rms noise of 0.25 mJy beam^-1.
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$\begin{figure} \par\psfig{figure=9987-f3.ps,width=15cm,clip} \end{figure}$	Figure 3: Color image of the central PWN in the SNR G0.9+0.1 at $\lambda$ 6 cm. The angular resolution is 2 $.\!\!^{\prime\prime}$ 9 $\times$ 1 $.\!\!^{\prime\prime}$ 6 and the rms noise 0.07 mJy/b.
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$\begin{figure} \par\psfig{figure=9987-f4.ps,width=16cm,clip} \end{figure}$	Figure 4: Grey-scale images of the central PWN in the SNR G0.9+0.1 at 90, 20, 6 and 3.6 cm wavelengths. The black cross marks the position of the X-ray point source CXOU J174722.8-280915. The different features individualized in the panel corresponding to the 6 cm image are discussed in the text.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{9987-f6.ps} \end{figure}$	Figure 6: Reprocessed XMM-Newton and Chandra X-ray images displayed together with the 6 cm radio image. Both X-ray images have X-ray contours (white) and a radio contour (black) overlapped to facilitate the identification of features and the multispectral comparison. The location of the pulsar candidate CXOU J174722.8-280915 is marked by a white plus sign.
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$\begin{figure} \par\includegraphics[width=6.3cm,clip]{9987-f7.ps} \end{figure}$	Figure 7: Spectrum of the PWN in G0.9+0.1 over the range 10⁸to 10¹⁹ Hz, with a spectral index $\alpha _{\rm R}=-0.18$ in the radio regime and $\alpha _{\rm X}=-1.1$ as derived from X-ray data. The extrapolation of the X-ray spectrum intersects that of the radio spectrum at the turnover frequency $\nu _{\rm b}=2.4\times 10^{12}$ Hz.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9987-f8.ps} \end{figure}$	Figure 8: Spectral energy distribution of the PWN in G0.9+0.1 from radio to VHE gamma-ray, joining the new estimates in the radio and X-ray bands with HESS measurements.
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