All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{9156fig1.eps} \end{figure}$ Figure 1: The G 15.1-1.6 in the H $\alpha$ + [N II] filter. Shadings run linearly from 0 to $220\times 10^{-17}$ erg s^-1 cm^-2 arcsec^-2. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction. The bright region in the northwest edge of the image is a known H II region (Lockman 1989).
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{9156fig2.eps} \end{figure}$ Figure 2: The G 15.1-1.6 in the [O III] filter. Shadings run linearly from 0 to $45\times 10^{-17}$ erg s^-1 cm^-2 arcsec^-2. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{9156fig3.eps} \end{figure}$ Figure 3: The continuum-subtracted mosaic of G 15.1-1.6 taken with the 1.3-m telescope in the light of H $\alpha$ + [N II]. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{9156fig4.eps} \end{figure}$ Figure 4: The continuum-subtracted mosaic of G 15.1-1.6 taken with the 1.3-m telescope in the light of [O III]. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction.
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In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{9156fig5.eps} \end{figure}$ Figure 5: Typical long-slit spectra.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{9156fig6.eps} \end{figure}$ Figure 6: The correlation between the H $\alpha$ + [N II] emission, and the radio emission at 4850 MHz (solid red line), the infrared emission at IRAS 60 $\mu$ m (solid green line). The 4850 MHz radio contours scale linearly from $3.54\times 10^{-2}$ Jy/beam, to 0.3 Jy/beam while the 60 $\mu$ m contours are at the level of 170, 200, 230, and 260 MJy/sr. The ellipse (dash blue line) defines the SNR's boundary approximately.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{9156fig1.eps} \end{figure}$	Figure 1: The G 15.1-1.6 in the H $\alpha$ + [N II] filter. Shadings run linearly from 0 to $220\times 10^{-17}$ erg s^-1 cm^-2 arcsec^-2. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction. The bright region in the northwest edge of the image is a known H II region (Lockman 1989).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{9156fig2.eps} \end{figure}$	Figure 2: The G 15.1-1.6 in the [O III] filter. Shadings run linearly from 0 to $45\times 10^{-17}$ erg s^-1 cm^-2 arcsec^-2. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{9156fig3.eps} \end{figure}$	Figure 3: The continuum-subtracted mosaic of G 15.1-1.6 taken with the 1.3-m telescope in the light of H $\alpha$ + [N II]. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{9156fig4.eps} \end{figure}$	Figure 4: The continuum-subtracted mosaic of G 15.1-1.6 taken with the 1.3-m telescope in the light of [O III]. The image has been smoothed to suppress the residuals from the imperfect continuum subtraction.
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$\begin{figure} \par\includegraphics[width=11.5cm,clip]{9156fig5.eps} \end{figure}$	Figure 5: Typical long-slit spectra.
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