All Figures

$\begin{figure} \par\resizebox{17.7cm}{!}{\includegraphics{2996.f1}} \end{figure}$ Figure 1: The field of G 82.2+5.3 in the H $\alpha +[$ N II] filter. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction. The open and the filled circles designate the positions of bright and dark nebulae, respectively, while the numbers in parentheses represent the surface of each nebula in square degrees as given by Lynds (1962, 1965). The open polygons show the positions where emission line ratios are measured (see also Sect. 3.3). The shadings run linearly from 0 to 400 $\times$ 10^-17 erg s^-1 cm^-2 arcsec^-2. The line segments seen near over-exposed stars in this figure and the next figures are due to the blooming effect.
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In the text

$\begin{figure} \par\resizebox{17.7cm}{!}{\includegraphics{2996.f2}} \end{figure}$ Figure 2: The [S II] image of the area around G 82.2+5.3. The morphology in these emission lines is similar to that of the H $\alpha +[$ N II] lines. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction, while the shadings run linearly from 0 to 60 $\times$ 10^-17 erg s^-1 cm^-2 arcsec^-2.
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In the text

$\begin{figure} \par\resizebox{17.25cm}{!}{\includegraphics{2996.f3}} \end{figure}$ Figure 3: The medium ionization line of [O III]5007 Å provides the sharpest view of G 82.2+5.3 ( left). The image has been smoothed to suppress the residuals from the imperfect continuum subtraction and the shadings run linearly from 0 to 30 $\times$ 10^-17 erg s^-1 cm^-2 arcsec^-2. The long rectangles indicate the projected positions of the slits on the sky and the numbers designate the areas discussed in the text. The right figure shows single long-slit spectra from areas II and III.
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In the text

$\begin{figure} \par\resizebox{17.25cm}{!}{\includegraphics{2996.f4}} \end{figure}$ Figure 4: The correlation between the [O III] emission and the radio emission at 326 MHz ( left) and 4850 MHz ( right) is shown in this figure. The 326 MHz radio contours (Rengelink et al. 1997) scale linearly from 0.01 Jy/beam to 0.09 Jy/beam, while the 4850 MHz contours scale from 5 $\times$ 10^-4 Jy/beam to 0.2 Jy/beam (Condon et al. 1994). The optical and radio data are rather well correlated in the east areas of the remnant. The radio emission in the west seems to be weeker and mainly related to the H II region.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{2996.f5}} \end{figure}$ Figure 5: The raw soft X-ray emission detected in the 8 ks ROSAT pointed observation is shown in this figure. The brightness scales linearly from 2 to 24 counts/pixel and the image has been smoothed with a Gaussian filter with $\sigma$ = 8 $^\prime$ . The radio contours at 326 MHz scale also also linearly from 0.015 to 0.09 Jy/beam (Rengelink et al. 1997).
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In the text

$\begin{figure} \par\resizebox{11.5cm}{!}{\includegraphics{2996.f6}} \end{figure}$ Figure 6: The brightness profile (crosses) of G 82.2+5.3 derived from the ROSAT data is shown in this figure. The open squares mark the exponential best fit with some limb brightening, while the open triangles mark the power-law best fit. The reader is referred to Sect. 4.1 for more details.
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In the text

$\begin{figure} \par\resizebox{16.8cm}{!}{\includegraphics{2996.f7}} \end{figure}$ Figure 7: The ASCA GIS2/3 data are shown in the left figure together with the best fit vmekal model, while the spectra from the SIS detectors are shown in the right figure with the same model (see Sect. 4.2).
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In the text

$\begin{figure} \par\resizebox{12cm}{!}{\includegraphics{2996.f8.eps}} \end{figure}$ Figure 8: Best fit and error contours (1 $\sigma$ to 4 $\sigma$ in steps of 1 $\sigma$ ) for the temperature ( kT) and the interstellar absorption column density $N\sb {\rm H}$ for one-temperature vmekal models to the ROSAT PSPC spectrum (lower left) and the ASCA GIS/SIS spectra (upper right). Note that there is essentially no overlap, indicating the need for more advanced models.
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In the text

$\begin{figure} \par\resizebox{17.7cm}{!}{\includegraphics{2996.f2}} \end{figure}$	Figure 2: The [S II] image of the area around G 82.2+5.3. The morphology in these emission lines is similar to that of the H $\alpha +[$ N II] lines. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction, while the shadings run linearly from 0 to 60 $\times$ 10^-17 erg s^-1 cm^-2 arcsec^-2.
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$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{2996.f5}} \end{figure}$	Figure 5: The raw soft X-ray emission detected in the 8 ks ROSAT pointed observation is shown in this figure. The brightness scales linearly from 2 to 24 counts/pixel and the image has been smoothed with a Gaussian filter with $\sigma$ = 8 $^\prime$ . The radio contours at 326 MHz scale also also linearly from 0.015 to 0.09 Jy/beam (Rengelink et al. 1997).
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$\begin{figure} \par\resizebox{11.5cm}{!}{\includegraphics{2996.f6}} \end{figure}$	Figure 6: The brightness profile (crosses) of G 82.2+5.3 derived from the ROSAT data is shown in this figure. The open squares mark the exponential best fit with some limb brightening, while the open triangles mark the power-law best fit. The reader is referred to Sect. 4.1 for more details.
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$\begin{figure} \par\resizebox{16.8cm}{!}{\includegraphics{2996.f7}} \end{figure}$	Figure 7: The ASCA GIS2/3 data are shown in the left figure together with the best fit vmekal model, while the spectra from the SIS detectors are shown in the right figure with the same model (see Sect. 4.2).
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$\begin{figure} \par\resizebox{12cm}{!}{\includegraphics{2996.f8.eps}} \end{figure}$	Figure 8: Best fit and error contours (1 $\sigma$ to 4 $\sigma$ in steps of 1 $\sigma$ ) for the temperature ( kT) and the interstellar absorption column density $N\sb {\rm H}$ for one-temperature vmekal models to the ROSAT PSPC spectrum (lower left) and the ASCA GIS/SIS spectra (upper right). Note that there is essentially no overlap, indicating the need for more advanced models.
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